what is a gamma-ray burst?
DESCRIPTION
Short g -ray flashes E > 100 keV 0.01 < t 90 < 1000s Diverse lightcurves BATSE detected 1/day = 1000 /year/universe Energy ~ 10 52 f g -1 f W/0.1 erg. Near star forming regions 2 SN Ibc associations Supernova component in lightcurves. What is a Gamma-Ray Burst?. - PowerPoint PPT PresentationTRANSCRIPT
What is a Gamma-Ray Burst
bull Short -ray flashes E gt 100 keV
bull 001 lt t90 lt 1000s
bull Diverse lightcurvesbull BATSE detected
1day = 1000 yearuniverse
bull Energy ~ 1052 f
-1 ferg
bull Near star forming regions
bull 2 SN Ibc associations
bull Supernova component in lightcurves
Superbowl Burst
ms variability + non-thermal spectrum Compactness
GRB Light Curve
M = E c2 ~ 10-6
Msun
GRB 990123
1 CGRO ~1o
2 BeppoSAX (X-ray)
6-33 hrs
34-54 hrs
~ 1rsquo
4 HST 17 days
3 Palomar lt 1 dayKeck
spectrum
z=160
Eiso =
3x1054 erg
~ Msunc2
9th mag flash
135 models (1993)
Note most are Galactic and are ruled out for long bursts
GRB photons are made far away from engine
Canrsquot observe engine directly in light (neutrinos gravitational waves)
Electromagnetic process or neutrino annihilation to tap power of central compact object
Hyper-accreting black hole or high field neutron star (rotating)
Well-localized bursts are all ldquolong-softrdquo
ldquoshort-hardrdquo bursts
Duration (s)
hardness
Kulkarni et al
NTT image (May 1 1998) of SN 1998bw in the barred spiral galaxy ESO 184-G82 [Galama et al AampAS 138 465 (1999)]
WFC error box (8) for GRB 980425 and two NFI x-ray sources The IPN error arc is also shown
1) Were the two events the same thing
2) Was GRB 980425 an ordinary GRB seen off-axis
SN 1998bwGRB 980425
Bloom et al (ApJL2002)
GRB991121
see also Hjorth et al Fox et al Nature (2003)
extremely close = 800 Mpc
GRB030329SN2003DH
SN 1998bwGRB 980425
The supernova - a Type Ic - was very unusual
Large mass of 56Ni 03 - 09 solar masses (note jets acting alone do not make 56Ni) Sollerman et al ApJL 537 127 (2000) McKinzie amp Schaefer PASP 111 964 (1999)
Extreme energy and mass gt 1052 erg gt 10 Msun Iwamoto et al Nature 395 672 (1998) Woosley Eastman amp Schmidt ApJ 516 788 (1999) Mazzali et al ApJ 559 1047 (2001)
Exceptionally strong radio source Li amp Chevalier ApJ 526 716 (1999) Relativistic matter was ejected 1050 - 1051 erg Wieringa Kulkarni amp Frail AampAS 138 467 (1999) Frail et al ApJL (2001) astroph-0102282
Probability favors the GRB-SN association Pian et al ApJ 536 778 (2000)
Merging neutron star - black hole pairs
Strengths
a) Known event b) Plenty of angular momentum c) Rapid time scale d) High energy e) Well developed numerical models
Weaknesses a) Outside star forming regions
b) Beaming and energy may be inadequate for long bursts
But this model may still be good for a class of bursts calledthe ldquoshort hardrdquo bursts for which we have no counterpart informationyet (SWIFT)
Ruffert amp Janka Rosswog et al Lee et al Aloy et al
Requirements on the Central Engineand its Immediate Surroundings
(long-soft bursts)bull Provide adequate energy at high Lorentz factor
bull Collimate the emergent beam to approximately 01 radians
bull In the internal shock model provide a beam with rapidly variable Lorentz factor
bull Allow for the observed diverse GRB light curves
bull Last approximately 10 s but much longer in some cases
bull Explain diverse events like GRB 980425
bull Produce a (Type Ibc) supernova in some cases
bull Make bursts in star forming regions
GRB central engine
bull Relativity (SR amp GR)bull Magnetic Fieldsbull Rotation (progenitors)bull Nuclear Physicsbull Neutrinosbull EOSbull Turbulencebull 3Dbull Range of Lengthscales
Muller (1999)
ldquoDelayedrdquo SN Explosion
ac
Accretion vs Neutrino heating
Burrows (2001)
Pre-Supernova Density Structure
Woosley amp Weaver (1995)
Bigger stars
Higher entropy
Shallower density gradients
Fryer ApJ 522 413 (1999) Burrows (1999)
Bigger stars
1 Accrete faster amp longer
2 Larger binding energy amp smaller explosion energy
explosion
binding
Failure of delayed mechanism
Fukuda (1982)
Heger (2000)
Stellar Rotation
no mass lossMass loss
No B fields
Collapsars
Type Masssun BH Time Scale Distance Comment
I 15-40 He prompt 20 s all z neutrino-dominated disk
II 10-40 He delayed 20 s ndash 1 hr all z black hole by fall back
III gt130 He prompt ~20 s zgt10 time dilated redshifted (1+z) very energetic pair instability low Z
A rotating massive star whose core collapses to a black hole and produces an accretion disk
Type I is what we are usually talking aboutThe 40 solar mass limit comes from assuming that all stars above 100 solar masses on the main sequence are unstable (except Pop III)
IFTwo plausible conditions occur
1 Failure of neutrino powered SN explosion
a completeb partial (fallback)
2 Rotating stellar coresj gt 3 x 1016 cm2s
THEN
Rapidly accreting black hole (M~01 Ms)fed by collapsing star (tdyn ~ 446 s frac12 ~ 10 s)Disk formation
COLLAPSAR
Collapsar Simulations
bull pre-SN 15 Msun Helium starbull Newtonian Hydrodynamics (PPM)bull alpha viscositybull rotationbull photodisintegration (NSE alpha n p)bull neutrino cooling thermal + URCA optically thinbull Ideal nucleons radiation relativistic degenerate
electrons positionsbull 2D axisymmetric spherical gridbull self gravity pseudo-Newtonian (PW)bull Rin = 9 Rs Rout = 9000 Rs
MacFadyen amp Woosley (1999)
Collapsar Disk AnimationPPM hydrodynamics Paczynski-Witta potential EOS neutrino cooling nuclear reactions viscosity
Stellar collapse w rotation
Density structure No disk no wind
Note Accretion shock funnel clearing pole to equator density contrast fluctuating polar density
Initial model 15 Msun Helium (Wolf-Rayet) star evolved with mass loss
R= 8 x 108 cm
Show inner 1 in radius disk mass = 001 M_sun
Low viscosity =001
Disk Formation Movie
Accretion Shock
Disk formation
t = 75 s
PhotodisintegrationSiOC -gt free neutronsAnd protons Enhanced neutrino cooling
neutrino coolong allows
accretion
no cooling=gt
dynamically unstable
CDAF
Could emit GWs but
maybe no GRB
= 01 ltMgt = 007 Msun s = 13 x 1053 ergs
spin
mass
Use 1D neutrino cooled
ldquoslimrdquo disk models
from Popham et al (1999)
Collapsar results
bull Sustained accretion gt10sbull Sufficient energy bull Time scale set by He core collapsebull Disk-feeding time scale not disk-drainingbull Neutrino cooling allows accretionbull Neutrino annihilation energetically
possiblendash calculable in any case
Funnel geometry
channels any fireball
Density contrasts can
be huge
Ejet = f Maccc2
MHD
T = 57 ms
E = 5 x 1050 ergs
Edep = 28 x 1048 erg
Jet BirthThermal energy deposition focused by toroidal funnel structure
fmax ~ 06 - 4
Relativistic Jet Movie
Collapsar stages1 Iron core collapse disk formation
T~1010K ~108gcm-3 photodisintegration cooling pair capture disk is free nucleons (2 s)
2 Polar density declines to allow jet birthfrac12v3 Edep (2-5 s)
3 Jet tunnels out of star (5 s) Wolf-Rayet4 Jet powered for ~10 more seconds
Evacuates polar channel and reaches asymptotic speed (10 s)
T_GRB T_collapse
Jupiter
Red Supergiant
R~1013 cm
Blue Supergiant
R~1012 cm
Wolf-Rayet Star
R~1011 cm
Type Ib or Ic
Supernova
Supernovae
Ia
WD cosmology
Type II
Hydrogen
Type I
No Hydrogen
Ib Ic
exploding WR
thermonuclear old pop E galaxies
core collapse massive stars
Nickel Wind Movie
ldquoNickel Windrdquo
T gt 5 x 109 K
Fallback in weak SN explosions
Shock reaches
surface of star but parts of star are
not ejected to infinity
Fallback accretion Mms ~ 25 Msun Same star
exploded with a range of explosion energies
Significant accretion for thousands of
seconds ndash days
If fallback fuels a jet with power
fmc2
May power ldquohypernovardquo or long duration
GRBWeak
supernova shock
Shock breakout X-Ray transient
2 ldquoBriefrdquo jet tengine tjet
Engine dies before jet breakout
Mildly relativistic shock breakout
MacFadyen (1999)
What made SN1998bw+GRB980425
1 Accretion powered hypernova w Nickel wind
MacFadyen (2002)
E~ 1052 erg M(Ni)~05 M
GRB from ~3 shock breakout (Tan et al 2001 Perna amp Vietri 2002)
Collapsars
bull Can make ldquolongrdquo GRBs in H stripped (WR) stars tengine gt tescape
bull Short bursts may be compact binary mergersbull Need SN failure amp angular momentum
ndash Low metallicity binary can help
bull Star can explode -gt SN if nickel is made Predicts GRBSN association Type Ibc
bull SNGRB ratio may depend on angular momentumbull ldquoNickel windrdquo can explode star -gt hypernova
ndash H env Type II (no GRB) no H Type I + GRB
GRBGW bull Long GRBs
ndash not brighter than SN in GW
ndash very far Gpc
ndash very rare lt 1 SN
bull Short GBsndash merging ns-bh binaries
ndash maybe closer than long bursts
ndash short delay between event and GRB
ndash good for SWIFTLIGO
Rates
bull SN 1s = 100000 day
bull GRB 1day (BATSE) = 1000day
bull GRB rate = 1 of SN rate
bull maybe more collapsars than GRBs
bull =gt more rapidly rotating SN
bull SN with collapsar engine
bull look for bright Type Ic (w broad lines)
SN GW
bull SN1998bwGRB980425
bull 40 Mpc
bull maybe dominant GRB
bull rapid rotaters
bull SNAPROTSE look for 1998bw 2003dh like SN
bull many light curves -gt better t_explode
Implications
bull Probe engine directly
bull collapse duration vs GRB duration
bull collapseGRB delay (internal vs external)
bull disk properties ndash low viscosity big disks
Issues
bull too much j =gt no GRB but bright GW
bull may need low metallicity for GRB
bull prefer high redshift
bull donrsquot know nearby rate
bull but 980425 may imply rate is high
bull look for weak GRBs like 980425
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
With decreasing metallicity the bindingenergy of the core and the size of the silicon core both increase making black hole formation more likely atlow metallicity Woosley Heger amp Weaver RMP (2002)
Black hole formation may be unavoidable for low metallicity
Solar metallicity
Low metallicity
In the absence of mass lossand magnetic fields there wouldbe abundant progenitors
Unfortunately nature has both
15 solar mass helium core born rotating rigidly at f times break up
The more difficult problem is the angular momentum Thisis a problem shared by all current GRB models that invokemassive stars
- What is a Gamma-Ray Burst
- Superbowl Burst
- Slide 3
- 135 models (1993)
- Slide 5
- Slide 6
- Slide 7
- GRB991121
- GRB030329SN2003DH
- Slide 10
- Slide 11
- Slide 12
- GRB central engine
- ldquoDelayedrdquo SN Explosion
- Pre-Supernova Density Structure
- Failure of delayed mechanism
- Stellar Rotation
- Slide 18
- Slide 19
- Collapsar Simulations
- Collapsar Disk Animation
- Disk Formation Movie
- Slide 23
- Slide 24
- Slide 25
- Collapsar results
- Slide 27
- Jet Birth
- Relativistic Jet Movie
- Collapsar stages
- Slide 31
- Slide 32
- Nickel Wind Movie
- Slide 34
- Slide 35
- Slide 36
- Slide 37
- Slide 38
- Collapsars
- GRBGW
- Rates
- SN GW
- Implications
- Issues
- Principle Results
- Slide 46
- Slide 47
-
Superbowl Burst
ms variability + non-thermal spectrum Compactness
GRB Light Curve
M = E c2 ~ 10-6
Msun
GRB 990123
1 CGRO ~1o
2 BeppoSAX (X-ray)
6-33 hrs
34-54 hrs
~ 1rsquo
4 HST 17 days
3 Palomar lt 1 dayKeck
spectrum
z=160
Eiso =
3x1054 erg
~ Msunc2
9th mag flash
135 models (1993)
Note most are Galactic and are ruled out for long bursts
GRB photons are made far away from engine
Canrsquot observe engine directly in light (neutrinos gravitational waves)
Electromagnetic process or neutrino annihilation to tap power of central compact object
Hyper-accreting black hole or high field neutron star (rotating)
Well-localized bursts are all ldquolong-softrdquo
ldquoshort-hardrdquo bursts
Duration (s)
hardness
Kulkarni et al
NTT image (May 1 1998) of SN 1998bw in the barred spiral galaxy ESO 184-G82 [Galama et al AampAS 138 465 (1999)]
WFC error box (8) for GRB 980425 and two NFI x-ray sources The IPN error arc is also shown
1) Were the two events the same thing
2) Was GRB 980425 an ordinary GRB seen off-axis
SN 1998bwGRB 980425
Bloom et al (ApJL2002)
GRB991121
see also Hjorth et al Fox et al Nature (2003)
extremely close = 800 Mpc
GRB030329SN2003DH
SN 1998bwGRB 980425
The supernova - a Type Ic - was very unusual
Large mass of 56Ni 03 - 09 solar masses (note jets acting alone do not make 56Ni) Sollerman et al ApJL 537 127 (2000) McKinzie amp Schaefer PASP 111 964 (1999)
Extreme energy and mass gt 1052 erg gt 10 Msun Iwamoto et al Nature 395 672 (1998) Woosley Eastman amp Schmidt ApJ 516 788 (1999) Mazzali et al ApJ 559 1047 (2001)
Exceptionally strong radio source Li amp Chevalier ApJ 526 716 (1999) Relativistic matter was ejected 1050 - 1051 erg Wieringa Kulkarni amp Frail AampAS 138 467 (1999) Frail et al ApJL (2001) astroph-0102282
Probability favors the GRB-SN association Pian et al ApJ 536 778 (2000)
Merging neutron star - black hole pairs
Strengths
a) Known event b) Plenty of angular momentum c) Rapid time scale d) High energy e) Well developed numerical models
Weaknesses a) Outside star forming regions
b) Beaming and energy may be inadequate for long bursts
But this model may still be good for a class of bursts calledthe ldquoshort hardrdquo bursts for which we have no counterpart informationyet (SWIFT)
Ruffert amp Janka Rosswog et al Lee et al Aloy et al
Requirements on the Central Engineand its Immediate Surroundings
(long-soft bursts)bull Provide adequate energy at high Lorentz factor
bull Collimate the emergent beam to approximately 01 radians
bull In the internal shock model provide a beam with rapidly variable Lorentz factor
bull Allow for the observed diverse GRB light curves
bull Last approximately 10 s but much longer in some cases
bull Explain diverse events like GRB 980425
bull Produce a (Type Ibc) supernova in some cases
bull Make bursts in star forming regions
GRB central engine
bull Relativity (SR amp GR)bull Magnetic Fieldsbull Rotation (progenitors)bull Nuclear Physicsbull Neutrinosbull EOSbull Turbulencebull 3Dbull Range of Lengthscales
Muller (1999)
ldquoDelayedrdquo SN Explosion
ac
Accretion vs Neutrino heating
Burrows (2001)
Pre-Supernova Density Structure
Woosley amp Weaver (1995)
Bigger stars
Higher entropy
Shallower density gradients
Fryer ApJ 522 413 (1999) Burrows (1999)
Bigger stars
1 Accrete faster amp longer
2 Larger binding energy amp smaller explosion energy
explosion
binding
Failure of delayed mechanism
Fukuda (1982)
Heger (2000)
Stellar Rotation
no mass lossMass loss
No B fields
Collapsars
Type Masssun BH Time Scale Distance Comment
I 15-40 He prompt 20 s all z neutrino-dominated disk
II 10-40 He delayed 20 s ndash 1 hr all z black hole by fall back
III gt130 He prompt ~20 s zgt10 time dilated redshifted (1+z) very energetic pair instability low Z
A rotating massive star whose core collapses to a black hole and produces an accretion disk
Type I is what we are usually talking aboutThe 40 solar mass limit comes from assuming that all stars above 100 solar masses on the main sequence are unstable (except Pop III)
IFTwo plausible conditions occur
1 Failure of neutrino powered SN explosion
a completeb partial (fallback)
2 Rotating stellar coresj gt 3 x 1016 cm2s
THEN
Rapidly accreting black hole (M~01 Ms)fed by collapsing star (tdyn ~ 446 s frac12 ~ 10 s)Disk formation
COLLAPSAR
Collapsar Simulations
bull pre-SN 15 Msun Helium starbull Newtonian Hydrodynamics (PPM)bull alpha viscositybull rotationbull photodisintegration (NSE alpha n p)bull neutrino cooling thermal + URCA optically thinbull Ideal nucleons radiation relativistic degenerate
electrons positionsbull 2D axisymmetric spherical gridbull self gravity pseudo-Newtonian (PW)bull Rin = 9 Rs Rout = 9000 Rs
MacFadyen amp Woosley (1999)
Collapsar Disk AnimationPPM hydrodynamics Paczynski-Witta potential EOS neutrino cooling nuclear reactions viscosity
Stellar collapse w rotation
Density structure No disk no wind
Note Accretion shock funnel clearing pole to equator density contrast fluctuating polar density
Initial model 15 Msun Helium (Wolf-Rayet) star evolved with mass loss
R= 8 x 108 cm
Show inner 1 in radius disk mass = 001 M_sun
Low viscosity =001
Disk Formation Movie
Accretion Shock
Disk formation
t = 75 s
PhotodisintegrationSiOC -gt free neutronsAnd protons Enhanced neutrino cooling
neutrino coolong allows
accretion
no cooling=gt
dynamically unstable
CDAF
Could emit GWs but
maybe no GRB
= 01 ltMgt = 007 Msun s = 13 x 1053 ergs
spin
mass
Use 1D neutrino cooled
ldquoslimrdquo disk models
from Popham et al (1999)
Collapsar results
bull Sustained accretion gt10sbull Sufficient energy bull Time scale set by He core collapsebull Disk-feeding time scale not disk-drainingbull Neutrino cooling allows accretionbull Neutrino annihilation energetically
possiblendash calculable in any case
Funnel geometry
channels any fireball
Density contrasts can
be huge
Ejet = f Maccc2
MHD
T = 57 ms
E = 5 x 1050 ergs
Edep = 28 x 1048 erg
Jet BirthThermal energy deposition focused by toroidal funnel structure
fmax ~ 06 - 4
Relativistic Jet Movie
Collapsar stages1 Iron core collapse disk formation
T~1010K ~108gcm-3 photodisintegration cooling pair capture disk is free nucleons (2 s)
2 Polar density declines to allow jet birthfrac12v3 Edep (2-5 s)
3 Jet tunnels out of star (5 s) Wolf-Rayet4 Jet powered for ~10 more seconds
Evacuates polar channel and reaches asymptotic speed (10 s)
T_GRB T_collapse
Jupiter
Red Supergiant
R~1013 cm
Blue Supergiant
R~1012 cm
Wolf-Rayet Star
R~1011 cm
Type Ib or Ic
Supernova
Supernovae
Ia
WD cosmology
Type II
Hydrogen
Type I
No Hydrogen
Ib Ic
exploding WR
thermonuclear old pop E galaxies
core collapse massive stars
Nickel Wind Movie
ldquoNickel Windrdquo
T gt 5 x 109 K
Fallback in weak SN explosions
Shock reaches
surface of star but parts of star are
not ejected to infinity
Fallback accretion Mms ~ 25 Msun Same star
exploded with a range of explosion energies
Significant accretion for thousands of
seconds ndash days
If fallback fuels a jet with power
fmc2
May power ldquohypernovardquo or long duration
GRBWeak
supernova shock
Shock breakout X-Ray transient
2 ldquoBriefrdquo jet tengine tjet
Engine dies before jet breakout
Mildly relativistic shock breakout
MacFadyen (1999)
What made SN1998bw+GRB980425
1 Accretion powered hypernova w Nickel wind
MacFadyen (2002)
E~ 1052 erg M(Ni)~05 M
GRB from ~3 shock breakout (Tan et al 2001 Perna amp Vietri 2002)
Collapsars
bull Can make ldquolongrdquo GRBs in H stripped (WR) stars tengine gt tescape
bull Short bursts may be compact binary mergersbull Need SN failure amp angular momentum
ndash Low metallicity binary can help
bull Star can explode -gt SN if nickel is made Predicts GRBSN association Type Ibc
bull SNGRB ratio may depend on angular momentumbull ldquoNickel windrdquo can explode star -gt hypernova
ndash H env Type II (no GRB) no H Type I + GRB
GRBGW bull Long GRBs
ndash not brighter than SN in GW
ndash very far Gpc
ndash very rare lt 1 SN
bull Short GBsndash merging ns-bh binaries
ndash maybe closer than long bursts
ndash short delay between event and GRB
ndash good for SWIFTLIGO
Rates
bull SN 1s = 100000 day
bull GRB 1day (BATSE) = 1000day
bull GRB rate = 1 of SN rate
bull maybe more collapsars than GRBs
bull =gt more rapidly rotating SN
bull SN with collapsar engine
bull look for bright Type Ic (w broad lines)
SN GW
bull SN1998bwGRB980425
bull 40 Mpc
bull maybe dominant GRB
bull rapid rotaters
bull SNAPROTSE look for 1998bw 2003dh like SN
bull many light curves -gt better t_explode
Implications
bull Probe engine directly
bull collapse duration vs GRB duration
bull collapseGRB delay (internal vs external)
bull disk properties ndash low viscosity big disks
Issues
bull too much j =gt no GRB but bright GW
bull may need low metallicity for GRB
bull prefer high redshift
bull donrsquot know nearby rate
bull but 980425 may imply rate is high
bull look for weak GRBs like 980425
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
With decreasing metallicity the bindingenergy of the core and the size of the silicon core both increase making black hole formation more likely atlow metallicity Woosley Heger amp Weaver RMP (2002)
Black hole formation may be unavoidable for low metallicity
Solar metallicity
Low metallicity
In the absence of mass lossand magnetic fields there wouldbe abundant progenitors
Unfortunately nature has both
15 solar mass helium core born rotating rigidly at f times break up
The more difficult problem is the angular momentum Thisis a problem shared by all current GRB models that invokemassive stars
- What is a Gamma-Ray Burst
- Superbowl Burst
- Slide 3
- 135 models (1993)
- Slide 5
- Slide 6
- Slide 7
- GRB991121
- GRB030329SN2003DH
- Slide 10
- Slide 11
- Slide 12
- GRB central engine
- ldquoDelayedrdquo SN Explosion
- Pre-Supernova Density Structure
- Failure of delayed mechanism
- Stellar Rotation
- Slide 18
- Slide 19
- Collapsar Simulations
- Collapsar Disk Animation
- Disk Formation Movie
- Slide 23
- Slide 24
- Slide 25
- Collapsar results
- Slide 27
- Jet Birth
- Relativistic Jet Movie
- Collapsar stages
- Slide 31
- Slide 32
- Nickel Wind Movie
- Slide 34
- Slide 35
- Slide 36
- Slide 37
- Slide 38
- Collapsars
- GRBGW
- Rates
- SN GW
- Implications
- Issues
- Principle Results
- Slide 46
- Slide 47
-
GRB 990123
1 CGRO ~1o
2 BeppoSAX (X-ray)
6-33 hrs
34-54 hrs
~ 1rsquo
4 HST 17 days
3 Palomar lt 1 dayKeck
spectrum
z=160
Eiso =
3x1054 erg
~ Msunc2
9th mag flash
135 models (1993)
Note most are Galactic and are ruled out for long bursts
GRB photons are made far away from engine
Canrsquot observe engine directly in light (neutrinos gravitational waves)
Electromagnetic process or neutrino annihilation to tap power of central compact object
Hyper-accreting black hole or high field neutron star (rotating)
Well-localized bursts are all ldquolong-softrdquo
ldquoshort-hardrdquo bursts
Duration (s)
hardness
Kulkarni et al
NTT image (May 1 1998) of SN 1998bw in the barred spiral galaxy ESO 184-G82 [Galama et al AampAS 138 465 (1999)]
WFC error box (8) for GRB 980425 and two NFI x-ray sources The IPN error arc is also shown
1) Were the two events the same thing
2) Was GRB 980425 an ordinary GRB seen off-axis
SN 1998bwGRB 980425
Bloom et al (ApJL2002)
GRB991121
see also Hjorth et al Fox et al Nature (2003)
extremely close = 800 Mpc
GRB030329SN2003DH
SN 1998bwGRB 980425
The supernova - a Type Ic - was very unusual
Large mass of 56Ni 03 - 09 solar masses (note jets acting alone do not make 56Ni) Sollerman et al ApJL 537 127 (2000) McKinzie amp Schaefer PASP 111 964 (1999)
Extreme energy and mass gt 1052 erg gt 10 Msun Iwamoto et al Nature 395 672 (1998) Woosley Eastman amp Schmidt ApJ 516 788 (1999) Mazzali et al ApJ 559 1047 (2001)
Exceptionally strong radio source Li amp Chevalier ApJ 526 716 (1999) Relativistic matter was ejected 1050 - 1051 erg Wieringa Kulkarni amp Frail AampAS 138 467 (1999) Frail et al ApJL (2001) astroph-0102282
Probability favors the GRB-SN association Pian et al ApJ 536 778 (2000)
Merging neutron star - black hole pairs
Strengths
a) Known event b) Plenty of angular momentum c) Rapid time scale d) High energy e) Well developed numerical models
Weaknesses a) Outside star forming regions
b) Beaming and energy may be inadequate for long bursts
But this model may still be good for a class of bursts calledthe ldquoshort hardrdquo bursts for which we have no counterpart informationyet (SWIFT)
Ruffert amp Janka Rosswog et al Lee et al Aloy et al
Requirements on the Central Engineand its Immediate Surroundings
(long-soft bursts)bull Provide adequate energy at high Lorentz factor
bull Collimate the emergent beam to approximately 01 radians
bull In the internal shock model provide a beam with rapidly variable Lorentz factor
bull Allow for the observed diverse GRB light curves
bull Last approximately 10 s but much longer in some cases
bull Explain diverse events like GRB 980425
bull Produce a (Type Ibc) supernova in some cases
bull Make bursts in star forming regions
GRB central engine
bull Relativity (SR amp GR)bull Magnetic Fieldsbull Rotation (progenitors)bull Nuclear Physicsbull Neutrinosbull EOSbull Turbulencebull 3Dbull Range of Lengthscales
Muller (1999)
ldquoDelayedrdquo SN Explosion
ac
Accretion vs Neutrino heating
Burrows (2001)
Pre-Supernova Density Structure
Woosley amp Weaver (1995)
Bigger stars
Higher entropy
Shallower density gradients
Fryer ApJ 522 413 (1999) Burrows (1999)
Bigger stars
1 Accrete faster amp longer
2 Larger binding energy amp smaller explosion energy
explosion
binding
Failure of delayed mechanism
Fukuda (1982)
Heger (2000)
Stellar Rotation
no mass lossMass loss
No B fields
Collapsars
Type Masssun BH Time Scale Distance Comment
I 15-40 He prompt 20 s all z neutrino-dominated disk
II 10-40 He delayed 20 s ndash 1 hr all z black hole by fall back
III gt130 He prompt ~20 s zgt10 time dilated redshifted (1+z) very energetic pair instability low Z
A rotating massive star whose core collapses to a black hole and produces an accretion disk
Type I is what we are usually talking aboutThe 40 solar mass limit comes from assuming that all stars above 100 solar masses on the main sequence are unstable (except Pop III)
IFTwo plausible conditions occur
1 Failure of neutrino powered SN explosion
a completeb partial (fallback)
2 Rotating stellar coresj gt 3 x 1016 cm2s
THEN
Rapidly accreting black hole (M~01 Ms)fed by collapsing star (tdyn ~ 446 s frac12 ~ 10 s)Disk formation
COLLAPSAR
Collapsar Simulations
bull pre-SN 15 Msun Helium starbull Newtonian Hydrodynamics (PPM)bull alpha viscositybull rotationbull photodisintegration (NSE alpha n p)bull neutrino cooling thermal + URCA optically thinbull Ideal nucleons radiation relativistic degenerate
electrons positionsbull 2D axisymmetric spherical gridbull self gravity pseudo-Newtonian (PW)bull Rin = 9 Rs Rout = 9000 Rs
MacFadyen amp Woosley (1999)
Collapsar Disk AnimationPPM hydrodynamics Paczynski-Witta potential EOS neutrino cooling nuclear reactions viscosity
Stellar collapse w rotation
Density structure No disk no wind
Note Accretion shock funnel clearing pole to equator density contrast fluctuating polar density
Initial model 15 Msun Helium (Wolf-Rayet) star evolved with mass loss
R= 8 x 108 cm
Show inner 1 in radius disk mass = 001 M_sun
Low viscosity =001
Disk Formation Movie
Accretion Shock
Disk formation
t = 75 s
PhotodisintegrationSiOC -gt free neutronsAnd protons Enhanced neutrino cooling
neutrino coolong allows
accretion
no cooling=gt
dynamically unstable
CDAF
Could emit GWs but
maybe no GRB
= 01 ltMgt = 007 Msun s = 13 x 1053 ergs
spin
mass
Use 1D neutrino cooled
ldquoslimrdquo disk models
from Popham et al (1999)
Collapsar results
bull Sustained accretion gt10sbull Sufficient energy bull Time scale set by He core collapsebull Disk-feeding time scale not disk-drainingbull Neutrino cooling allows accretionbull Neutrino annihilation energetically
possiblendash calculable in any case
Funnel geometry
channels any fireball
Density contrasts can
be huge
Ejet = f Maccc2
MHD
T = 57 ms
E = 5 x 1050 ergs
Edep = 28 x 1048 erg
Jet BirthThermal energy deposition focused by toroidal funnel structure
fmax ~ 06 - 4
Relativistic Jet Movie
Collapsar stages1 Iron core collapse disk formation
T~1010K ~108gcm-3 photodisintegration cooling pair capture disk is free nucleons (2 s)
2 Polar density declines to allow jet birthfrac12v3 Edep (2-5 s)
3 Jet tunnels out of star (5 s) Wolf-Rayet4 Jet powered for ~10 more seconds
Evacuates polar channel and reaches asymptotic speed (10 s)
T_GRB T_collapse
Jupiter
Red Supergiant
R~1013 cm
Blue Supergiant
R~1012 cm
Wolf-Rayet Star
R~1011 cm
Type Ib or Ic
Supernova
Supernovae
Ia
WD cosmology
Type II
Hydrogen
Type I
No Hydrogen
Ib Ic
exploding WR
thermonuclear old pop E galaxies
core collapse massive stars
Nickel Wind Movie
ldquoNickel Windrdquo
T gt 5 x 109 K
Fallback in weak SN explosions
Shock reaches
surface of star but parts of star are
not ejected to infinity
Fallback accretion Mms ~ 25 Msun Same star
exploded with a range of explosion energies
Significant accretion for thousands of
seconds ndash days
If fallback fuels a jet with power
fmc2
May power ldquohypernovardquo or long duration
GRBWeak
supernova shock
Shock breakout X-Ray transient
2 ldquoBriefrdquo jet tengine tjet
Engine dies before jet breakout
Mildly relativistic shock breakout
MacFadyen (1999)
What made SN1998bw+GRB980425
1 Accretion powered hypernova w Nickel wind
MacFadyen (2002)
E~ 1052 erg M(Ni)~05 M
GRB from ~3 shock breakout (Tan et al 2001 Perna amp Vietri 2002)
Collapsars
bull Can make ldquolongrdquo GRBs in H stripped (WR) stars tengine gt tescape
bull Short bursts may be compact binary mergersbull Need SN failure amp angular momentum
ndash Low metallicity binary can help
bull Star can explode -gt SN if nickel is made Predicts GRBSN association Type Ibc
bull SNGRB ratio may depend on angular momentumbull ldquoNickel windrdquo can explode star -gt hypernova
ndash H env Type II (no GRB) no H Type I + GRB
GRBGW bull Long GRBs
ndash not brighter than SN in GW
ndash very far Gpc
ndash very rare lt 1 SN
bull Short GBsndash merging ns-bh binaries
ndash maybe closer than long bursts
ndash short delay between event and GRB
ndash good for SWIFTLIGO
Rates
bull SN 1s = 100000 day
bull GRB 1day (BATSE) = 1000day
bull GRB rate = 1 of SN rate
bull maybe more collapsars than GRBs
bull =gt more rapidly rotating SN
bull SN with collapsar engine
bull look for bright Type Ic (w broad lines)
SN GW
bull SN1998bwGRB980425
bull 40 Mpc
bull maybe dominant GRB
bull rapid rotaters
bull SNAPROTSE look for 1998bw 2003dh like SN
bull many light curves -gt better t_explode
Implications
bull Probe engine directly
bull collapse duration vs GRB duration
bull collapseGRB delay (internal vs external)
bull disk properties ndash low viscosity big disks
Issues
bull too much j =gt no GRB but bright GW
bull may need low metallicity for GRB
bull prefer high redshift
bull donrsquot know nearby rate
bull but 980425 may imply rate is high
bull look for weak GRBs like 980425
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
With decreasing metallicity the bindingenergy of the core and the size of the silicon core both increase making black hole formation more likely atlow metallicity Woosley Heger amp Weaver RMP (2002)
Black hole formation may be unavoidable for low metallicity
Solar metallicity
Low metallicity
In the absence of mass lossand magnetic fields there wouldbe abundant progenitors
Unfortunately nature has both
15 solar mass helium core born rotating rigidly at f times break up
The more difficult problem is the angular momentum Thisis a problem shared by all current GRB models that invokemassive stars
- What is a Gamma-Ray Burst
- Superbowl Burst
- Slide 3
- 135 models (1993)
- Slide 5
- Slide 6
- Slide 7
- GRB991121
- GRB030329SN2003DH
- Slide 10
- Slide 11
- Slide 12
- GRB central engine
- ldquoDelayedrdquo SN Explosion
- Pre-Supernova Density Structure
- Failure of delayed mechanism
- Stellar Rotation
- Slide 18
- Slide 19
- Collapsar Simulations
- Collapsar Disk Animation
- Disk Formation Movie
- Slide 23
- Slide 24
- Slide 25
- Collapsar results
- Slide 27
- Jet Birth
- Relativistic Jet Movie
- Collapsar stages
- Slide 31
- Slide 32
- Nickel Wind Movie
- Slide 34
- Slide 35
- Slide 36
- Slide 37
- Slide 38
- Collapsars
- GRBGW
- Rates
- SN GW
- Implications
- Issues
- Principle Results
- Slide 46
- Slide 47
-
135 models (1993)
Note most are Galactic and are ruled out for long bursts
GRB photons are made far away from engine
Canrsquot observe engine directly in light (neutrinos gravitational waves)
Electromagnetic process or neutrino annihilation to tap power of central compact object
Hyper-accreting black hole or high field neutron star (rotating)
Well-localized bursts are all ldquolong-softrdquo
ldquoshort-hardrdquo bursts
Duration (s)
hardness
Kulkarni et al
NTT image (May 1 1998) of SN 1998bw in the barred spiral galaxy ESO 184-G82 [Galama et al AampAS 138 465 (1999)]
WFC error box (8) for GRB 980425 and two NFI x-ray sources The IPN error arc is also shown
1) Were the two events the same thing
2) Was GRB 980425 an ordinary GRB seen off-axis
SN 1998bwGRB 980425
Bloom et al (ApJL2002)
GRB991121
see also Hjorth et al Fox et al Nature (2003)
extremely close = 800 Mpc
GRB030329SN2003DH
SN 1998bwGRB 980425
The supernova - a Type Ic - was very unusual
Large mass of 56Ni 03 - 09 solar masses (note jets acting alone do not make 56Ni) Sollerman et al ApJL 537 127 (2000) McKinzie amp Schaefer PASP 111 964 (1999)
Extreme energy and mass gt 1052 erg gt 10 Msun Iwamoto et al Nature 395 672 (1998) Woosley Eastman amp Schmidt ApJ 516 788 (1999) Mazzali et al ApJ 559 1047 (2001)
Exceptionally strong radio source Li amp Chevalier ApJ 526 716 (1999) Relativistic matter was ejected 1050 - 1051 erg Wieringa Kulkarni amp Frail AampAS 138 467 (1999) Frail et al ApJL (2001) astroph-0102282
Probability favors the GRB-SN association Pian et al ApJ 536 778 (2000)
Merging neutron star - black hole pairs
Strengths
a) Known event b) Plenty of angular momentum c) Rapid time scale d) High energy e) Well developed numerical models
Weaknesses a) Outside star forming regions
b) Beaming and energy may be inadequate for long bursts
But this model may still be good for a class of bursts calledthe ldquoshort hardrdquo bursts for which we have no counterpart informationyet (SWIFT)
Ruffert amp Janka Rosswog et al Lee et al Aloy et al
Requirements on the Central Engineand its Immediate Surroundings
(long-soft bursts)bull Provide adequate energy at high Lorentz factor
bull Collimate the emergent beam to approximately 01 radians
bull In the internal shock model provide a beam with rapidly variable Lorentz factor
bull Allow for the observed diverse GRB light curves
bull Last approximately 10 s but much longer in some cases
bull Explain diverse events like GRB 980425
bull Produce a (Type Ibc) supernova in some cases
bull Make bursts in star forming regions
GRB central engine
bull Relativity (SR amp GR)bull Magnetic Fieldsbull Rotation (progenitors)bull Nuclear Physicsbull Neutrinosbull EOSbull Turbulencebull 3Dbull Range of Lengthscales
Muller (1999)
ldquoDelayedrdquo SN Explosion
ac
Accretion vs Neutrino heating
Burrows (2001)
Pre-Supernova Density Structure
Woosley amp Weaver (1995)
Bigger stars
Higher entropy
Shallower density gradients
Fryer ApJ 522 413 (1999) Burrows (1999)
Bigger stars
1 Accrete faster amp longer
2 Larger binding energy amp smaller explosion energy
explosion
binding
Failure of delayed mechanism
Fukuda (1982)
Heger (2000)
Stellar Rotation
no mass lossMass loss
No B fields
Collapsars
Type Masssun BH Time Scale Distance Comment
I 15-40 He prompt 20 s all z neutrino-dominated disk
II 10-40 He delayed 20 s ndash 1 hr all z black hole by fall back
III gt130 He prompt ~20 s zgt10 time dilated redshifted (1+z) very energetic pair instability low Z
A rotating massive star whose core collapses to a black hole and produces an accretion disk
Type I is what we are usually talking aboutThe 40 solar mass limit comes from assuming that all stars above 100 solar masses on the main sequence are unstable (except Pop III)
IFTwo plausible conditions occur
1 Failure of neutrino powered SN explosion
a completeb partial (fallback)
2 Rotating stellar coresj gt 3 x 1016 cm2s
THEN
Rapidly accreting black hole (M~01 Ms)fed by collapsing star (tdyn ~ 446 s frac12 ~ 10 s)Disk formation
COLLAPSAR
Collapsar Simulations
bull pre-SN 15 Msun Helium starbull Newtonian Hydrodynamics (PPM)bull alpha viscositybull rotationbull photodisintegration (NSE alpha n p)bull neutrino cooling thermal + URCA optically thinbull Ideal nucleons radiation relativistic degenerate
electrons positionsbull 2D axisymmetric spherical gridbull self gravity pseudo-Newtonian (PW)bull Rin = 9 Rs Rout = 9000 Rs
MacFadyen amp Woosley (1999)
Collapsar Disk AnimationPPM hydrodynamics Paczynski-Witta potential EOS neutrino cooling nuclear reactions viscosity
Stellar collapse w rotation
Density structure No disk no wind
Note Accretion shock funnel clearing pole to equator density contrast fluctuating polar density
Initial model 15 Msun Helium (Wolf-Rayet) star evolved with mass loss
R= 8 x 108 cm
Show inner 1 in radius disk mass = 001 M_sun
Low viscosity =001
Disk Formation Movie
Accretion Shock
Disk formation
t = 75 s
PhotodisintegrationSiOC -gt free neutronsAnd protons Enhanced neutrino cooling
neutrino coolong allows
accretion
no cooling=gt
dynamically unstable
CDAF
Could emit GWs but
maybe no GRB
= 01 ltMgt = 007 Msun s = 13 x 1053 ergs
spin
mass
Use 1D neutrino cooled
ldquoslimrdquo disk models
from Popham et al (1999)
Collapsar results
bull Sustained accretion gt10sbull Sufficient energy bull Time scale set by He core collapsebull Disk-feeding time scale not disk-drainingbull Neutrino cooling allows accretionbull Neutrino annihilation energetically
possiblendash calculable in any case
Funnel geometry
channels any fireball
Density contrasts can
be huge
Ejet = f Maccc2
MHD
T = 57 ms
E = 5 x 1050 ergs
Edep = 28 x 1048 erg
Jet BirthThermal energy deposition focused by toroidal funnel structure
fmax ~ 06 - 4
Relativistic Jet Movie
Collapsar stages1 Iron core collapse disk formation
T~1010K ~108gcm-3 photodisintegration cooling pair capture disk is free nucleons (2 s)
2 Polar density declines to allow jet birthfrac12v3 Edep (2-5 s)
3 Jet tunnels out of star (5 s) Wolf-Rayet4 Jet powered for ~10 more seconds
Evacuates polar channel and reaches asymptotic speed (10 s)
T_GRB T_collapse
Jupiter
Red Supergiant
R~1013 cm
Blue Supergiant
R~1012 cm
Wolf-Rayet Star
R~1011 cm
Type Ib or Ic
Supernova
Supernovae
Ia
WD cosmology
Type II
Hydrogen
Type I
No Hydrogen
Ib Ic
exploding WR
thermonuclear old pop E galaxies
core collapse massive stars
Nickel Wind Movie
ldquoNickel Windrdquo
T gt 5 x 109 K
Fallback in weak SN explosions
Shock reaches
surface of star but parts of star are
not ejected to infinity
Fallback accretion Mms ~ 25 Msun Same star
exploded with a range of explosion energies
Significant accretion for thousands of
seconds ndash days
If fallback fuels a jet with power
fmc2
May power ldquohypernovardquo or long duration
GRBWeak
supernova shock
Shock breakout X-Ray transient
2 ldquoBriefrdquo jet tengine tjet
Engine dies before jet breakout
Mildly relativistic shock breakout
MacFadyen (1999)
What made SN1998bw+GRB980425
1 Accretion powered hypernova w Nickel wind
MacFadyen (2002)
E~ 1052 erg M(Ni)~05 M
GRB from ~3 shock breakout (Tan et al 2001 Perna amp Vietri 2002)
Collapsars
bull Can make ldquolongrdquo GRBs in H stripped (WR) stars tengine gt tescape
bull Short bursts may be compact binary mergersbull Need SN failure amp angular momentum
ndash Low metallicity binary can help
bull Star can explode -gt SN if nickel is made Predicts GRBSN association Type Ibc
bull SNGRB ratio may depend on angular momentumbull ldquoNickel windrdquo can explode star -gt hypernova
ndash H env Type II (no GRB) no H Type I + GRB
GRBGW bull Long GRBs
ndash not brighter than SN in GW
ndash very far Gpc
ndash very rare lt 1 SN
bull Short GBsndash merging ns-bh binaries
ndash maybe closer than long bursts
ndash short delay between event and GRB
ndash good for SWIFTLIGO
Rates
bull SN 1s = 100000 day
bull GRB 1day (BATSE) = 1000day
bull GRB rate = 1 of SN rate
bull maybe more collapsars than GRBs
bull =gt more rapidly rotating SN
bull SN with collapsar engine
bull look for bright Type Ic (w broad lines)
SN GW
bull SN1998bwGRB980425
bull 40 Mpc
bull maybe dominant GRB
bull rapid rotaters
bull SNAPROTSE look for 1998bw 2003dh like SN
bull many light curves -gt better t_explode
Implications
bull Probe engine directly
bull collapse duration vs GRB duration
bull collapseGRB delay (internal vs external)
bull disk properties ndash low viscosity big disks
Issues
bull too much j =gt no GRB but bright GW
bull may need low metallicity for GRB
bull prefer high redshift
bull donrsquot know nearby rate
bull but 980425 may imply rate is high
bull look for weak GRBs like 980425
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
With decreasing metallicity the bindingenergy of the core and the size of the silicon core both increase making black hole formation more likely atlow metallicity Woosley Heger amp Weaver RMP (2002)
Black hole formation may be unavoidable for low metallicity
Solar metallicity
Low metallicity
In the absence of mass lossand magnetic fields there wouldbe abundant progenitors
Unfortunately nature has both
15 solar mass helium core born rotating rigidly at f times break up
The more difficult problem is the angular momentum Thisis a problem shared by all current GRB models that invokemassive stars
- What is a Gamma-Ray Burst
- Superbowl Burst
- Slide 3
- 135 models (1993)
- Slide 5
- Slide 6
- Slide 7
- GRB991121
- GRB030329SN2003DH
- Slide 10
- Slide 11
- Slide 12
- GRB central engine
- ldquoDelayedrdquo SN Explosion
- Pre-Supernova Density Structure
- Failure of delayed mechanism
- Stellar Rotation
- Slide 18
- Slide 19
- Collapsar Simulations
- Collapsar Disk Animation
- Disk Formation Movie
- Slide 23
- Slide 24
- Slide 25
- Collapsar results
- Slide 27
- Jet Birth
- Relativistic Jet Movie
- Collapsar stages
- Slide 31
- Slide 32
- Nickel Wind Movie
- Slide 34
- Slide 35
- Slide 36
- Slide 37
- Slide 38
- Collapsars
- GRBGW
- Rates
- SN GW
- Implications
- Issues
- Principle Results
- Slide 46
- Slide 47
-
GRB photons are made far away from engine
Canrsquot observe engine directly in light (neutrinos gravitational waves)
Electromagnetic process or neutrino annihilation to tap power of central compact object
Hyper-accreting black hole or high field neutron star (rotating)
Well-localized bursts are all ldquolong-softrdquo
ldquoshort-hardrdquo bursts
Duration (s)
hardness
Kulkarni et al
NTT image (May 1 1998) of SN 1998bw in the barred spiral galaxy ESO 184-G82 [Galama et al AampAS 138 465 (1999)]
WFC error box (8) for GRB 980425 and two NFI x-ray sources The IPN error arc is also shown
1) Were the two events the same thing
2) Was GRB 980425 an ordinary GRB seen off-axis
SN 1998bwGRB 980425
Bloom et al (ApJL2002)
GRB991121
see also Hjorth et al Fox et al Nature (2003)
extremely close = 800 Mpc
GRB030329SN2003DH
SN 1998bwGRB 980425
The supernova - a Type Ic - was very unusual
Large mass of 56Ni 03 - 09 solar masses (note jets acting alone do not make 56Ni) Sollerman et al ApJL 537 127 (2000) McKinzie amp Schaefer PASP 111 964 (1999)
Extreme energy and mass gt 1052 erg gt 10 Msun Iwamoto et al Nature 395 672 (1998) Woosley Eastman amp Schmidt ApJ 516 788 (1999) Mazzali et al ApJ 559 1047 (2001)
Exceptionally strong radio source Li amp Chevalier ApJ 526 716 (1999) Relativistic matter was ejected 1050 - 1051 erg Wieringa Kulkarni amp Frail AampAS 138 467 (1999) Frail et al ApJL (2001) astroph-0102282
Probability favors the GRB-SN association Pian et al ApJ 536 778 (2000)
Merging neutron star - black hole pairs
Strengths
a) Known event b) Plenty of angular momentum c) Rapid time scale d) High energy e) Well developed numerical models
Weaknesses a) Outside star forming regions
b) Beaming and energy may be inadequate for long bursts
But this model may still be good for a class of bursts calledthe ldquoshort hardrdquo bursts for which we have no counterpart informationyet (SWIFT)
Ruffert amp Janka Rosswog et al Lee et al Aloy et al
Requirements on the Central Engineand its Immediate Surroundings
(long-soft bursts)bull Provide adequate energy at high Lorentz factor
bull Collimate the emergent beam to approximately 01 radians
bull In the internal shock model provide a beam with rapidly variable Lorentz factor
bull Allow for the observed diverse GRB light curves
bull Last approximately 10 s but much longer in some cases
bull Explain diverse events like GRB 980425
bull Produce a (Type Ibc) supernova in some cases
bull Make bursts in star forming regions
GRB central engine
bull Relativity (SR amp GR)bull Magnetic Fieldsbull Rotation (progenitors)bull Nuclear Physicsbull Neutrinosbull EOSbull Turbulencebull 3Dbull Range of Lengthscales
Muller (1999)
ldquoDelayedrdquo SN Explosion
ac
Accretion vs Neutrino heating
Burrows (2001)
Pre-Supernova Density Structure
Woosley amp Weaver (1995)
Bigger stars
Higher entropy
Shallower density gradients
Fryer ApJ 522 413 (1999) Burrows (1999)
Bigger stars
1 Accrete faster amp longer
2 Larger binding energy amp smaller explosion energy
explosion
binding
Failure of delayed mechanism
Fukuda (1982)
Heger (2000)
Stellar Rotation
no mass lossMass loss
No B fields
Collapsars
Type Masssun BH Time Scale Distance Comment
I 15-40 He prompt 20 s all z neutrino-dominated disk
II 10-40 He delayed 20 s ndash 1 hr all z black hole by fall back
III gt130 He prompt ~20 s zgt10 time dilated redshifted (1+z) very energetic pair instability low Z
A rotating massive star whose core collapses to a black hole and produces an accretion disk
Type I is what we are usually talking aboutThe 40 solar mass limit comes from assuming that all stars above 100 solar masses on the main sequence are unstable (except Pop III)
IFTwo plausible conditions occur
1 Failure of neutrino powered SN explosion
a completeb partial (fallback)
2 Rotating stellar coresj gt 3 x 1016 cm2s
THEN
Rapidly accreting black hole (M~01 Ms)fed by collapsing star (tdyn ~ 446 s frac12 ~ 10 s)Disk formation
COLLAPSAR
Collapsar Simulations
bull pre-SN 15 Msun Helium starbull Newtonian Hydrodynamics (PPM)bull alpha viscositybull rotationbull photodisintegration (NSE alpha n p)bull neutrino cooling thermal + URCA optically thinbull Ideal nucleons radiation relativistic degenerate
electrons positionsbull 2D axisymmetric spherical gridbull self gravity pseudo-Newtonian (PW)bull Rin = 9 Rs Rout = 9000 Rs
MacFadyen amp Woosley (1999)
Collapsar Disk AnimationPPM hydrodynamics Paczynski-Witta potential EOS neutrino cooling nuclear reactions viscosity
Stellar collapse w rotation
Density structure No disk no wind
Note Accretion shock funnel clearing pole to equator density contrast fluctuating polar density
Initial model 15 Msun Helium (Wolf-Rayet) star evolved with mass loss
R= 8 x 108 cm
Show inner 1 in radius disk mass = 001 M_sun
Low viscosity =001
Disk Formation Movie
Accretion Shock
Disk formation
t = 75 s
PhotodisintegrationSiOC -gt free neutronsAnd protons Enhanced neutrino cooling
neutrino coolong allows
accretion
no cooling=gt
dynamically unstable
CDAF
Could emit GWs but
maybe no GRB
= 01 ltMgt = 007 Msun s = 13 x 1053 ergs
spin
mass
Use 1D neutrino cooled
ldquoslimrdquo disk models
from Popham et al (1999)
Collapsar results
bull Sustained accretion gt10sbull Sufficient energy bull Time scale set by He core collapsebull Disk-feeding time scale not disk-drainingbull Neutrino cooling allows accretionbull Neutrino annihilation energetically
possiblendash calculable in any case
Funnel geometry
channels any fireball
Density contrasts can
be huge
Ejet = f Maccc2
MHD
T = 57 ms
E = 5 x 1050 ergs
Edep = 28 x 1048 erg
Jet BirthThermal energy deposition focused by toroidal funnel structure
fmax ~ 06 - 4
Relativistic Jet Movie
Collapsar stages1 Iron core collapse disk formation
T~1010K ~108gcm-3 photodisintegration cooling pair capture disk is free nucleons (2 s)
2 Polar density declines to allow jet birthfrac12v3 Edep (2-5 s)
3 Jet tunnels out of star (5 s) Wolf-Rayet4 Jet powered for ~10 more seconds
Evacuates polar channel and reaches asymptotic speed (10 s)
T_GRB T_collapse
Jupiter
Red Supergiant
R~1013 cm
Blue Supergiant
R~1012 cm
Wolf-Rayet Star
R~1011 cm
Type Ib or Ic
Supernova
Supernovae
Ia
WD cosmology
Type II
Hydrogen
Type I
No Hydrogen
Ib Ic
exploding WR
thermonuclear old pop E galaxies
core collapse massive stars
Nickel Wind Movie
ldquoNickel Windrdquo
T gt 5 x 109 K
Fallback in weak SN explosions
Shock reaches
surface of star but parts of star are
not ejected to infinity
Fallback accretion Mms ~ 25 Msun Same star
exploded with a range of explosion energies
Significant accretion for thousands of
seconds ndash days
If fallback fuels a jet with power
fmc2
May power ldquohypernovardquo or long duration
GRBWeak
supernova shock
Shock breakout X-Ray transient
2 ldquoBriefrdquo jet tengine tjet
Engine dies before jet breakout
Mildly relativistic shock breakout
MacFadyen (1999)
What made SN1998bw+GRB980425
1 Accretion powered hypernova w Nickel wind
MacFadyen (2002)
E~ 1052 erg M(Ni)~05 M
GRB from ~3 shock breakout (Tan et al 2001 Perna amp Vietri 2002)
Collapsars
bull Can make ldquolongrdquo GRBs in H stripped (WR) stars tengine gt tescape
bull Short bursts may be compact binary mergersbull Need SN failure amp angular momentum
ndash Low metallicity binary can help
bull Star can explode -gt SN if nickel is made Predicts GRBSN association Type Ibc
bull SNGRB ratio may depend on angular momentumbull ldquoNickel windrdquo can explode star -gt hypernova
ndash H env Type II (no GRB) no H Type I + GRB
GRBGW bull Long GRBs
ndash not brighter than SN in GW
ndash very far Gpc
ndash very rare lt 1 SN
bull Short GBsndash merging ns-bh binaries
ndash maybe closer than long bursts
ndash short delay between event and GRB
ndash good for SWIFTLIGO
Rates
bull SN 1s = 100000 day
bull GRB 1day (BATSE) = 1000day
bull GRB rate = 1 of SN rate
bull maybe more collapsars than GRBs
bull =gt more rapidly rotating SN
bull SN with collapsar engine
bull look for bright Type Ic (w broad lines)
SN GW
bull SN1998bwGRB980425
bull 40 Mpc
bull maybe dominant GRB
bull rapid rotaters
bull SNAPROTSE look for 1998bw 2003dh like SN
bull many light curves -gt better t_explode
Implications
bull Probe engine directly
bull collapse duration vs GRB duration
bull collapseGRB delay (internal vs external)
bull disk properties ndash low viscosity big disks
Issues
bull too much j =gt no GRB but bright GW
bull may need low metallicity for GRB
bull prefer high redshift
bull donrsquot know nearby rate
bull but 980425 may imply rate is high
bull look for weak GRBs like 980425
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
With decreasing metallicity the bindingenergy of the core and the size of the silicon core both increase making black hole formation more likely atlow metallicity Woosley Heger amp Weaver RMP (2002)
Black hole formation may be unavoidable for low metallicity
Solar metallicity
Low metallicity
In the absence of mass lossand magnetic fields there wouldbe abundant progenitors
Unfortunately nature has both
15 solar mass helium core born rotating rigidly at f times break up
The more difficult problem is the angular momentum Thisis a problem shared by all current GRB models that invokemassive stars
- What is a Gamma-Ray Burst
- Superbowl Burst
- Slide 3
- 135 models (1993)
- Slide 5
- Slide 6
- Slide 7
- GRB991121
- GRB030329SN2003DH
- Slide 10
- Slide 11
- Slide 12
- GRB central engine
- ldquoDelayedrdquo SN Explosion
- Pre-Supernova Density Structure
- Failure of delayed mechanism
- Stellar Rotation
- Slide 18
- Slide 19
- Collapsar Simulations
- Collapsar Disk Animation
- Disk Formation Movie
- Slide 23
- Slide 24
- Slide 25
- Collapsar results
- Slide 27
- Jet Birth
- Relativistic Jet Movie
- Collapsar stages
- Slide 31
- Slide 32
- Nickel Wind Movie
- Slide 34
- Slide 35
- Slide 36
- Slide 37
- Slide 38
- Collapsars
- GRBGW
- Rates
- SN GW
- Implications
- Issues
- Principle Results
- Slide 46
- Slide 47
-
Well-localized bursts are all ldquolong-softrdquo
ldquoshort-hardrdquo bursts
Duration (s)
hardness
Kulkarni et al
NTT image (May 1 1998) of SN 1998bw in the barred spiral galaxy ESO 184-G82 [Galama et al AampAS 138 465 (1999)]
WFC error box (8) for GRB 980425 and two NFI x-ray sources The IPN error arc is also shown
1) Were the two events the same thing
2) Was GRB 980425 an ordinary GRB seen off-axis
SN 1998bwGRB 980425
Bloom et al (ApJL2002)
GRB991121
see also Hjorth et al Fox et al Nature (2003)
extremely close = 800 Mpc
GRB030329SN2003DH
SN 1998bwGRB 980425
The supernova - a Type Ic - was very unusual
Large mass of 56Ni 03 - 09 solar masses (note jets acting alone do not make 56Ni) Sollerman et al ApJL 537 127 (2000) McKinzie amp Schaefer PASP 111 964 (1999)
Extreme energy and mass gt 1052 erg gt 10 Msun Iwamoto et al Nature 395 672 (1998) Woosley Eastman amp Schmidt ApJ 516 788 (1999) Mazzali et al ApJ 559 1047 (2001)
Exceptionally strong radio source Li amp Chevalier ApJ 526 716 (1999) Relativistic matter was ejected 1050 - 1051 erg Wieringa Kulkarni amp Frail AampAS 138 467 (1999) Frail et al ApJL (2001) astroph-0102282
Probability favors the GRB-SN association Pian et al ApJ 536 778 (2000)
Merging neutron star - black hole pairs
Strengths
a) Known event b) Plenty of angular momentum c) Rapid time scale d) High energy e) Well developed numerical models
Weaknesses a) Outside star forming regions
b) Beaming and energy may be inadequate for long bursts
But this model may still be good for a class of bursts calledthe ldquoshort hardrdquo bursts for which we have no counterpart informationyet (SWIFT)
Ruffert amp Janka Rosswog et al Lee et al Aloy et al
Requirements on the Central Engineand its Immediate Surroundings
(long-soft bursts)bull Provide adequate energy at high Lorentz factor
bull Collimate the emergent beam to approximately 01 radians
bull In the internal shock model provide a beam with rapidly variable Lorentz factor
bull Allow for the observed diverse GRB light curves
bull Last approximately 10 s but much longer in some cases
bull Explain diverse events like GRB 980425
bull Produce a (Type Ibc) supernova in some cases
bull Make bursts in star forming regions
GRB central engine
bull Relativity (SR amp GR)bull Magnetic Fieldsbull Rotation (progenitors)bull Nuclear Physicsbull Neutrinosbull EOSbull Turbulencebull 3Dbull Range of Lengthscales
Muller (1999)
ldquoDelayedrdquo SN Explosion
ac
Accretion vs Neutrino heating
Burrows (2001)
Pre-Supernova Density Structure
Woosley amp Weaver (1995)
Bigger stars
Higher entropy
Shallower density gradients
Fryer ApJ 522 413 (1999) Burrows (1999)
Bigger stars
1 Accrete faster amp longer
2 Larger binding energy amp smaller explosion energy
explosion
binding
Failure of delayed mechanism
Fukuda (1982)
Heger (2000)
Stellar Rotation
no mass lossMass loss
No B fields
Collapsars
Type Masssun BH Time Scale Distance Comment
I 15-40 He prompt 20 s all z neutrino-dominated disk
II 10-40 He delayed 20 s ndash 1 hr all z black hole by fall back
III gt130 He prompt ~20 s zgt10 time dilated redshifted (1+z) very energetic pair instability low Z
A rotating massive star whose core collapses to a black hole and produces an accretion disk
Type I is what we are usually talking aboutThe 40 solar mass limit comes from assuming that all stars above 100 solar masses on the main sequence are unstable (except Pop III)
IFTwo plausible conditions occur
1 Failure of neutrino powered SN explosion
a completeb partial (fallback)
2 Rotating stellar coresj gt 3 x 1016 cm2s
THEN
Rapidly accreting black hole (M~01 Ms)fed by collapsing star (tdyn ~ 446 s frac12 ~ 10 s)Disk formation
COLLAPSAR
Collapsar Simulations
bull pre-SN 15 Msun Helium starbull Newtonian Hydrodynamics (PPM)bull alpha viscositybull rotationbull photodisintegration (NSE alpha n p)bull neutrino cooling thermal + URCA optically thinbull Ideal nucleons radiation relativistic degenerate
electrons positionsbull 2D axisymmetric spherical gridbull self gravity pseudo-Newtonian (PW)bull Rin = 9 Rs Rout = 9000 Rs
MacFadyen amp Woosley (1999)
Collapsar Disk AnimationPPM hydrodynamics Paczynski-Witta potential EOS neutrino cooling nuclear reactions viscosity
Stellar collapse w rotation
Density structure No disk no wind
Note Accretion shock funnel clearing pole to equator density contrast fluctuating polar density
Initial model 15 Msun Helium (Wolf-Rayet) star evolved with mass loss
R= 8 x 108 cm
Show inner 1 in radius disk mass = 001 M_sun
Low viscosity =001
Disk Formation Movie
Accretion Shock
Disk formation
t = 75 s
PhotodisintegrationSiOC -gt free neutronsAnd protons Enhanced neutrino cooling
neutrino coolong allows
accretion
no cooling=gt
dynamically unstable
CDAF
Could emit GWs but
maybe no GRB
= 01 ltMgt = 007 Msun s = 13 x 1053 ergs
spin
mass
Use 1D neutrino cooled
ldquoslimrdquo disk models
from Popham et al (1999)
Collapsar results
bull Sustained accretion gt10sbull Sufficient energy bull Time scale set by He core collapsebull Disk-feeding time scale not disk-drainingbull Neutrino cooling allows accretionbull Neutrino annihilation energetically
possiblendash calculable in any case
Funnel geometry
channels any fireball
Density contrasts can
be huge
Ejet = f Maccc2
MHD
T = 57 ms
E = 5 x 1050 ergs
Edep = 28 x 1048 erg
Jet BirthThermal energy deposition focused by toroidal funnel structure
fmax ~ 06 - 4
Relativistic Jet Movie
Collapsar stages1 Iron core collapse disk formation
T~1010K ~108gcm-3 photodisintegration cooling pair capture disk is free nucleons (2 s)
2 Polar density declines to allow jet birthfrac12v3 Edep (2-5 s)
3 Jet tunnels out of star (5 s) Wolf-Rayet4 Jet powered for ~10 more seconds
Evacuates polar channel and reaches asymptotic speed (10 s)
T_GRB T_collapse
Jupiter
Red Supergiant
R~1013 cm
Blue Supergiant
R~1012 cm
Wolf-Rayet Star
R~1011 cm
Type Ib or Ic
Supernova
Supernovae
Ia
WD cosmology
Type II
Hydrogen
Type I
No Hydrogen
Ib Ic
exploding WR
thermonuclear old pop E galaxies
core collapse massive stars
Nickel Wind Movie
ldquoNickel Windrdquo
T gt 5 x 109 K
Fallback in weak SN explosions
Shock reaches
surface of star but parts of star are
not ejected to infinity
Fallback accretion Mms ~ 25 Msun Same star
exploded with a range of explosion energies
Significant accretion for thousands of
seconds ndash days
If fallback fuels a jet with power
fmc2
May power ldquohypernovardquo or long duration
GRBWeak
supernova shock
Shock breakout X-Ray transient
2 ldquoBriefrdquo jet tengine tjet
Engine dies before jet breakout
Mildly relativistic shock breakout
MacFadyen (1999)
What made SN1998bw+GRB980425
1 Accretion powered hypernova w Nickel wind
MacFadyen (2002)
E~ 1052 erg M(Ni)~05 M
GRB from ~3 shock breakout (Tan et al 2001 Perna amp Vietri 2002)
Collapsars
bull Can make ldquolongrdquo GRBs in H stripped (WR) stars tengine gt tescape
bull Short bursts may be compact binary mergersbull Need SN failure amp angular momentum
ndash Low metallicity binary can help
bull Star can explode -gt SN if nickel is made Predicts GRBSN association Type Ibc
bull SNGRB ratio may depend on angular momentumbull ldquoNickel windrdquo can explode star -gt hypernova
ndash H env Type II (no GRB) no H Type I + GRB
GRBGW bull Long GRBs
ndash not brighter than SN in GW
ndash very far Gpc
ndash very rare lt 1 SN
bull Short GBsndash merging ns-bh binaries
ndash maybe closer than long bursts
ndash short delay between event and GRB
ndash good for SWIFTLIGO
Rates
bull SN 1s = 100000 day
bull GRB 1day (BATSE) = 1000day
bull GRB rate = 1 of SN rate
bull maybe more collapsars than GRBs
bull =gt more rapidly rotating SN
bull SN with collapsar engine
bull look for bright Type Ic (w broad lines)
SN GW
bull SN1998bwGRB980425
bull 40 Mpc
bull maybe dominant GRB
bull rapid rotaters
bull SNAPROTSE look for 1998bw 2003dh like SN
bull many light curves -gt better t_explode
Implications
bull Probe engine directly
bull collapse duration vs GRB duration
bull collapseGRB delay (internal vs external)
bull disk properties ndash low viscosity big disks
Issues
bull too much j =gt no GRB but bright GW
bull may need low metallicity for GRB
bull prefer high redshift
bull donrsquot know nearby rate
bull but 980425 may imply rate is high
bull look for weak GRBs like 980425
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
With decreasing metallicity the bindingenergy of the core and the size of the silicon core both increase making black hole formation more likely atlow metallicity Woosley Heger amp Weaver RMP (2002)
Black hole formation may be unavoidable for low metallicity
Solar metallicity
Low metallicity
In the absence of mass lossand magnetic fields there wouldbe abundant progenitors
Unfortunately nature has both
15 solar mass helium core born rotating rigidly at f times break up
The more difficult problem is the angular momentum Thisis a problem shared by all current GRB models that invokemassive stars
- What is a Gamma-Ray Burst
- Superbowl Burst
- Slide 3
- 135 models (1993)
- Slide 5
- Slide 6
- Slide 7
- GRB991121
- GRB030329SN2003DH
- Slide 10
- Slide 11
- Slide 12
- GRB central engine
- ldquoDelayedrdquo SN Explosion
- Pre-Supernova Density Structure
- Failure of delayed mechanism
- Stellar Rotation
- Slide 18
- Slide 19
- Collapsar Simulations
- Collapsar Disk Animation
- Disk Formation Movie
- Slide 23
- Slide 24
- Slide 25
- Collapsar results
- Slide 27
- Jet Birth
- Relativistic Jet Movie
- Collapsar stages
- Slide 31
- Slide 32
- Nickel Wind Movie
- Slide 34
- Slide 35
- Slide 36
- Slide 37
- Slide 38
- Collapsars
- GRBGW
- Rates
- SN GW
- Implications
- Issues
- Principle Results
- Slide 46
- Slide 47
-
NTT image (May 1 1998) of SN 1998bw in the barred spiral galaxy ESO 184-G82 [Galama et al AampAS 138 465 (1999)]
WFC error box (8) for GRB 980425 and two NFI x-ray sources The IPN error arc is also shown
1) Were the two events the same thing
2) Was GRB 980425 an ordinary GRB seen off-axis
SN 1998bwGRB 980425
Bloom et al (ApJL2002)
GRB991121
see also Hjorth et al Fox et al Nature (2003)
extremely close = 800 Mpc
GRB030329SN2003DH
SN 1998bwGRB 980425
The supernova - a Type Ic - was very unusual
Large mass of 56Ni 03 - 09 solar masses (note jets acting alone do not make 56Ni) Sollerman et al ApJL 537 127 (2000) McKinzie amp Schaefer PASP 111 964 (1999)
Extreme energy and mass gt 1052 erg gt 10 Msun Iwamoto et al Nature 395 672 (1998) Woosley Eastman amp Schmidt ApJ 516 788 (1999) Mazzali et al ApJ 559 1047 (2001)
Exceptionally strong radio source Li amp Chevalier ApJ 526 716 (1999) Relativistic matter was ejected 1050 - 1051 erg Wieringa Kulkarni amp Frail AampAS 138 467 (1999) Frail et al ApJL (2001) astroph-0102282
Probability favors the GRB-SN association Pian et al ApJ 536 778 (2000)
Merging neutron star - black hole pairs
Strengths
a) Known event b) Plenty of angular momentum c) Rapid time scale d) High energy e) Well developed numerical models
Weaknesses a) Outside star forming regions
b) Beaming and energy may be inadequate for long bursts
But this model may still be good for a class of bursts calledthe ldquoshort hardrdquo bursts for which we have no counterpart informationyet (SWIFT)
Ruffert amp Janka Rosswog et al Lee et al Aloy et al
Requirements on the Central Engineand its Immediate Surroundings
(long-soft bursts)bull Provide adequate energy at high Lorentz factor
bull Collimate the emergent beam to approximately 01 radians
bull In the internal shock model provide a beam with rapidly variable Lorentz factor
bull Allow for the observed diverse GRB light curves
bull Last approximately 10 s but much longer in some cases
bull Explain diverse events like GRB 980425
bull Produce a (Type Ibc) supernova in some cases
bull Make bursts in star forming regions
GRB central engine
bull Relativity (SR amp GR)bull Magnetic Fieldsbull Rotation (progenitors)bull Nuclear Physicsbull Neutrinosbull EOSbull Turbulencebull 3Dbull Range of Lengthscales
Muller (1999)
ldquoDelayedrdquo SN Explosion
ac
Accretion vs Neutrino heating
Burrows (2001)
Pre-Supernova Density Structure
Woosley amp Weaver (1995)
Bigger stars
Higher entropy
Shallower density gradients
Fryer ApJ 522 413 (1999) Burrows (1999)
Bigger stars
1 Accrete faster amp longer
2 Larger binding energy amp smaller explosion energy
explosion
binding
Failure of delayed mechanism
Fukuda (1982)
Heger (2000)
Stellar Rotation
no mass lossMass loss
No B fields
Collapsars
Type Masssun BH Time Scale Distance Comment
I 15-40 He prompt 20 s all z neutrino-dominated disk
II 10-40 He delayed 20 s ndash 1 hr all z black hole by fall back
III gt130 He prompt ~20 s zgt10 time dilated redshifted (1+z) very energetic pair instability low Z
A rotating massive star whose core collapses to a black hole and produces an accretion disk
Type I is what we are usually talking aboutThe 40 solar mass limit comes from assuming that all stars above 100 solar masses on the main sequence are unstable (except Pop III)
IFTwo plausible conditions occur
1 Failure of neutrino powered SN explosion
a completeb partial (fallback)
2 Rotating stellar coresj gt 3 x 1016 cm2s
THEN
Rapidly accreting black hole (M~01 Ms)fed by collapsing star (tdyn ~ 446 s frac12 ~ 10 s)Disk formation
COLLAPSAR
Collapsar Simulations
bull pre-SN 15 Msun Helium starbull Newtonian Hydrodynamics (PPM)bull alpha viscositybull rotationbull photodisintegration (NSE alpha n p)bull neutrino cooling thermal + URCA optically thinbull Ideal nucleons radiation relativistic degenerate
electrons positionsbull 2D axisymmetric spherical gridbull self gravity pseudo-Newtonian (PW)bull Rin = 9 Rs Rout = 9000 Rs
MacFadyen amp Woosley (1999)
Collapsar Disk AnimationPPM hydrodynamics Paczynski-Witta potential EOS neutrino cooling nuclear reactions viscosity
Stellar collapse w rotation
Density structure No disk no wind
Note Accretion shock funnel clearing pole to equator density contrast fluctuating polar density
Initial model 15 Msun Helium (Wolf-Rayet) star evolved with mass loss
R= 8 x 108 cm
Show inner 1 in radius disk mass = 001 M_sun
Low viscosity =001
Disk Formation Movie
Accretion Shock
Disk formation
t = 75 s
PhotodisintegrationSiOC -gt free neutronsAnd protons Enhanced neutrino cooling
neutrino coolong allows
accretion
no cooling=gt
dynamically unstable
CDAF
Could emit GWs but
maybe no GRB
= 01 ltMgt = 007 Msun s = 13 x 1053 ergs
spin
mass
Use 1D neutrino cooled
ldquoslimrdquo disk models
from Popham et al (1999)
Collapsar results
bull Sustained accretion gt10sbull Sufficient energy bull Time scale set by He core collapsebull Disk-feeding time scale not disk-drainingbull Neutrino cooling allows accretionbull Neutrino annihilation energetically
possiblendash calculable in any case
Funnel geometry
channels any fireball
Density contrasts can
be huge
Ejet = f Maccc2
MHD
T = 57 ms
E = 5 x 1050 ergs
Edep = 28 x 1048 erg
Jet BirthThermal energy deposition focused by toroidal funnel structure
fmax ~ 06 - 4
Relativistic Jet Movie
Collapsar stages1 Iron core collapse disk formation
T~1010K ~108gcm-3 photodisintegration cooling pair capture disk is free nucleons (2 s)
2 Polar density declines to allow jet birthfrac12v3 Edep (2-5 s)
3 Jet tunnels out of star (5 s) Wolf-Rayet4 Jet powered for ~10 more seconds
Evacuates polar channel and reaches asymptotic speed (10 s)
T_GRB T_collapse
Jupiter
Red Supergiant
R~1013 cm
Blue Supergiant
R~1012 cm
Wolf-Rayet Star
R~1011 cm
Type Ib or Ic
Supernova
Supernovae
Ia
WD cosmology
Type II
Hydrogen
Type I
No Hydrogen
Ib Ic
exploding WR
thermonuclear old pop E galaxies
core collapse massive stars
Nickel Wind Movie
ldquoNickel Windrdquo
T gt 5 x 109 K
Fallback in weak SN explosions
Shock reaches
surface of star but parts of star are
not ejected to infinity
Fallback accretion Mms ~ 25 Msun Same star
exploded with a range of explosion energies
Significant accretion for thousands of
seconds ndash days
If fallback fuels a jet with power
fmc2
May power ldquohypernovardquo or long duration
GRBWeak
supernova shock
Shock breakout X-Ray transient
2 ldquoBriefrdquo jet tengine tjet
Engine dies before jet breakout
Mildly relativistic shock breakout
MacFadyen (1999)
What made SN1998bw+GRB980425
1 Accretion powered hypernova w Nickel wind
MacFadyen (2002)
E~ 1052 erg M(Ni)~05 M
GRB from ~3 shock breakout (Tan et al 2001 Perna amp Vietri 2002)
Collapsars
bull Can make ldquolongrdquo GRBs in H stripped (WR) stars tengine gt tescape
bull Short bursts may be compact binary mergersbull Need SN failure amp angular momentum
ndash Low metallicity binary can help
bull Star can explode -gt SN if nickel is made Predicts GRBSN association Type Ibc
bull SNGRB ratio may depend on angular momentumbull ldquoNickel windrdquo can explode star -gt hypernova
ndash H env Type II (no GRB) no H Type I + GRB
GRBGW bull Long GRBs
ndash not brighter than SN in GW
ndash very far Gpc
ndash very rare lt 1 SN
bull Short GBsndash merging ns-bh binaries
ndash maybe closer than long bursts
ndash short delay between event and GRB
ndash good for SWIFTLIGO
Rates
bull SN 1s = 100000 day
bull GRB 1day (BATSE) = 1000day
bull GRB rate = 1 of SN rate
bull maybe more collapsars than GRBs
bull =gt more rapidly rotating SN
bull SN with collapsar engine
bull look for bright Type Ic (w broad lines)
SN GW
bull SN1998bwGRB980425
bull 40 Mpc
bull maybe dominant GRB
bull rapid rotaters
bull SNAPROTSE look for 1998bw 2003dh like SN
bull many light curves -gt better t_explode
Implications
bull Probe engine directly
bull collapse duration vs GRB duration
bull collapseGRB delay (internal vs external)
bull disk properties ndash low viscosity big disks
Issues
bull too much j =gt no GRB but bright GW
bull may need low metallicity for GRB
bull prefer high redshift
bull donrsquot know nearby rate
bull but 980425 may imply rate is high
bull look for weak GRBs like 980425
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
With decreasing metallicity the bindingenergy of the core and the size of the silicon core both increase making black hole formation more likely atlow metallicity Woosley Heger amp Weaver RMP (2002)
Black hole formation may be unavoidable for low metallicity
Solar metallicity
Low metallicity
In the absence of mass lossand magnetic fields there wouldbe abundant progenitors
Unfortunately nature has both
15 solar mass helium core born rotating rigidly at f times break up
The more difficult problem is the angular momentum Thisis a problem shared by all current GRB models that invokemassive stars
- What is a Gamma-Ray Burst
- Superbowl Burst
- Slide 3
- 135 models (1993)
- Slide 5
- Slide 6
- Slide 7
- GRB991121
- GRB030329SN2003DH
- Slide 10
- Slide 11
- Slide 12
- GRB central engine
- ldquoDelayedrdquo SN Explosion
- Pre-Supernova Density Structure
- Failure of delayed mechanism
- Stellar Rotation
- Slide 18
- Slide 19
- Collapsar Simulations
- Collapsar Disk Animation
- Disk Formation Movie
- Slide 23
- Slide 24
- Slide 25
- Collapsar results
- Slide 27
- Jet Birth
- Relativistic Jet Movie
- Collapsar stages
- Slide 31
- Slide 32
- Nickel Wind Movie
- Slide 34
- Slide 35
- Slide 36
- Slide 37
- Slide 38
- Collapsars
- GRBGW
- Rates
- SN GW
- Implications
- Issues
- Principle Results
- Slide 46
- Slide 47
-
Bloom et al (ApJL2002)
GRB991121
see also Hjorth et al Fox et al Nature (2003)
extremely close = 800 Mpc
GRB030329SN2003DH
SN 1998bwGRB 980425
The supernova - a Type Ic - was very unusual
Large mass of 56Ni 03 - 09 solar masses (note jets acting alone do not make 56Ni) Sollerman et al ApJL 537 127 (2000) McKinzie amp Schaefer PASP 111 964 (1999)
Extreme energy and mass gt 1052 erg gt 10 Msun Iwamoto et al Nature 395 672 (1998) Woosley Eastman amp Schmidt ApJ 516 788 (1999) Mazzali et al ApJ 559 1047 (2001)
Exceptionally strong radio source Li amp Chevalier ApJ 526 716 (1999) Relativistic matter was ejected 1050 - 1051 erg Wieringa Kulkarni amp Frail AampAS 138 467 (1999) Frail et al ApJL (2001) astroph-0102282
Probability favors the GRB-SN association Pian et al ApJ 536 778 (2000)
Merging neutron star - black hole pairs
Strengths
a) Known event b) Plenty of angular momentum c) Rapid time scale d) High energy e) Well developed numerical models
Weaknesses a) Outside star forming regions
b) Beaming and energy may be inadequate for long bursts
But this model may still be good for a class of bursts calledthe ldquoshort hardrdquo bursts for which we have no counterpart informationyet (SWIFT)
Ruffert amp Janka Rosswog et al Lee et al Aloy et al
Requirements on the Central Engineand its Immediate Surroundings
(long-soft bursts)bull Provide adequate energy at high Lorentz factor
bull Collimate the emergent beam to approximately 01 radians
bull In the internal shock model provide a beam with rapidly variable Lorentz factor
bull Allow for the observed diverse GRB light curves
bull Last approximately 10 s but much longer in some cases
bull Explain diverse events like GRB 980425
bull Produce a (Type Ibc) supernova in some cases
bull Make bursts in star forming regions
GRB central engine
bull Relativity (SR amp GR)bull Magnetic Fieldsbull Rotation (progenitors)bull Nuclear Physicsbull Neutrinosbull EOSbull Turbulencebull 3Dbull Range of Lengthscales
Muller (1999)
ldquoDelayedrdquo SN Explosion
ac
Accretion vs Neutrino heating
Burrows (2001)
Pre-Supernova Density Structure
Woosley amp Weaver (1995)
Bigger stars
Higher entropy
Shallower density gradients
Fryer ApJ 522 413 (1999) Burrows (1999)
Bigger stars
1 Accrete faster amp longer
2 Larger binding energy amp smaller explosion energy
explosion
binding
Failure of delayed mechanism
Fukuda (1982)
Heger (2000)
Stellar Rotation
no mass lossMass loss
No B fields
Collapsars
Type Masssun BH Time Scale Distance Comment
I 15-40 He prompt 20 s all z neutrino-dominated disk
II 10-40 He delayed 20 s ndash 1 hr all z black hole by fall back
III gt130 He prompt ~20 s zgt10 time dilated redshifted (1+z) very energetic pair instability low Z
A rotating massive star whose core collapses to a black hole and produces an accretion disk
Type I is what we are usually talking aboutThe 40 solar mass limit comes from assuming that all stars above 100 solar masses on the main sequence are unstable (except Pop III)
IFTwo plausible conditions occur
1 Failure of neutrino powered SN explosion
a completeb partial (fallback)
2 Rotating stellar coresj gt 3 x 1016 cm2s
THEN
Rapidly accreting black hole (M~01 Ms)fed by collapsing star (tdyn ~ 446 s frac12 ~ 10 s)Disk formation
COLLAPSAR
Collapsar Simulations
bull pre-SN 15 Msun Helium starbull Newtonian Hydrodynamics (PPM)bull alpha viscositybull rotationbull photodisintegration (NSE alpha n p)bull neutrino cooling thermal + URCA optically thinbull Ideal nucleons radiation relativistic degenerate
electrons positionsbull 2D axisymmetric spherical gridbull self gravity pseudo-Newtonian (PW)bull Rin = 9 Rs Rout = 9000 Rs
MacFadyen amp Woosley (1999)
Collapsar Disk AnimationPPM hydrodynamics Paczynski-Witta potential EOS neutrino cooling nuclear reactions viscosity
Stellar collapse w rotation
Density structure No disk no wind
Note Accretion shock funnel clearing pole to equator density contrast fluctuating polar density
Initial model 15 Msun Helium (Wolf-Rayet) star evolved with mass loss
R= 8 x 108 cm
Show inner 1 in radius disk mass = 001 M_sun
Low viscosity =001
Disk Formation Movie
Accretion Shock
Disk formation
t = 75 s
PhotodisintegrationSiOC -gt free neutronsAnd protons Enhanced neutrino cooling
neutrino coolong allows
accretion
no cooling=gt
dynamically unstable
CDAF
Could emit GWs but
maybe no GRB
= 01 ltMgt = 007 Msun s = 13 x 1053 ergs
spin
mass
Use 1D neutrino cooled
ldquoslimrdquo disk models
from Popham et al (1999)
Collapsar results
bull Sustained accretion gt10sbull Sufficient energy bull Time scale set by He core collapsebull Disk-feeding time scale not disk-drainingbull Neutrino cooling allows accretionbull Neutrino annihilation energetically
possiblendash calculable in any case
Funnel geometry
channels any fireball
Density contrasts can
be huge
Ejet = f Maccc2
MHD
T = 57 ms
E = 5 x 1050 ergs
Edep = 28 x 1048 erg
Jet BirthThermal energy deposition focused by toroidal funnel structure
fmax ~ 06 - 4
Relativistic Jet Movie
Collapsar stages1 Iron core collapse disk formation
T~1010K ~108gcm-3 photodisintegration cooling pair capture disk is free nucleons (2 s)
2 Polar density declines to allow jet birthfrac12v3 Edep (2-5 s)
3 Jet tunnels out of star (5 s) Wolf-Rayet4 Jet powered for ~10 more seconds
Evacuates polar channel and reaches asymptotic speed (10 s)
T_GRB T_collapse
Jupiter
Red Supergiant
R~1013 cm
Blue Supergiant
R~1012 cm
Wolf-Rayet Star
R~1011 cm
Type Ib or Ic
Supernova
Supernovae
Ia
WD cosmology
Type II
Hydrogen
Type I
No Hydrogen
Ib Ic
exploding WR
thermonuclear old pop E galaxies
core collapse massive stars
Nickel Wind Movie
ldquoNickel Windrdquo
T gt 5 x 109 K
Fallback in weak SN explosions
Shock reaches
surface of star but parts of star are
not ejected to infinity
Fallback accretion Mms ~ 25 Msun Same star
exploded with a range of explosion energies
Significant accretion for thousands of
seconds ndash days
If fallback fuels a jet with power
fmc2
May power ldquohypernovardquo or long duration
GRBWeak
supernova shock
Shock breakout X-Ray transient
2 ldquoBriefrdquo jet tengine tjet
Engine dies before jet breakout
Mildly relativistic shock breakout
MacFadyen (1999)
What made SN1998bw+GRB980425
1 Accretion powered hypernova w Nickel wind
MacFadyen (2002)
E~ 1052 erg M(Ni)~05 M
GRB from ~3 shock breakout (Tan et al 2001 Perna amp Vietri 2002)
Collapsars
bull Can make ldquolongrdquo GRBs in H stripped (WR) stars tengine gt tescape
bull Short bursts may be compact binary mergersbull Need SN failure amp angular momentum
ndash Low metallicity binary can help
bull Star can explode -gt SN if nickel is made Predicts GRBSN association Type Ibc
bull SNGRB ratio may depend on angular momentumbull ldquoNickel windrdquo can explode star -gt hypernova
ndash H env Type II (no GRB) no H Type I + GRB
GRBGW bull Long GRBs
ndash not brighter than SN in GW
ndash very far Gpc
ndash very rare lt 1 SN
bull Short GBsndash merging ns-bh binaries
ndash maybe closer than long bursts
ndash short delay between event and GRB
ndash good for SWIFTLIGO
Rates
bull SN 1s = 100000 day
bull GRB 1day (BATSE) = 1000day
bull GRB rate = 1 of SN rate
bull maybe more collapsars than GRBs
bull =gt more rapidly rotating SN
bull SN with collapsar engine
bull look for bright Type Ic (w broad lines)
SN GW
bull SN1998bwGRB980425
bull 40 Mpc
bull maybe dominant GRB
bull rapid rotaters
bull SNAPROTSE look for 1998bw 2003dh like SN
bull many light curves -gt better t_explode
Implications
bull Probe engine directly
bull collapse duration vs GRB duration
bull collapseGRB delay (internal vs external)
bull disk properties ndash low viscosity big disks
Issues
bull too much j =gt no GRB but bright GW
bull may need low metallicity for GRB
bull prefer high redshift
bull donrsquot know nearby rate
bull but 980425 may imply rate is high
bull look for weak GRBs like 980425
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
With decreasing metallicity the bindingenergy of the core and the size of the silicon core both increase making black hole formation more likely atlow metallicity Woosley Heger amp Weaver RMP (2002)
Black hole formation may be unavoidable for low metallicity
Solar metallicity
Low metallicity
In the absence of mass lossand magnetic fields there wouldbe abundant progenitors
Unfortunately nature has both
15 solar mass helium core born rotating rigidly at f times break up
The more difficult problem is the angular momentum Thisis a problem shared by all current GRB models that invokemassive stars
- What is a Gamma-Ray Burst
- Superbowl Burst
- Slide 3
- 135 models (1993)
- Slide 5
- Slide 6
- Slide 7
- GRB991121
- GRB030329SN2003DH
- Slide 10
- Slide 11
- Slide 12
- GRB central engine
- ldquoDelayedrdquo SN Explosion
- Pre-Supernova Density Structure
- Failure of delayed mechanism
- Stellar Rotation
- Slide 18
- Slide 19
- Collapsar Simulations
- Collapsar Disk Animation
- Disk Formation Movie
- Slide 23
- Slide 24
- Slide 25
- Collapsar results
- Slide 27
- Jet Birth
- Relativistic Jet Movie
- Collapsar stages
- Slide 31
- Slide 32
- Nickel Wind Movie
- Slide 34
- Slide 35
- Slide 36
- Slide 37
- Slide 38
- Collapsars
- GRBGW
- Rates
- SN GW
- Implications
- Issues
- Principle Results
- Slide 46
- Slide 47
-
see also Hjorth et al Fox et al Nature (2003)
extremely close = 800 Mpc
GRB030329SN2003DH
SN 1998bwGRB 980425
The supernova - a Type Ic - was very unusual
Large mass of 56Ni 03 - 09 solar masses (note jets acting alone do not make 56Ni) Sollerman et al ApJL 537 127 (2000) McKinzie amp Schaefer PASP 111 964 (1999)
Extreme energy and mass gt 1052 erg gt 10 Msun Iwamoto et al Nature 395 672 (1998) Woosley Eastman amp Schmidt ApJ 516 788 (1999) Mazzali et al ApJ 559 1047 (2001)
Exceptionally strong radio source Li amp Chevalier ApJ 526 716 (1999) Relativistic matter was ejected 1050 - 1051 erg Wieringa Kulkarni amp Frail AampAS 138 467 (1999) Frail et al ApJL (2001) astroph-0102282
Probability favors the GRB-SN association Pian et al ApJ 536 778 (2000)
Merging neutron star - black hole pairs
Strengths
a) Known event b) Plenty of angular momentum c) Rapid time scale d) High energy e) Well developed numerical models
Weaknesses a) Outside star forming regions
b) Beaming and energy may be inadequate for long bursts
But this model may still be good for a class of bursts calledthe ldquoshort hardrdquo bursts for which we have no counterpart informationyet (SWIFT)
Ruffert amp Janka Rosswog et al Lee et al Aloy et al
Requirements on the Central Engineand its Immediate Surroundings
(long-soft bursts)bull Provide adequate energy at high Lorentz factor
bull Collimate the emergent beam to approximately 01 radians
bull In the internal shock model provide a beam with rapidly variable Lorentz factor
bull Allow for the observed diverse GRB light curves
bull Last approximately 10 s but much longer in some cases
bull Explain diverse events like GRB 980425
bull Produce a (Type Ibc) supernova in some cases
bull Make bursts in star forming regions
GRB central engine
bull Relativity (SR amp GR)bull Magnetic Fieldsbull Rotation (progenitors)bull Nuclear Physicsbull Neutrinosbull EOSbull Turbulencebull 3Dbull Range of Lengthscales
Muller (1999)
ldquoDelayedrdquo SN Explosion
ac
Accretion vs Neutrino heating
Burrows (2001)
Pre-Supernova Density Structure
Woosley amp Weaver (1995)
Bigger stars
Higher entropy
Shallower density gradients
Fryer ApJ 522 413 (1999) Burrows (1999)
Bigger stars
1 Accrete faster amp longer
2 Larger binding energy amp smaller explosion energy
explosion
binding
Failure of delayed mechanism
Fukuda (1982)
Heger (2000)
Stellar Rotation
no mass lossMass loss
No B fields
Collapsars
Type Masssun BH Time Scale Distance Comment
I 15-40 He prompt 20 s all z neutrino-dominated disk
II 10-40 He delayed 20 s ndash 1 hr all z black hole by fall back
III gt130 He prompt ~20 s zgt10 time dilated redshifted (1+z) very energetic pair instability low Z
A rotating massive star whose core collapses to a black hole and produces an accretion disk
Type I is what we are usually talking aboutThe 40 solar mass limit comes from assuming that all stars above 100 solar masses on the main sequence are unstable (except Pop III)
IFTwo plausible conditions occur
1 Failure of neutrino powered SN explosion
a completeb partial (fallback)
2 Rotating stellar coresj gt 3 x 1016 cm2s
THEN
Rapidly accreting black hole (M~01 Ms)fed by collapsing star (tdyn ~ 446 s frac12 ~ 10 s)Disk formation
COLLAPSAR
Collapsar Simulations
bull pre-SN 15 Msun Helium starbull Newtonian Hydrodynamics (PPM)bull alpha viscositybull rotationbull photodisintegration (NSE alpha n p)bull neutrino cooling thermal + URCA optically thinbull Ideal nucleons radiation relativistic degenerate
electrons positionsbull 2D axisymmetric spherical gridbull self gravity pseudo-Newtonian (PW)bull Rin = 9 Rs Rout = 9000 Rs
MacFadyen amp Woosley (1999)
Collapsar Disk AnimationPPM hydrodynamics Paczynski-Witta potential EOS neutrino cooling nuclear reactions viscosity
Stellar collapse w rotation
Density structure No disk no wind
Note Accretion shock funnel clearing pole to equator density contrast fluctuating polar density
Initial model 15 Msun Helium (Wolf-Rayet) star evolved with mass loss
R= 8 x 108 cm
Show inner 1 in radius disk mass = 001 M_sun
Low viscosity =001
Disk Formation Movie
Accretion Shock
Disk formation
t = 75 s
PhotodisintegrationSiOC -gt free neutronsAnd protons Enhanced neutrino cooling
neutrino coolong allows
accretion
no cooling=gt
dynamically unstable
CDAF
Could emit GWs but
maybe no GRB
= 01 ltMgt = 007 Msun s = 13 x 1053 ergs
spin
mass
Use 1D neutrino cooled
ldquoslimrdquo disk models
from Popham et al (1999)
Collapsar results
bull Sustained accretion gt10sbull Sufficient energy bull Time scale set by He core collapsebull Disk-feeding time scale not disk-drainingbull Neutrino cooling allows accretionbull Neutrino annihilation energetically
possiblendash calculable in any case
Funnel geometry
channels any fireball
Density contrasts can
be huge
Ejet = f Maccc2
MHD
T = 57 ms
E = 5 x 1050 ergs
Edep = 28 x 1048 erg
Jet BirthThermal energy deposition focused by toroidal funnel structure
fmax ~ 06 - 4
Relativistic Jet Movie
Collapsar stages1 Iron core collapse disk formation
T~1010K ~108gcm-3 photodisintegration cooling pair capture disk is free nucleons (2 s)
2 Polar density declines to allow jet birthfrac12v3 Edep (2-5 s)
3 Jet tunnels out of star (5 s) Wolf-Rayet4 Jet powered for ~10 more seconds
Evacuates polar channel and reaches asymptotic speed (10 s)
T_GRB T_collapse
Jupiter
Red Supergiant
R~1013 cm
Blue Supergiant
R~1012 cm
Wolf-Rayet Star
R~1011 cm
Type Ib or Ic
Supernova
Supernovae
Ia
WD cosmology
Type II
Hydrogen
Type I
No Hydrogen
Ib Ic
exploding WR
thermonuclear old pop E galaxies
core collapse massive stars
Nickel Wind Movie
ldquoNickel Windrdquo
T gt 5 x 109 K
Fallback in weak SN explosions
Shock reaches
surface of star but parts of star are
not ejected to infinity
Fallback accretion Mms ~ 25 Msun Same star
exploded with a range of explosion energies
Significant accretion for thousands of
seconds ndash days
If fallback fuels a jet with power
fmc2
May power ldquohypernovardquo or long duration
GRBWeak
supernova shock
Shock breakout X-Ray transient
2 ldquoBriefrdquo jet tengine tjet
Engine dies before jet breakout
Mildly relativistic shock breakout
MacFadyen (1999)
What made SN1998bw+GRB980425
1 Accretion powered hypernova w Nickel wind
MacFadyen (2002)
E~ 1052 erg M(Ni)~05 M
GRB from ~3 shock breakout (Tan et al 2001 Perna amp Vietri 2002)
Collapsars
bull Can make ldquolongrdquo GRBs in H stripped (WR) stars tengine gt tescape
bull Short bursts may be compact binary mergersbull Need SN failure amp angular momentum
ndash Low metallicity binary can help
bull Star can explode -gt SN if nickel is made Predicts GRBSN association Type Ibc
bull SNGRB ratio may depend on angular momentumbull ldquoNickel windrdquo can explode star -gt hypernova
ndash H env Type II (no GRB) no H Type I + GRB
GRBGW bull Long GRBs
ndash not brighter than SN in GW
ndash very far Gpc
ndash very rare lt 1 SN
bull Short GBsndash merging ns-bh binaries
ndash maybe closer than long bursts
ndash short delay between event and GRB
ndash good for SWIFTLIGO
Rates
bull SN 1s = 100000 day
bull GRB 1day (BATSE) = 1000day
bull GRB rate = 1 of SN rate
bull maybe more collapsars than GRBs
bull =gt more rapidly rotating SN
bull SN with collapsar engine
bull look for bright Type Ic (w broad lines)
SN GW
bull SN1998bwGRB980425
bull 40 Mpc
bull maybe dominant GRB
bull rapid rotaters
bull SNAPROTSE look for 1998bw 2003dh like SN
bull many light curves -gt better t_explode
Implications
bull Probe engine directly
bull collapse duration vs GRB duration
bull collapseGRB delay (internal vs external)
bull disk properties ndash low viscosity big disks
Issues
bull too much j =gt no GRB but bright GW
bull may need low metallicity for GRB
bull prefer high redshift
bull donrsquot know nearby rate
bull but 980425 may imply rate is high
bull look for weak GRBs like 980425
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
With decreasing metallicity the bindingenergy of the core and the size of the silicon core both increase making black hole formation more likely atlow metallicity Woosley Heger amp Weaver RMP (2002)
Black hole formation may be unavoidable for low metallicity
Solar metallicity
Low metallicity
In the absence of mass lossand magnetic fields there wouldbe abundant progenitors
Unfortunately nature has both
15 solar mass helium core born rotating rigidly at f times break up
The more difficult problem is the angular momentum Thisis a problem shared by all current GRB models that invokemassive stars
- What is a Gamma-Ray Burst
- Superbowl Burst
- Slide 3
- 135 models (1993)
- Slide 5
- Slide 6
- Slide 7
- GRB991121
- GRB030329SN2003DH
- Slide 10
- Slide 11
- Slide 12
- GRB central engine
- ldquoDelayedrdquo SN Explosion
- Pre-Supernova Density Structure
- Failure of delayed mechanism
- Stellar Rotation
- Slide 18
- Slide 19
- Collapsar Simulations
- Collapsar Disk Animation
- Disk Formation Movie
- Slide 23
- Slide 24
- Slide 25
- Collapsar results
- Slide 27
- Jet Birth
- Relativistic Jet Movie
- Collapsar stages
- Slide 31
- Slide 32
- Nickel Wind Movie
- Slide 34
- Slide 35
- Slide 36
- Slide 37
- Slide 38
- Collapsars
- GRBGW
- Rates
- SN GW
- Implications
- Issues
- Principle Results
- Slide 46
- Slide 47
-
SN 1998bwGRB 980425
The supernova - a Type Ic - was very unusual
Large mass of 56Ni 03 - 09 solar masses (note jets acting alone do not make 56Ni) Sollerman et al ApJL 537 127 (2000) McKinzie amp Schaefer PASP 111 964 (1999)
Extreme energy and mass gt 1052 erg gt 10 Msun Iwamoto et al Nature 395 672 (1998) Woosley Eastman amp Schmidt ApJ 516 788 (1999) Mazzali et al ApJ 559 1047 (2001)
Exceptionally strong radio source Li amp Chevalier ApJ 526 716 (1999) Relativistic matter was ejected 1050 - 1051 erg Wieringa Kulkarni amp Frail AampAS 138 467 (1999) Frail et al ApJL (2001) astroph-0102282
Probability favors the GRB-SN association Pian et al ApJ 536 778 (2000)
Merging neutron star - black hole pairs
Strengths
a) Known event b) Plenty of angular momentum c) Rapid time scale d) High energy e) Well developed numerical models
Weaknesses a) Outside star forming regions
b) Beaming and energy may be inadequate for long bursts
But this model may still be good for a class of bursts calledthe ldquoshort hardrdquo bursts for which we have no counterpart informationyet (SWIFT)
Ruffert amp Janka Rosswog et al Lee et al Aloy et al
Requirements on the Central Engineand its Immediate Surroundings
(long-soft bursts)bull Provide adequate energy at high Lorentz factor
bull Collimate the emergent beam to approximately 01 radians
bull In the internal shock model provide a beam with rapidly variable Lorentz factor
bull Allow for the observed diverse GRB light curves
bull Last approximately 10 s but much longer in some cases
bull Explain diverse events like GRB 980425
bull Produce a (Type Ibc) supernova in some cases
bull Make bursts in star forming regions
GRB central engine
bull Relativity (SR amp GR)bull Magnetic Fieldsbull Rotation (progenitors)bull Nuclear Physicsbull Neutrinosbull EOSbull Turbulencebull 3Dbull Range of Lengthscales
Muller (1999)
ldquoDelayedrdquo SN Explosion
ac
Accretion vs Neutrino heating
Burrows (2001)
Pre-Supernova Density Structure
Woosley amp Weaver (1995)
Bigger stars
Higher entropy
Shallower density gradients
Fryer ApJ 522 413 (1999) Burrows (1999)
Bigger stars
1 Accrete faster amp longer
2 Larger binding energy amp smaller explosion energy
explosion
binding
Failure of delayed mechanism
Fukuda (1982)
Heger (2000)
Stellar Rotation
no mass lossMass loss
No B fields
Collapsars
Type Masssun BH Time Scale Distance Comment
I 15-40 He prompt 20 s all z neutrino-dominated disk
II 10-40 He delayed 20 s ndash 1 hr all z black hole by fall back
III gt130 He prompt ~20 s zgt10 time dilated redshifted (1+z) very energetic pair instability low Z
A rotating massive star whose core collapses to a black hole and produces an accretion disk
Type I is what we are usually talking aboutThe 40 solar mass limit comes from assuming that all stars above 100 solar masses on the main sequence are unstable (except Pop III)
IFTwo plausible conditions occur
1 Failure of neutrino powered SN explosion
a completeb partial (fallback)
2 Rotating stellar coresj gt 3 x 1016 cm2s
THEN
Rapidly accreting black hole (M~01 Ms)fed by collapsing star (tdyn ~ 446 s frac12 ~ 10 s)Disk formation
COLLAPSAR
Collapsar Simulations
bull pre-SN 15 Msun Helium starbull Newtonian Hydrodynamics (PPM)bull alpha viscositybull rotationbull photodisintegration (NSE alpha n p)bull neutrino cooling thermal + URCA optically thinbull Ideal nucleons radiation relativistic degenerate
electrons positionsbull 2D axisymmetric spherical gridbull self gravity pseudo-Newtonian (PW)bull Rin = 9 Rs Rout = 9000 Rs
MacFadyen amp Woosley (1999)
Collapsar Disk AnimationPPM hydrodynamics Paczynski-Witta potential EOS neutrino cooling nuclear reactions viscosity
Stellar collapse w rotation
Density structure No disk no wind
Note Accretion shock funnel clearing pole to equator density contrast fluctuating polar density
Initial model 15 Msun Helium (Wolf-Rayet) star evolved with mass loss
R= 8 x 108 cm
Show inner 1 in radius disk mass = 001 M_sun
Low viscosity =001
Disk Formation Movie
Accretion Shock
Disk formation
t = 75 s
PhotodisintegrationSiOC -gt free neutronsAnd protons Enhanced neutrino cooling
neutrino coolong allows
accretion
no cooling=gt
dynamically unstable
CDAF
Could emit GWs but
maybe no GRB
= 01 ltMgt = 007 Msun s = 13 x 1053 ergs
spin
mass
Use 1D neutrino cooled
ldquoslimrdquo disk models
from Popham et al (1999)
Collapsar results
bull Sustained accretion gt10sbull Sufficient energy bull Time scale set by He core collapsebull Disk-feeding time scale not disk-drainingbull Neutrino cooling allows accretionbull Neutrino annihilation energetically
possiblendash calculable in any case
Funnel geometry
channels any fireball
Density contrasts can
be huge
Ejet = f Maccc2
MHD
T = 57 ms
E = 5 x 1050 ergs
Edep = 28 x 1048 erg
Jet BirthThermal energy deposition focused by toroidal funnel structure
fmax ~ 06 - 4
Relativistic Jet Movie
Collapsar stages1 Iron core collapse disk formation
T~1010K ~108gcm-3 photodisintegration cooling pair capture disk is free nucleons (2 s)
2 Polar density declines to allow jet birthfrac12v3 Edep (2-5 s)
3 Jet tunnels out of star (5 s) Wolf-Rayet4 Jet powered for ~10 more seconds
Evacuates polar channel and reaches asymptotic speed (10 s)
T_GRB T_collapse
Jupiter
Red Supergiant
R~1013 cm
Blue Supergiant
R~1012 cm
Wolf-Rayet Star
R~1011 cm
Type Ib or Ic
Supernova
Supernovae
Ia
WD cosmology
Type II
Hydrogen
Type I
No Hydrogen
Ib Ic
exploding WR
thermonuclear old pop E galaxies
core collapse massive stars
Nickel Wind Movie
ldquoNickel Windrdquo
T gt 5 x 109 K
Fallback in weak SN explosions
Shock reaches
surface of star but parts of star are
not ejected to infinity
Fallback accretion Mms ~ 25 Msun Same star
exploded with a range of explosion energies
Significant accretion for thousands of
seconds ndash days
If fallback fuels a jet with power
fmc2
May power ldquohypernovardquo or long duration
GRBWeak
supernova shock
Shock breakout X-Ray transient
2 ldquoBriefrdquo jet tengine tjet
Engine dies before jet breakout
Mildly relativistic shock breakout
MacFadyen (1999)
What made SN1998bw+GRB980425
1 Accretion powered hypernova w Nickel wind
MacFadyen (2002)
E~ 1052 erg M(Ni)~05 M
GRB from ~3 shock breakout (Tan et al 2001 Perna amp Vietri 2002)
Collapsars
bull Can make ldquolongrdquo GRBs in H stripped (WR) stars tengine gt tescape
bull Short bursts may be compact binary mergersbull Need SN failure amp angular momentum
ndash Low metallicity binary can help
bull Star can explode -gt SN if nickel is made Predicts GRBSN association Type Ibc
bull SNGRB ratio may depend on angular momentumbull ldquoNickel windrdquo can explode star -gt hypernova
ndash H env Type II (no GRB) no H Type I + GRB
GRBGW bull Long GRBs
ndash not brighter than SN in GW
ndash very far Gpc
ndash very rare lt 1 SN
bull Short GBsndash merging ns-bh binaries
ndash maybe closer than long bursts
ndash short delay between event and GRB
ndash good for SWIFTLIGO
Rates
bull SN 1s = 100000 day
bull GRB 1day (BATSE) = 1000day
bull GRB rate = 1 of SN rate
bull maybe more collapsars than GRBs
bull =gt more rapidly rotating SN
bull SN with collapsar engine
bull look for bright Type Ic (w broad lines)
SN GW
bull SN1998bwGRB980425
bull 40 Mpc
bull maybe dominant GRB
bull rapid rotaters
bull SNAPROTSE look for 1998bw 2003dh like SN
bull many light curves -gt better t_explode
Implications
bull Probe engine directly
bull collapse duration vs GRB duration
bull collapseGRB delay (internal vs external)
bull disk properties ndash low viscosity big disks
Issues
bull too much j =gt no GRB but bright GW
bull may need low metallicity for GRB
bull prefer high redshift
bull donrsquot know nearby rate
bull but 980425 may imply rate is high
bull look for weak GRBs like 980425
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
With decreasing metallicity the bindingenergy of the core and the size of the silicon core both increase making black hole formation more likely atlow metallicity Woosley Heger amp Weaver RMP (2002)
Black hole formation may be unavoidable for low metallicity
Solar metallicity
Low metallicity
In the absence of mass lossand magnetic fields there wouldbe abundant progenitors
Unfortunately nature has both
15 solar mass helium core born rotating rigidly at f times break up
The more difficult problem is the angular momentum Thisis a problem shared by all current GRB models that invokemassive stars
- What is a Gamma-Ray Burst
- Superbowl Burst
- Slide 3
- 135 models (1993)
- Slide 5
- Slide 6
- Slide 7
- GRB991121
- GRB030329SN2003DH
- Slide 10
- Slide 11
- Slide 12
- GRB central engine
- ldquoDelayedrdquo SN Explosion
- Pre-Supernova Density Structure
- Failure of delayed mechanism
- Stellar Rotation
- Slide 18
- Slide 19
- Collapsar Simulations
- Collapsar Disk Animation
- Disk Formation Movie
- Slide 23
- Slide 24
- Slide 25
- Collapsar results
- Slide 27
- Jet Birth
- Relativistic Jet Movie
- Collapsar stages
- Slide 31
- Slide 32
- Nickel Wind Movie
- Slide 34
- Slide 35
- Slide 36
- Slide 37
- Slide 38
- Collapsars
- GRBGW
- Rates
- SN GW
- Implications
- Issues
- Principle Results
- Slide 46
- Slide 47
-
Merging neutron star - black hole pairs
Strengths
a) Known event b) Plenty of angular momentum c) Rapid time scale d) High energy e) Well developed numerical models
Weaknesses a) Outside star forming regions
b) Beaming and energy may be inadequate for long bursts
But this model may still be good for a class of bursts calledthe ldquoshort hardrdquo bursts for which we have no counterpart informationyet (SWIFT)
Ruffert amp Janka Rosswog et al Lee et al Aloy et al
Requirements on the Central Engineand its Immediate Surroundings
(long-soft bursts)bull Provide adequate energy at high Lorentz factor
bull Collimate the emergent beam to approximately 01 radians
bull In the internal shock model provide a beam with rapidly variable Lorentz factor
bull Allow for the observed diverse GRB light curves
bull Last approximately 10 s but much longer in some cases
bull Explain diverse events like GRB 980425
bull Produce a (Type Ibc) supernova in some cases
bull Make bursts in star forming regions
GRB central engine
bull Relativity (SR amp GR)bull Magnetic Fieldsbull Rotation (progenitors)bull Nuclear Physicsbull Neutrinosbull EOSbull Turbulencebull 3Dbull Range of Lengthscales
Muller (1999)
ldquoDelayedrdquo SN Explosion
ac
Accretion vs Neutrino heating
Burrows (2001)
Pre-Supernova Density Structure
Woosley amp Weaver (1995)
Bigger stars
Higher entropy
Shallower density gradients
Fryer ApJ 522 413 (1999) Burrows (1999)
Bigger stars
1 Accrete faster amp longer
2 Larger binding energy amp smaller explosion energy
explosion
binding
Failure of delayed mechanism
Fukuda (1982)
Heger (2000)
Stellar Rotation
no mass lossMass loss
No B fields
Collapsars
Type Masssun BH Time Scale Distance Comment
I 15-40 He prompt 20 s all z neutrino-dominated disk
II 10-40 He delayed 20 s ndash 1 hr all z black hole by fall back
III gt130 He prompt ~20 s zgt10 time dilated redshifted (1+z) very energetic pair instability low Z
A rotating massive star whose core collapses to a black hole and produces an accretion disk
Type I is what we are usually talking aboutThe 40 solar mass limit comes from assuming that all stars above 100 solar masses on the main sequence are unstable (except Pop III)
IFTwo plausible conditions occur
1 Failure of neutrino powered SN explosion
a completeb partial (fallback)
2 Rotating stellar coresj gt 3 x 1016 cm2s
THEN
Rapidly accreting black hole (M~01 Ms)fed by collapsing star (tdyn ~ 446 s frac12 ~ 10 s)Disk formation
COLLAPSAR
Collapsar Simulations
bull pre-SN 15 Msun Helium starbull Newtonian Hydrodynamics (PPM)bull alpha viscositybull rotationbull photodisintegration (NSE alpha n p)bull neutrino cooling thermal + URCA optically thinbull Ideal nucleons radiation relativistic degenerate
electrons positionsbull 2D axisymmetric spherical gridbull self gravity pseudo-Newtonian (PW)bull Rin = 9 Rs Rout = 9000 Rs
MacFadyen amp Woosley (1999)
Collapsar Disk AnimationPPM hydrodynamics Paczynski-Witta potential EOS neutrino cooling nuclear reactions viscosity
Stellar collapse w rotation
Density structure No disk no wind
Note Accretion shock funnel clearing pole to equator density contrast fluctuating polar density
Initial model 15 Msun Helium (Wolf-Rayet) star evolved with mass loss
R= 8 x 108 cm
Show inner 1 in radius disk mass = 001 M_sun
Low viscosity =001
Disk Formation Movie
Accretion Shock
Disk formation
t = 75 s
PhotodisintegrationSiOC -gt free neutronsAnd protons Enhanced neutrino cooling
neutrino coolong allows
accretion
no cooling=gt
dynamically unstable
CDAF
Could emit GWs but
maybe no GRB
= 01 ltMgt = 007 Msun s = 13 x 1053 ergs
spin
mass
Use 1D neutrino cooled
ldquoslimrdquo disk models
from Popham et al (1999)
Collapsar results
bull Sustained accretion gt10sbull Sufficient energy bull Time scale set by He core collapsebull Disk-feeding time scale not disk-drainingbull Neutrino cooling allows accretionbull Neutrino annihilation energetically
possiblendash calculable in any case
Funnel geometry
channels any fireball
Density contrasts can
be huge
Ejet = f Maccc2
MHD
T = 57 ms
E = 5 x 1050 ergs
Edep = 28 x 1048 erg
Jet BirthThermal energy deposition focused by toroidal funnel structure
fmax ~ 06 - 4
Relativistic Jet Movie
Collapsar stages1 Iron core collapse disk formation
T~1010K ~108gcm-3 photodisintegration cooling pair capture disk is free nucleons (2 s)
2 Polar density declines to allow jet birthfrac12v3 Edep (2-5 s)
3 Jet tunnels out of star (5 s) Wolf-Rayet4 Jet powered for ~10 more seconds
Evacuates polar channel and reaches asymptotic speed (10 s)
T_GRB T_collapse
Jupiter
Red Supergiant
R~1013 cm
Blue Supergiant
R~1012 cm
Wolf-Rayet Star
R~1011 cm
Type Ib or Ic
Supernova
Supernovae
Ia
WD cosmology
Type II
Hydrogen
Type I
No Hydrogen
Ib Ic
exploding WR
thermonuclear old pop E galaxies
core collapse massive stars
Nickel Wind Movie
ldquoNickel Windrdquo
T gt 5 x 109 K
Fallback in weak SN explosions
Shock reaches
surface of star but parts of star are
not ejected to infinity
Fallback accretion Mms ~ 25 Msun Same star
exploded with a range of explosion energies
Significant accretion for thousands of
seconds ndash days
If fallback fuels a jet with power
fmc2
May power ldquohypernovardquo or long duration
GRBWeak
supernova shock
Shock breakout X-Ray transient
2 ldquoBriefrdquo jet tengine tjet
Engine dies before jet breakout
Mildly relativistic shock breakout
MacFadyen (1999)
What made SN1998bw+GRB980425
1 Accretion powered hypernova w Nickel wind
MacFadyen (2002)
E~ 1052 erg M(Ni)~05 M
GRB from ~3 shock breakout (Tan et al 2001 Perna amp Vietri 2002)
Collapsars
bull Can make ldquolongrdquo GRBs in H stripped (WR) stars tengine gt tescape
bull Short bursts may be compact binary mergersbull Need SN failure amp angular momentum
ndash Low metallicity binary can help
bull Star can explode -gt SN if nickel is made Predicts GRBSN association Type Ibc
bull SNGRB ratio may depend on angular momentumbull ldquoNickel windrdquo can explode star -gt hypernova
ndash H env Type II (no GRB) no H Type I + GRB
GRBGW bull Long GRBs
ndash not brighter than SN in GW
ndash very far Gpc
ndash very rare lt 1 SN
bull Short GBsndash merging ns-bh binaries
ndash maybe closer than long bursts
ndash short delay between event and GRB
ndash good for SWIFTLIGO
Rates
bull SN 1s = 100000 day
bull GRB 1day (BATSE) = 1000day
bull GRB rate = 1 of SN rate
bull maybe more collapsars than GRBs
bull =gt more rapidly rotating SN
bull SN with collapsar engine
bull look for bright Type Ic (w broad lines)
SN GW
bull SN1998bwGRB980425
bull 40 Mpc
bull maybe dominant GRB
bull rapid rotaters
bull SNAPROTSE look for 1998bw 2003dh like SN
bull many light curves -gt better t_explode
Implications
bull Probe engine directly
bull collapse duration vs GRB duration
bull collapseGRB delay (internal vs external)
bull disk properties ndash low viscosity big disks
Issues
bull too much j =gt no GRB but bright GW
bull may need low metallicity for GRB
bull prefer high redshift
bull donrsquot know nearby rate
bull but 980425 may imply rate is high
bull look for weak GRBs like 980425
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
With decreasing metallicity the bindingenergy of the core and the size of the silicon core both increase making black hole formation more likely atlow metallicity Woosley Heger amp Weaver RMP (2002)
Black hole formation may be unavoidable for low metallicity
Solar metallicity
Low metallicity
In the absence of mass lossand magnetic fields there wouldbe abundant progenitors
Unfortunately nature has both
15 solar mass helium core born rotating rigidly at f times break up
The more difficult problem is the angular momentum Thisis a problem shared by all current GRB models that invokemassive stars
- What is a Gamma-Ray Burst
- Superbowl Burst
- Slide 3
- 135 models (1993)
- Slide 5
- Slide 6
- Slide 7
- GRB991121
- GRB030329SN2003DH
- Slide 10
- Slide 11
- Slide 12
- GRB central engine
- ldquoDelayedrdquo SN Explosion
- Pre-Supernova Density Structure
- Failure of delayed mechanism
- Stellar Rotation
- Slide 18
- Slide 19
- Collapsar Simulations
- Collapsar Disk Animation
- Disk Formation Movie
- Slide 23
- Slide 24
- Slide 25
- Collapsar results
- Slide 27
- Jet Birth
- Relativistic Jet Movie
- Collapsar stages
- Slide 31
- Slide 32
- Nickel Wind Movie
- Slide 34
- Slide 35
- Slide 36
- Slide 37
- Slide 38
- Collapsars
- GRBGW
- Rates
- SN GW
- Implications
- Issues
- Principle Results
- Slide 46
- Slide 47
-
Requirements on the Central Engineand its Immediate Surroundings
(long-soft bursts)bull Provide adequate energy at high Lorentz factor
bull Collimate the emergent beam to approximately 01 radians
bull In the internal shock model provide a beam with rapidly variable Lorentz factor
bull Allow for the observed diverse GRB light curves
bull Last approximately 10 s but much longer in some cases
bull Explain diverse events like GRB 980425
bull Produce a (Type Ibc) supernova in some cases
bull Make bursts in star forming regions
GRB central engine
bull Relativity (SR amp GR)bull Magnetic Fieldsbull Rotation (progenitors)bull Nuclear Physicsbull Neutrinosbull EOSbull Turbulencebull 3Dbull Range of Lengthscales
Muller (1999)
ldquoDelayedrdquo SN Explosion
ac
Accretion vs Neutrino heating
Burrows (2001)
Pre-Supernova Density Structure
Woosley amp Weaver (1995)
Bigger stars
Higher entropy
Shallower density gradients
Fryer ApJ 522 413 (1999) Burrows (1999)
Bigger stars
1 Accrete faster amp longer
2 Larger binding energy amp smaller explosion energy
explosion
binding
Failure of delayed mechanism
Fukuda (1982)
Heger (2000)
Stellar Rotation
no mass lossMass loss
No B fields
Collapsars
Type Masssun BH Time Scale Distance Comment
I 15-40 He prompt 20 s all z neutrino-dominated disk
II 10-40 He delayed 20 s ndash 1 hr all z black hole by fall back
III gt130 He prompt ~20 s zgt10 time dilated redshifted (1+z) very energetic pair instability low Z
A rotating massive star whose core collapses to a black hole and produces an accretion disk
Type I is what we are usually talking aboutThe 40 solar mass limit comes from assuming that all stars above 100 solar masses on the main sequence are unstable (except Pop III)
IFTwo plausible conditions occur
1 Failure of neutrino powered SN explosion
a completeb partial (fallback)
2 Rotating stellar coresj gt 3 x 1016 cm2s
THEN
Rapidly accreting black hole (M~01 Ms)fed by collapsing star (tdyn ~ 446 s frac12 ~ 10 s)Disk formation
COLLAPSAR
Collapsar Simulations
bull pre-SN 15 Msun Helium starbull Newtonian Hydrodynamics (PPM)bull alpha viscositybull rotationbull photodisintegration (NSE alpha n p)bull neutrino cooling thermal + URCA optically thinbull Ideal nucleons radiation relativistic degenerate
electrons positionsbull 2D axisymmetric spherical gridbull self gravity pseudo-Newtonian (PW)bull Rin = 9 Rs Rout = 9000 Rs
MacFadyen amp Woosley (1999)
Collapsar Disk AnimationPPM hydrodynamics Paczynski-Witta potential EOS neutrino cooling nuclear reactions viscosity
Stellar collapse w rotation
Density structure No disk no wind
Note Accretion shock funnel clearing pole to equator density contrast fluctuating polar density
Initial model 15 Msun Helium (Wolf-Rayet) star evolved with mass loss
R= 8 x 108 cm
Show inner 1 in radius disk mass = 001 M_sun
Low viscosity =001
Disk Formation Movie
Accretion Shock
Disk formation
t = 75 s
PhotodisintegrationSiOC -gt free neutronsAnd protons Enhanced neutrino cooling
neutrino coolong allows
accretion
no cooling=gt
dynamically unstable
CDAF
Could emit GWs but
maybe no GRB
= 01 ltMgt = 007 Msun s = 13 x 1053 ergs
spin
mass
Use 1D neutrino cooled
ldquoslimrdquo disk models
from Popham et al (1999)
Collapsar results
bull Sustained accretion gt10sbull Sufficient energy bull Time scale set by He core collapsebull Disk-feeding time scale not disk-drainingbull Neutrino cooling allows accretionbull Neutrino annihilation energetically
possiblendash calculable in any case
Funnel geometry
channels any fireball
Density contrasts can
be huge
Ejet = f Maccc2
MHD
T = 57 ms
E = 5 x 1050 ergs
Edep = 28 x 1048 erg
Jet BirthThermal energy deposition focused by toroidal funnel structure
fmax ~ 06 - 4
Relativistic Jet Movie
Collapsar stages1 Iron core collapse disk formation
T~1010K ~108gcm-3 photodisintegration cooling pair capture disk is free nucleons (2 s)
2 Polar density declines to allow jet birthfrac12v3 Edep (2-5 s)
3 Jet tunnels out of star (5 s) Wolf-Rayet4 Jet powered for ~10 more seconds
Evacuates polar channel and reaches asymptotic speed (10 s)
T_GRB T_collapse
Jupiter
Red Supergiant
R~1013 cm
Blue Supergiant
R~1012 cm
Wolf-Rayet Star
R~1011 cm
Type Ib or Ic
Supernova
Supernovae
Ia
WD cosmology
Type II
Hydrogen
Type I
No Hydrogen
Ib Ic
exploding WR
thermonuclear old pop E galaxies
core collapse massive stars
Nickel Wind Movie
ldquoNickel Windrdquo
T gt 5 x 109 K
Fallback in weak SN explosions
Shock reaches
surface of star but parts of star are
not ejected to infinity
Fallback accretion Mms ~ 25 Msun Same star
exploded with a range of explosion energies
Significant accretion for thousands of
seconds ndash days
If fallback fuels a jet with power
fmc2
May power ldquohypernovardquo or long duration
GRBWeak
supernova shock
Shock breakout X-Ray transient
2 ldquoBriefrdquo jet tengine tjet
Engine dies before jet breakout
Mildly relativistic shock breakout
MacFadyen (1999)
What made SN1998bw+GRB980425
1 Accretion powered hypernova w Nickel wind
MacFadyen (2002)
E~ 1052 erg M(Ni)~05 M
GRB from ~3 shock breakout (Tan et al 2001 Perna amp Vietri 2002)
Collapsars
bull Can make ldquolongrdquo GRBs in H stripped (WR) stars tengine gt tescape
bull Short bursts may be compact binary mergersbull Need SN failure amp angular momentum
ndash Low metallicity binary can help
bull Star can explode -gt SN if nickel is made Predicts GRBSN association Type Ibc
bull SNGRB ratio may depend on angular momentumbull ldquoNickel windrdquo can explode star -gt hypernova
ndash H env Type II (no GRB) no H Type I + GRB
GRBGW bull Long GRBs
ndash not brighter than SN in GW
ndash very far Gpc
ndash very rare lt 1 SN
bull Short GBsndash merging ns-bh binaries
ndash maybe closer than long bursts
ndash short delay between event and GRB
ndash good for SWIFTLIGO
Rates
bull SN 1s = 100000 day
bull GRB 1day (BATSE) = 1000day
bull GRB rate = 1 of SN rate
bull maybe more collapsars than GRBs
bull =gt more rapidly rotating SN
bull SN with collapsar engine
bull look for bright Type Ic (w broad lines)
SN GW
bull SN1998bwGRB980425
bull 40 Mpc
bull maybe dominant GRB
bull rapid rotaters
bull SNAPROTSE look for 1998bw 2003dh like SN
bull many light curves -gt better t_explode
Implications
bull Probe engine directly
bull collapse duration vs GRB duration
bull collapseGRB delay (internal vs external)
bull disk properties ndash low viscosity big disks
Issues
bull too much j =gt no GRB but bright GW
bull may need low metallicity for GRB
bull prefer high redshift
bull donrsquot know nearby rate
bull but 980425 may imply rate is high
bull look for weak GRBs like 980425
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
With decreasing metallicity the bindingenergy of the core and the size of the silicon core both increase making black hole formation more likely atlow metallicity Woosley Heger amp Weaver RMP (2002)
Black hole formation may be unavoidable for low metallicity
Solar metallicity
Low metallicity
In the absence of mass lossand magnetic fields there wouldbe abundant progenitors
Unfortunately nature has both
15 solar mass helium core born rotating rigidly at f times break up
The more difficult problem is the angular momentum Thisis a problem shared by all current GRB models that invokemassive stars
- What is a Gamma-Ray Burst
- Superbowl Burst
- Slide 3
- 135 models (1993)
- Slide 5
- Slide 6
- Slide 7
- GRB991121
- GRB030329SN2003DH
- Slide 10
- Slide 11
- Slide 12
- GRB central engine
- ldquoDelayedrdquo SN Explosion
- Pre-Supernova Density Structure
- Failure of delayed mechanism
- Stellar Rotation
- Slide 18
- Slide 19
- Collapsar Simulations
- Collapsar Disk Animation
- Disk Formation Movie
- Slide 23
- Slide 24
- Slide 25
- Collapsar results
- Slide 27
- Jet Birth
- Relativistic Jet Movie
- Collapsar stages
- Slide 31
- Slide 32
- Nickel Wind Movie
- Slide 34
- Slide 35
- Slide 36
- Slide 37
- Slide 38
- Collapsars
- GRBGW
- Rates
- SN GW
- Implications
- Issues
- Principle Results
- Slide 46
- Slide 47
-
GRB central engine
bull Relativity (SR amp GR)bull Magnetic Fieldsbull Rotation (progenitors)bull Nuclear Physicsbull Neutrinosbull EOSbull Turbulencebull 3Dbull Range of Lengthscales
Muller (1999)
ldquoDelayedrdquo SN Explosion
ac
Accretion vs Neutrino heating
Burrows (2001)
Pre-Supernova Density Structure
Woosley amp Weaver (1995)
Bigger stars
Higher entropy
Shallower density gradients
Fryer ApJ 522 413 (1999) Burrows (1999)
Bigger stars
1 Accrete faster amp longer
2 Larger binding energy amp smaller explosion energy
explosion
binding
Failure of delayed mechanism
Fukuda (1982)
Heger (2000)
Stellar Rotation
no mass lossMass loss
No B fields
Collapsars
Type Masssun BH Time Scale Distance Comment
I 15-40 He prompt 20 s all z neutrino-dominated disk
II 10-40 He delayed 20 s ndash 1 hr all z black hole by fall back
III gt130 He prompt ~20 s zgt10 time dilated redshifted (1+z) very energetic pair instability low Z
A rotating massive star whose core collapses to a black hole and produces an accretion disk
Type I is what we are usually talking aboutThe 40 solar mass limit comes from assuming that all stars above 100 solar masses on the main sequence are unstable (except Pop III)
IFTwo plausible conditions occur
1 Failure of neutrino powered SN explosion
a completeb partial (fallback)
2 Rotating stellar coresj gt 3 x 1016 cm2s
THEN
Rapidly accreting black hole (M~01 Ms)fed by collapsing star (tdyn ~ 446 s frac12 ~ 10 s)Disk formation
COLLAPSAR
Collapsar Simulations
bull pre-SN 15 Msun Helium starbull Newtonian Hydrodynamics (PPM)bull alpha viscositybull rotationbull photodisintegration (NSE alpha n p)bull neutrino cooling thermal + URCA optically thinbull Ideal nucleons radiation relativistic degenerate
electrons positionsbull 2D axisymmetric spherical gridbull self gravity pseudo-Newtonian (PW)bull Rin = 9 Rs Rout = 9000 Rs
MacFadyen amp Woosley (1999)
Collapsar Disk AnimationPPM hydrodynamics Paczynski-Witta potential EOS neutrino cooling nuclear reactions viscosity
Stellar collapse w rotation
Density structure No disk no wind
Note Accretion shock funnel clearing pole to equator density contrast fluctuating polar density
Initial model 15 Msun Helium (Wolf-Rayet) star evolved with mass loss
R= 8 x 108 cm
Show inner 1 in radius disk mass = 001 M_sun
Low viscosity =001
Disk Formation Movie
Accretion Shock
Disk formation
t = 75 s
PhotodisintegrationSiOC -gt free neutronsAnd protons Enhanced neutrino cooling
neutrino coolong allows
accretion
no cooling=gt
dynamically unstable
CDAF
Could emit GWs but
maybe no GRB
= 01 ltMgt = 007 Msun s = 13 x 1053 ergs
spin
mass
Use 1D neutrino cooled
ldquoslimrdquo disk models
from Popham et al (1999)
Collapsar results
bull Sustained accretion gt10sbull Sufficient energy bull Time scale set by He core collapsebull Disk-feeding time scale not disk-drainingbull Neutrino cooling allows accretionbull Neutrino annihilation energetically
possiblendash calculable in any case
Funnel geometry
channels any fireball
Density contrasts can
be huge
Ejet = f Maccc2
MHD
T = 57 ms
E = 5 x 1050 ergs
Edep = 28 x 1048 erg
Jet BirthThermal energy deposition focused by toroidal funnel structure
fmax ~ 06 - 4
Relativistic Jet Movie
Collapsar stages1 Iron core collapse disk formation
T~1010K ~108gcm-3 photodisintegration cooling pair capture disk is free nucleons (2 s)
2 Polar density declines to allow jet birthfrac12v3 Edep (2-5 s)
3 Jet tunnels out of star (5 s) Wolf-Rayet4 Jet powered for ~10 more seconds
Evacuates polar channel and reaches asymptotic speed (10 s)
T_GRB T_collapse
Jupiter
Red Supergiant
R~1013 cm
Blue Supergiant
R~1012 cm
Wolf-Rayet Star
R~1011 cm
Type Ib or Ic
Supernova
Supernovae
Ia
WD cosmology
Type II
Hydrogen
Type I
No Hydrogen
Ib Ic
exploding WR
thermonuclear old pop E galaxies
core collapse massive stars
Nickel Wind Movie
ldquoNickel Windrdquo
T gt 5 x 109 K
Fallback in weak SN explosions
Shock reaches
surface of star but parts of star are
not ejected to infinity
Fallback accretion Mms ~ 25 Msun Same star
exploded with a range of explosion energies
Significant accretion for thousands of
seconds ndash days
If fallback fuels a jet with power
fmc2
May power ldquohypernovardquo or long duration
GRBWeak
supernova shock
Shock breakout X-Ray transient
2 ldquoBriefrdquo jet tengine tjet
Engine dies before jet breakout
Mildly relativistic shock breakout
MacFadyen (1999)
What made SN1998bw+GRB980425
1 Accretion powered hypernova w Nickel wind
MacFadyen (2002)
E~ 1052 erg M(Ni)~05 M
GRB from ~3 shock breakout (Tan et al 2001 Perna amp Vietri 2002)
Collapsars
bull Can make ldquolongrdquo GRBs in H stripped (WR) stars tengine gt tescape
bull Short bursts may be compact binary mergersbull Need SN failure amp angular momentum
ndash Low metallicity binary can help
bull Star can explode -gt SN if nickel is made Predicts GRBSN association Type Ibc
bull SNGRB ratio may depend on angular momentumbull ldquoNickel windrdquo can explode star -gt hypernova
ndash H env Type II (no GRB) no H Type I + GRB
GRBGW bull Long GRBs
ndash not brighter than SN in GW
ndash very far Gpc
ndash very rare lt 1 SN
bull Short GBsndash merging ns-bh binaries
ndash maybe closer than long bursts
ndash short delay between event and GRB
ndash good for SWIFTLIGO
Rates
bull SN 1s = 100000 day
bull GRB 1day (BATSE) = 1000day
bull GRB rate = 1 of SN rate
bull maybe more collapsars than GRBs
bull =gt more rapidly rotating SN
bull SN with collapsar engine
bull look for bright Type Ic (w broad lines)
SN GW
bull SN1998bwGRB980425
bull 40 Mpc
bull maybe dominant GRB
bull rapid rotaters
bull SNAPROTSE look for 1998bw 2003dh like SN
bull many light curves -gt better t_explode
Implications
bull Probe engine directly
bull collapse duration vs GRB duration
bull collapseGRB delay (internal vs external)
bull disk properties ndash low viscosity big disks
Issues
bull too much j =gt no GRB but bright GW
bull may need low metallicity for GRB
bull prefer high redshift
bull donrsquot know nearby rate
bull but 980425 may imply rate is high
bull look for weak GRBs like 980425
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
With decreasing metallicity the bindingenergy of the core and the size of the silicon core both increase making black hole formation more likely atlow metallicity Woosley Heger amp Weaver RMP (2002)
Black hole formation may be unavoidable for low metallicity
Solar metallicity
Low metallicity
In the absence of mass lossand magnetic fields there wouldbe abundant progenitors
Unfortunately nature has both
15 solar mass helium core born rotating rigidly at f times break up
The more difficult problem is the angular momentum Thisis a problem shared by all current GRB models that invokemassive stars
- What is a Gamma-Ray Burst
- Superbowl Burst
- Slide 3
- 135 models (1993)
- Slide 5
- Slide 6
- Slide 7
- GRB991121
- GRB030329SN2003DH
- Slide 10
- Slide 11
- Slide 12
- GRB central engine
- ldquoDelayedrdquo SN Explosion
- Pre-Supernova Density Structure
- Failure of delayed mechanism
- Stellar Rotation
- Slide 18
- Slide 19
- Collapsar Simulations
- Collapsar Disk Animation
- Disk Formation Movie
- Slide 23
- Slide 24
- Slide 25
- Collapsar results
- Slide 27
- Jet Birth
- Relativistic Jet Movie
- Collapsar stages
- Slide 31
- Slide 32
- Nickel Wind Movie
- Slide 34
- Slide 35
- Slide 36
- Slide 37
- Slide 38
- Collapsars
- GRBGW
- Rates
- SN GW
- Implications
- Issues
- Principle Results
- Slide 46
- Slide 47
-
Muller (1999)
ldquoDelayedrdquo SN Explosion
ac
Accretion vs Neutrino heating
Burrows (2001)
Pre-Supernova Density Structure
Woosley amp Weaver (1995)
Bigger stars
Higher entropy
Shallower density gradients
Fryer ApJ 522 413 (1999) Burrows (1999)
Bigger stars
1 Accrete faster amp longer
2 Larger binding energy amp smaller explosion energy
explosion
binding
Failure of delayed mechanism
Fukuda (1982)
Heger (2000)
Stellar Rotation
no mass lossMass loss
No B fields
Collapsars
Type Masssun BH Time Scale Distance Comment
I 15-40 He prompt 20 s all z neutrino-dominated disk
II 10-40 He delayed 20 s ndash 1 hr all z black hole by fall back
III gt130 He prompt ~20 s zgt10 time dilated redshifted (1+z) very energetic pair instability low Z
A rotating massive star whose core collapses to a black hole and produces an accretion disk
Type I is what we are usually talking aboutThe 40 solar mass limit comes from assuming that all stars above 100 solar masses on the main sequence are unstable (except Pop III)
IFTwo plausible conditions occur
1 Failure of neutrino powered SN explosion
a completeb partial (fallback)
2 Rotating stellar coresj gt 3 x 1016 cm2s
THEN
Rapidly accreting black hole (M~01 Ms)fed by collapsing star (tdyn ~ 446 s frac12 ~ 10 s)Disk formation
COLLAPSAR
Collapsar Simulations
bull pre-SN 15 Msun Helium starbull Newtonian Hydrodynamics (PPM)bull alpha viscositybull rotationbull photodisintegration (NSE alpha n p)bull neutrino cooling thermal + URCA optically thinbull Ideal nucleons radiation relativistic degenerate
electrons positionsbull 2D axisymmetric spherical gridbull self gravity pseudo-Newtonian (PW)bull Rin = 9 Rs Rout = 9000 Rs
MacFadyen amp Woosley (1999)
Collapsar Disk AnimationPPM hydrodynamics Paczynski-Witta potential EOS neutrino cooling nuclear reactions viscosity
Stellar collapse w rotation
Density structure No disk no wind
Note Accretion shock funnel clearing pole to equator density contrast fluctuating polar density
Initial model 15 Msun Helium (Wolf-Rayet) star evolved with mass loss
R= 8 x 108 cm
Show inner 1 in radius disk mass = 001 M_sun
Low viscosity =001
Disk Formation Movie
Accretion Shock
Disk formation
t = 75 s
PhotodisintegrationSiOC -gt free neutronsAnd protons Enhanced neutrino cooling
neutrino coolong allows
accretion
no cooling=gt
dynamically unstable
CDAF
Could emit GWs but
maybe no GRB
= 01 ltMgt = 007 Msun s = 13 x 1053 ergs
spin
mass
Use 1D neutrino cooled
ldquoslimrdquo disk models
from Popham et al (1999)
Collapsar results
bull Sustained accretion gt10sbull Sufficient energy bull Time scale set by He core collapsebull Disk-feeding time scale not disk-drainingbull Neutrino cooling allows accretionbull Neutrino annihilation energetically
possiblendash calculable in any case
Funnel geometry
channels any fireball
Density contrasts can
be huge
Ejet = f Maccc2
MHD
T = 57 ms
E = 5 x 1050 ergs
Edep = 28 x 1048 erg
Jet BirthThermal energy deposition focused by toroidal funnel structure
fmax ~ 06 - 4
Relativistic Jet Movie
Collapsar stages1 Iron core collapse disk formation
T~1010K ~108gcm-3 photodisintegration cooling pair capture disk is free nucleons (2 s)
2 Polar density declines to allow jet birthfrac12v3 Edep (2-5 s)
3 Jet tunnels out of star (5 s) Wolf-Rayet4 Jet powered for ~10 more seconds
Evacuates polar channel and reaches asymptotic speed (10 s)
T_GRB T_collapse
Jupiter
Red Supergiant
R~1013 cm
Blue Supergiant
R~1012 cm
Wolf-Rayet Star
R~1011 cm
Type Ib or Ic
Supernova
Supernovae
Ia
WD cosmology
Type II
Hydrogen
Type I
No Hydrogen
Ib Ic
exploding WR
thermonuclear old pop E galaxies
core collapse massive stars
Nickel Wind Movie
ldquoNickel Windrdquo
T gt 5 x 109 K
Fallback in weak SN explosions
Shock reaches
surface of star but parts of star are
not ejected to infinity
Fallback accretion Mms ~ 25 Msun Same star
exploded with a range of explosion energies
Significant accretion for thousands of
seconds ndash days
If fallback fuels a jet with power
fmc2
May power ldquohypernovardquo or long duration
GRBWeak
supernova shock
Shock breakout X-Ray transient
2 ldquoBriefrdquo jet tengine tjet
Engine dies before jet breakout
Mildly relativistic shock breakout
MacFadyen (1999)
What made SN1998bw+GRB980425
1 Accretion powered hypernova w Nickel wind
MacFadyen (2002)
E~ 1052 erg M(Ni)~05 M
GRB from ~3 shock breakout (Tan et al 2001 Perna amp Vietri 2002)
Collapsars
bull Can make ldquolongrdquo GRBs in H stripped (WR) stars tengine gt tescape
bull Short bursts may be compact binary mergersbull Need SN failure amp angular momentum
ndash Low metallicity binary can help
bull Star can explode -gt SN if nickel is made Predicts GRBSN association Type Ibc
bull SNGRB ratio may depend on angular momentumbull ldquoNickel windrdquo can explode star -gt hypernova
ndash H env Type II (no GRB) no H Type I + GRB
GRBGW bull Long GRBs
ndash not brighter than SN in GW
ndash very far Gpc
ndash very rare lt 1 SN
bull Short GBsndash merging ns-bh binaries
ndash maybe closer than long bursts
ndash short delay between event and GRB
ndash good for SWIFTLIGO
Rates
bull SN 1s = 100000 day
bull GRB 1day (BATSE) = 1000day
bull GRB rate = 1 of SN rate
bull maybe more collapsars than GRBs
bull =gt more rapidly rotating SN
bull SN with collapsar engine
bull look for bright Type Ic (w broad lines)
SN GW
bull SN1998bwGRB980425
bull 40 Mpc
bull maybe dominant GRB
bull rapid rotaters
bull SNAPROTSE look for 1998bw 2003dh like SN
bull many light curves -gt better t_explode
Implications
bull Probe engine directly
bull collapse duration vs GRB duration
bull collapseGRB delay (internal vs external)
bull disk properties ndash low viscosity big disks
Issues
bull too much j =gt no GRB but bright GW
bull may need low metallicity for GRB
bull prefer high redshift
bull donrsquot know nearby rate
bull but 980425 may imply rate is high
bull look for weak GRBs like 980425
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
With decreasing metallicity the bindingenergy of the core and the size of the silicon core both increase making black hole formation more likely atlow metallicity Woosley Heger amp Weaver RMP (2002)
Black hole formation may be unavoidable for low metallicity
Solar metallicity
Low metallicity
In the absence of mass lossand magnetic fields there wouldbe abundant progenitors
Unfortunately nature has both
15 solar mass helium core born rotating rigidly at f times break up
The more difficult problem is the angular momentum Thisis a problem shared by all current GRB models that invokemassive stars
- What is a Gamma-Ray Burst
- Superbowl Burst
- Slide 3
- 135 models (1993)
- Slide 5
- Slide 6
- Slide 7
- GRB991121
- GRB030329SN2003DH
- Slide 10
- Slide 11
- Slide 12
- GRB central engine
- ldquoDelayedrdquo SN Explosion
- Pre-Supernova Density Structure
- Failure of delayed mechanism
- Stellar Rotation
- Slide 18
- Slide 19
- Collapsar Simulations
- Collapsar Disk Animation
- Disk Formation Movie
- Slide 23
- Slide 24
- Slide 25
- Collapsar results
- Slide 27
- Jet Birth
- Relativistic Jet Movie
- Collapsar stages
- Slide 31
- Slide 32
- Nickel Wind Movie
- Slide 34
- Slide 35
- Slide 36
- Slide 37
- Slide 38
- Collapsars
- GRBGW
- Rates
- SN GW
- Implications
- Issues
- Principle Results
- Slide 46
- Slide 47
-
Pre-Supernova Density Structure
Woosley amp Weaver (1995)
Bigger stars
Higher entropy
Shallower density gradients
Fryer ApJ 522 413 (1999) Burrows (1999)
Bigger stars
1 Accrete faster amp longer
2 Larger binding energy amp smaller explosion energy
explosion
binding
Failure of delayed mechanism
Fukuda (1982)
Heger (2000)
Stellar Rotation
no mass lossMass loss
No B fields
Collapsars
Type Masssun BH Time Scale Distance Comment
I 15-40 He prompt 20 s all z neutrino-dominated disk
II 10-40 He delayed 20 s ndash 1 hr all z black hole by fall back
III gt130 He prompt ~20 s zgt10 time dilated redshifted (1+z) very energetic pair instability low Z
A rotating massive star whose core collapses to a black hole and produces an accretion disk
Type I is what we are usually talking aboutThe 40 solar mass limit comes from assuming that all stars above 100 solar masses on the main sequence are unstable (except Pop III)
IFTwo plausible conditions occur
1 Failure of neutrino powered SN explosion
a completeb partial (fallback)
2 Rotating stellar coresj gt 3 x 1016 cm2s
THEN
Rapidly accreting black hole (M~01 Ms)fed by collapsing star (tdyn ~ 446 s frac12 ~ 10 s)Disk formation
COLLAPSAR
Collapsar Simulations
bull pre-SN 15 Msun Helium starbull Newtonian Hydrodynamics (PPM)bull alpha viscositybull rotationbull photodisintegration (NSE alpha n p)bull neutrino cooling thermal + URCA optically thinbull Ideal nucleons radiation relativistic degenerate
electrons positionsbull 2D axisymmetric spherical gridbull self gravity pseudo-Newtonian (PW)bull Rin = 9 Rs Rout = 9000 Rs
MacFadyen amp Woosley (1999)
Collapsar Disk AnimationPPM hydrodynamics Paczynski-Witta potential EOS neutrino cooling nuclear reactions viscosity
Stellar collapse w rotation
Density structure No disk no wind
Note Accretion shock funnel clearing pole to equator density contrast fluctuating polar density
Initial model 15 Msun Helium (Wolf-Rayet) star evolved with mass loss
R= 8 x 108 cm
Show inner 1 in radius disk mass = 001 M_sun
Low viscosity =001
Disk Formation Movie
Accretion Shock
Disk formation
t = 75 s
PhotodisintegrationSiOC -gt free neutronsAnd protons Enhanced neutrino cooling
neutrino coolong allows
accretion
no cooling=gt
dynamically unstable
CDAF
Could emit GWs but
maybe no GRB
= 01 ltMgt = 007 Msun s = 13 x 1053 ergs
spin
mass
Use 1D neutrino cooled
ldquoslimrdquo disk models
from Popham et al (1999)
Collapsar results
bull Sustained accretion gt10sbull Sufficient energy bull Time scale set by He core collapsebull Disk-feeding time scale not disk-drainingbull Neutrino cooling allows accretionbull Neutrino annihilation energetically
possiblendash calculable in any case
Funnel geometry
channels any fireball
Density contrasts can
be huge
Ejet = f Maccc2
MHD
T = 57 ms
E = 5 x 1050 ergs
Edep = 28 x 1048 erg
Jet BirthThermal energy deposition focused by toroidal funnel structure
fmax ~ 06 - 4
Relativistic Jet Movie
Collapsar stages1 Iron core collapse disk formation
T~1010K ~108gcm-3 photodisintegration cooling pair capture disk is free nucleons (2 s)
2 Polar density declines to allow jet birthfrac12v3 Edep (2-5 s)
3 Jet tunnels out of star (5 s) Wolf-Rayet4 Jet powered for ~10 more seconds
Evacuates polar channel and reaches asymptotic speed (10 s)
T_GRB T_collapse
Jupiter
Red Supergiant
R~1013 cm
Blue Supergiant
R~1012 cm
Wolf-Rayet Star
R~1011 cm
Type Ib or Ic
Supernova
Supernovae
Ia
WD cosmology
Type II
Hydrogen
Type I
No Hydrogen
Ib Ic
exploding WR
thermonuclear old pop E galaxies
core collapse massive stars
Nickel Wind Movie
ldquoNickel Windrdquo
T gt 5 x 109 K
Fallback in weak SN explosions
Shock reaches
surface of star but parts of star are
not ejected to infinity
Fallback accretion Mms ~ 25 Msun Same star
exploded with a range of explosion energies
Significant accretion for thousands of
seconds ndash days
If fallback fuels a jet with power
fmc2
May power ldquohypernovardquo or long duration
GRBWeak
supernova shock
Shock breakout X-Ray transient
2 ldquoBriefrdquo jet tengine tjet
Engine dies before jet breakout
Mildly relativistic shock breakout
MacFadyen (1999)
What made SN1998bw+GRB980425
1 Accretion powered hypernova w Nickel wind
MacFadyen (2002)
E~ 1052 erg M(Ni)~05 M
GRB from ~3 shock breakout (Tan et al 2001 Perna amp Vietri 2002)
Collapsars
bull Can make ldquolongrdquo GRBs in H stripped (WR) stars tengine gt tescape
bull Short bursts may be compact binary mergersbull Need SN failure amp angular momentum
ndash Low metallicity binary can help
bull Star can explode -gt SN if nickel is made Predicts GRBSN association Type Ibc
bull SNGRB ratio may depend on angular momentumbull ldquoNickel windrdquo can explode star -gt hypernova
ndash H env Type II (no GRB) no H Type I + GRB
GRBGW bull Long GRBs
ndash not brighter than SN in GW
ndash very far Gpc
ndash very rare lt 1 SN
bull Short GBsndash merging ns-bh binaries
ndash maybe closer than long bursts
ndash short delay between event and GRB
ndash good for SWIFTLIGO
Rates
bull SN 1s = 100000 day
bull GRB 1day (BATSE) = 1000day
bull GRB rate = 1 of SN rate
bull maybe more collapsars than GRBs
bull =gt more rapidly rotating SN
bull SN with collapsar engine
bull look for bright Type Ic (w broad lines)
SN GW
bull SN1998bwGRB980425
bull 40 Mpc
bull maybe dominant GRB
bull rapid rotaters
bull SNAPROTSE look for 1998bw 2003dh like SN
bull many light curves -gt better t_explode
Implications
bull Probe engine directly
bull collapse duration vs GRB duration
bull collapseGRB delay (internal vs external)
bull disk properties ndash low viscosity big disks
Issues
bull too much j =gt no GRB but bright GW
bull may need low metallicity for GRB
bull prefer high redshift
bull donrsquot know nearby rate
bull but 980425 may imply rate is high
bull look for weak GRBs like 980425
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
With decreasing metallicity the bindingenergy of the core and the size of the silicon core both increase making black hole formation more likely atlow metallicity Woosley Heger amp Weaver RMP (2002)
Black hole formation may be unavoidable for low metallicity
Solar metallicity
Low metallicity
In the absence of mass lossand magnetic fields there wouldbe abundant progenitors
Unfortunately nature has both
15 solar mass helium core born rotating rigidly at f times break up
The more difficult problem is the angular momentum Thisis a problem shared by all current GRB models that invokemassive stars
- What is a Gamma-Ray Burst
- Superbowl Burst
- Slide 3
- 135 models (1993)
- Slide 5
- Slide 6
- Slide 7
- GRB991121
- GRB030329SN2003DH
- Slide 10
- Slide 11
- Slide 12
- GRB central engine
- ldquoDelayedrdquo SN Explosion
- Pre-Supernova Density Structure
- Failure of delayed mechanism
- Stellar Rotation
- Slide 18
- Slide 19
- Collapsar Simulations
- Collapsar Disk Animation
- Disk Formation Movie
- Slide 23
- Slide 24
- Slide 25
- Collapsar results
- Slide 27
- Jet Birth
- Relativistic Jet Movie
- Collapsar stages
- Slide 31
- Slide 32
- Nickel Wind Movie
- Slide 34
- Slide 35
- Slide 36
- Slide 37
- Slide 38
- Collapsars
- GRBGW
- Rates
- SN GW
- Implications
- Issues
- Principle Results
- Slide 46
- Slide 47
-
Fryer ApJ 522 413 (1999) Burrows (1999)
Bigger stars
1 Accrete faster amp longer
2 Larger binding energy amp smaller explosion energy
explosion
binding
Failure of delayed mechanism
Fukuda (1982)
Heger (2000)
Stellar Rotation
no mass lossMass loss
No B fields
Collapsars
Type Masssun BH Time Scale Distance Comment
I 15-40 He prompt 20 s all z neutrino-dominated disk
II 10-40 He delayed 20 s ndash 1 hr all z black hole by fall back
III gt130 He prompt ~20 s zgt10 time dilated redshifted (1+z) very energetic pair instability low Z
A rotating massive star whose core collapses to a black hole and produces an accretion disk
Type I is what we are usually talking aboutThe 40 solar mass limit comes from assuming that all stars above 100 solar masses on the main sequence are unstable (except Pop III)
IFTwo plausible conditions occur
1 Failure of neutrino powered SN explosion
a completeb partial (fallback)
2 Rotating stellar coresj gt 3 x 1016 cm2s
THEN
Rapidly accreting black hole (M~01 Ms)fed by collapsing star (tdyn ~ 446 s frac12 ~ 10 s)Disk formation
COLLAPSAR
Collapsar Simulations
bull pre-SN 15 Msun Helium starbull Newtonian Hydrodynamics (PPM)bull alpha viscositybull rotationbull photodisintegration (NSE alpha n p)bull neutrino cooling thermal + URCA optically thinbull Ideal nucleons radiation relativistic degenerate
electrons positionsbull 2D axisymmetric spherical gridbull self gravity pseudo-Newtonian (PW)bull Rin = 9 Rs Rout = 9000 Rs
MacFadyen amp Woosley (1999)
Collapsar Disk AnimationPPM hydrodynamics Paczynski-Witta potential EOS neutrino cooling nuclear reactions viscosity
Stellar collapse w rotation
Density structure No disk no wind
Note Accretion shock funnel clearing pole to equator density contrast fluctuating polar density
Initial model 15 Msun Helium (Wolf-Rayet) star evolved with mass loss
R= 8 x 108 cm
Show inner 1 in radius disk mass = 001 M_sun
Low viscosity =001
Disk Formation Movie
Accretion Shock
Disk formation
t = 75 s
PhotodisintegrationSiOC -gt free neutronsAnd protons Enhanced neutrino cooling
neutrino coolong allows
accretion
no cooling=gt
dynamically unstable
CDAF
Could emit GWs but
maybe no GRB
= 01 ltMgt = 007 Msun s = 13 x 1053 ergs
spin
mass
Use 1D neutrino cooled
ldquoslimrdquo disk models
from Popham et al (1999)
Collapsar results
bull Sustained accretion gt10sbull Sufficient energy bull Time scale set by He core collapsebull Disk-feeding time scale not disk-drainingbull Neutrino cooling allows accretionbull Neutrino annihilation energetically
possiblendash calculable in any case
Funnel geometry
channels any fireball
Density contrasts can
be huge
Ejet = f Maccc2
MHD
T = 57 ms
E = 5 x 1050 ergs
Edep = 28 x 1048 erg
Jet BirthThermal energy deposition focused by toroidal funnel structure
fmax ~ 06 - 4
Relativistic Jet Movie
Collapsar stages1 Iron core collapse disk formation
T~1010K ~108gcm-3 photodisintegration cooling pair capture disk is free nucleons (2 s)
2 Polar density declines to allow jet birthfrac12v3 Edep (2-5 s)
3 Jet tunnels out of star (5 s) Wolf-Rayet4 Jet powered for ~10 more seconds
Evacuates polar channel and reaches asymptotic speed (10 s)
T_GRB T_collapse
Jupiter
Red Supergiant
R~1013 cm
Blue Supergiant
R~1012 cm
Wolf-Rayet Star
R~1011 cm
Type Ib or Ic
Supernova
Supernovae
Ia
WD cosmology
Type II
Hydrogen
Type I
No Hydrogen
Ib Ic
exploding WR
thermonuclear old pop E galaxies
core collapse massive stars
Nickel Wind Movie
ldquoNickel Windrdquo
T gt 5 x 109 K
Fallback in weak SN explosions
Shock reaches
surface of star but parts of star are
not ejected to infinity
Fallback accretion Mms ~ 25 Msun Same star
exploded with a range of explosion energies
Significant accretion for thousands of
seconds ndash days
If fallback fuels a jet with power
fmc2
May power ldquohypernovardquo or long duration
GRBWeak
supernova shock
Shock breakout X-Ray transient
2 ldquoBriefrdquo jet tengine tjet
Engine dies before jet breakout
Mildly relativistic shock breakout
MacFadyen (1999)
What made SN1998bw+GRB980425
1 Accretion powered hypernova w Nickel wind
MacFadyen (2002)
E~ 1052 erg M(Ni)~05 M
GRB from ~3 shock breakout (Tan et al 2001 Perna amp Vietri 2002)
Collapsars
bull Can make ldquolongrdquo GRBs in H stripped (WR) stars tengine gt tescape
bull Short bursts may be compact binary mergersbull Need SN failure amp angular momentum
ndash Low metallicity binary can help
bull Star can explode -gt SN if nickel is made Predicts GRBSN association Type Ibc
bull SNGRB ratio may depend on angular momentumbull ldquoNickel windrdquo can explode star -gt hypernova
ndash H env Type II (no GRB) no H Type I + GRB
GRBGW bull Long GRBs
ndash not brighter than SN in GW
ndash very far Gpc
ndash very rare lt 1 SN
bull Short GBsndash merging ns-bh binaries
ndash maybe closer than long bursts
ndash short delay between event and GRB
ndash good for SWIFTLIGO
Rates
bull SN 1s = 100000 day
bull GRB 1day (BATSE) = 1000day
bull GRB rate = 1 of SN rate
bull maybe more collapsars than GRBs
bull =gt more rapidly rotating SN
bull SN with collapsar engine
bull look for bright Type Ic (w broad lines)
SN GW
bull SN1998bwGRB980425
bull 40 Mpc
bull maybe dominant GRB
bull rapid rotaters
bull SNAPROTSE look for 1998bw 2003dh like SN
bull many light curves -gt better t_explode
Implications
bull Probe engine directly
bull collapse duration vs GRB duration
bull collapseGRB delay (internal vs external)
bull disk properties ndash low viscosity big disks
Issues
bull too much j =gt no GRB but bright GW
bull may need low metallicity for GRB
bull prefer high redshift
bull donrsquot know nearby rate
bull but 980425 may imply rate is high
bull look for weak GRBs like 980425
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
With decreasing metallicity the bindingenergy of the core and the size of the silicon core both increase making black hole formation more likely atlow metallicity Woosley Heger amp Weaver RMP (2002)
Black hole formation may be unavoidable for low metallicity
Solar metallicity
Low metallicity
In the absence of mass lossand magnetic fields there wouldbe abundant progenitors
Unfortunately nature has both
15 solar mass helium core born rotating rigidly at f times break up
The more difficult problem is the angular momentum Thisis a problem shared by all current GRB models that invokemassive stars
- What is a Gamma-Ray Burst
- Superbowl Burst
- Slide 3
- 135 models (1993)
- Slide 5
- Slide 6
- Slide 7
- GRB991121
- GRB030329SN2003DH
- Slide 10
- Slide 11
- Slide 12
- GRB central engine
- ldquoDelayedrdquo SN Explosion
- Pre-Supernova Density Structure
- Failure of delayed mechanism
- Stellar Rotation
- Slide 18
- Slide 19
- Collapsar Simulations
- Collapsar Disk Animation
- Disk Formation Movie
- Slide 23
- Slide 24
- Slide 25
- Collapsar results
- Slide 27
- Jet Birth
- Relativistic Jet Movie
- Collapsar stages
- Slide 31
- Slide 32
- Nickel Wind Movie
- Slide 34
- Slide 35
- Slide 36
- Slide 37
- Slide 38
- Collapsars
- GRBGW
- Rates
- SN GW
- Implications
- Issues
- Principle Results
- Slide 46
- Slide 47
-
Fukuda (1982)
Heger (2000)
Stellar Rotation
no mass lossMass loss
No B fields
Collapsars
Type Masssun BH Time Scale Distance Comment
I 15-40 He prompt 20 s all z neutrino-dominated disk
II 10-40 He delayed 20 s ndash 1 hr all z black hole by fall back
III gt130 He prompt ~20 s zgt10 time dilated redshifted (1+z) very energetic pair instability low Z
A rotating massive star whose core collapses to a black hole and produces an accretion disk
Type I is what we are usually talking aboutThe 40 solar mass limit comes from assuming that all stars above 100 solar masses on the main sequence are unstable (except Pop III)
IFTwo plausible conditions occur
1 Failure of neutrino powered SN explosion
a completeb partial (fallback)
2 Rotating stellar coresj gt 3 x 1016 cm2s
THEN
Rapidly accreting black hole (M~01 Ms)fed by collapsing star (tdyn ~ 446 s frac12 ~ 10 s)Disk formation
COLLAPSAR
Collapsar Simulations
bull pre-SN 15 Msun Helium starbull Newtonian Hydrodynamics (PPM)bull alpha viscositybull rotationbull photodisintegration (NSE alpha n p)bull neutrino cooling thermal + URCA optically thinbull Ideal nucleons radiation relativistic degenerate
electrons positionsbull 2D axisymmetric spherical gridbull self gravity pseudo-Newtonian (PW)bull Rin = 9 Rs Rout = 9000 Rs
MacFadyen amp Woosley (1999)
Collapsar Disk AnimationPPM hydrodynamics Paczynski-Witta potential EOS neutrino cooling nuclear reactions viscosity
Stellar collapse w rotation
Density structure No disk no wind
Note Accretion shock funnel clearing pole to equator density contrast fluctuating polar density
Initial model 15 Msun Helium (Wolf-Rayet) star evolved with mass loss
R= 8 x 108 cm
Show inner 1 in radius disk mass = 001 M_sun
Low viscosity =001
Disk Formation Movie
Accretion Shock
Disk formation
t = 75 s
PhotodisintegrationSiOC -gt free neutronsAnd protons Enhanced neutrino cooling
neutrino coolong allows
accretion
no cooling=gt
dynamically unstable
CDAF
Could emit GWs but
maybe no GRB
= 01 ltMgt = 007 Msun s = 13 x 1053 ergs
spin
mass
Use 1D neutrino cooled
ldquoslimrdquo disk models
from Popham et al (1999)
Collapsar results
bull Sustained accretion gt10sbull Sufficient energy bull Time scale set by He core collapsebull Disk-feeding time scale not disk-drainingbull Neutrino cooling allows accretionbull Neutrino annihilation energetically
possiblendash calculable in any case
Funnel geometry
channels any fireball
Density contrasts can
be huge
Ejet = f Maccc2
MHD
T = 57 ms
E = 5 x 1050 ergs
Edep = 28 x 1048 erg
Jet BirthThermal energy deposition focused by toroidal funnel structure
fmax ~ 06 - 4
Relativistic Jet Movie
Collapsar stages1 Iron core collapse disk formation
T~1010K ~108gcm-3 photodisintegration cooling pair capture disk is free nucleons (2 s)
2 Polar density declines to allow jet birthfrac12v3 Edep (2-5 s)
3 Jet tunnels out of star (5 s) Wolf-Rayet4 Jet powered for ~10 more seconds
Evacuates polar channel and reaches asymptotic speed (10 s)
T_GRB T_collapse
Jupiter
Red Supergiant
R~1013 cm
Blue Supergiant
R~1012 cm
Wolf-Rayet Star
R~1011 cm
Type Ib or Ic
Supernova
Supernovae
Ia
WD cosmology
Type II
Hydrogen
Type I
No Hydrogen
Ib Ic
exploding WR
thermonuclear old pop E galaxies
core collapse massive stars
Nickel Wind Movie
ldquoNickel Windrdquo
T gt 5 x 109 K
Fallback in weak SN explosions
Shock reaches
surface of star but parts of star are
not ejected to infinity
Fallback accretion Mms ~ 25 Msun Same star
exploded with a range of explosion energies
Significant accretion for thousands of
seconds ndash days
If fallback fuels a jet with power
fmc2
May power ldquohypernovardquo or long duration
GRBWeak
supernova shock
Shock breakout X-Ray transient
2 ldquoBriefrdquo jet tengine tjet
Engine dies before jet breakout
Mildly relativistic shock breakout
MacFadyen (1999)
What made SN1998bw+GRB980425
1 Accretion powered hypernova w Nickel wind
MacFadyen (2002)
E~ 1052 erg M(Ni)~05 M
GRB from ~3 shock breakout (Tan et al 2001 Perna amp Vietri 2002)
Collapsars
bull Can make ldquolongrdquo GRBs in H stripped (WR) stars tengine gt tescape
bull Short bursts may be compact binary mergersbull Need SN failure amp angular momentum
ndash Low metallicity binary can help
bull Star can explode -gt SN if nickel is made Predicts GRBSN association Type Ibc
bull SNGRB ratio may depend on angular momentumbull ldquoNickel windrdquo can explode star -gt hypernova
ndash H env Type II (no GRB) no H Type I + GRB
GRBGW bull Long GRBs
ndash not brighter than SN in GW
ndash very far Gpc
ndash very rare lt 1 SN
bull Short GBsndash merging ns-bh binaries
ndash maybe closer than long bursts
ndash short delay between event and GRB
ndash good for SWIFTLIGO
Rates
bull SN 1s = 100000 day
bull GRB 1day (BATSE) = 1000day
bull GRB rate = 1 of SN rate
bull maybe more collapsars than GRBs
bull =gt more rapidly rotating SN
bull SN with collapsar engine
bull look for bright Type Ic (w broad lines)
SN GW
bull SN1998bwGRB980425
bull 40 Mpc
bull maybe dominant GRB
bull rapid rotaters
bull SNAPROTSE look for 1998bw 2003dh like SN
bull many light curves -gt better t_explode
Implications
bull Probe engine directly
bull collapse duration vs GRB duration
bull collapseGRB delay (internal vs external)
bull disk properties ndash low viscosity big disks
Issues
bull too much j =gt no GRB but bright GW
bull may need low metallicity for GRB
bull prefer high redshift
bull donrsquot know nearby rate
bull but 980425 may imply rate is high
bull look for weak GRBs like 980425
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
With decreasing metallicity the bindingenergy of the core and the size of the silicon core both increase making black hole formation more likely atlow metallicity Woosley Heger amp Weaver RMP (2002)
Black hole formation may be unavoidable for low metallicity
Solar metallicity
Low metallicity
In the absence of mass lossand magnetic fields there wouldbe abundant progenitors
Unfortunately nature has both
15 solar mass helium core born rotating rigidly at f times break up
The more difficult problem is the angular momentum Thisis a problem shared by all current GRB models that invokemassive stars
- What is a Gamma-Ray Burst
- Superbowl Burst
- Slide 3
- 135 models (1993)
- Slide 5
- Slide 6
- Slide 7
- GRB991121
- GRB030329SN2003DH
- Slide 10
- Slide 11
- Slide 12
- GRB central engine
- ldquoDelayedrdquo SN Explosion
- Pre-Supernova Density Structure
- Failure of delayed mechanism
- Stellar Rotation
- Slide 18
- Slide 19
- Collapsar Simulations
- Collapsar Disk Animation
- Disk Formation Movie
- Slide 23
- Slide 24
- Slide 25
- Collapsar results
- Slide 27
- Jet Birth
- Relativistic Jet Movie
- Collapsar stages
- Slide 31
- Slide 32
- Nickel Wind Movie
- Slide 34
- Slide 35
- Slide 36
- Slide 37
- Slide 38
- Collapsars
- GRBGW
- Rates
- SN GW
- Implications
- Issues
- Principle Results
- Slide 46
- Slide 47
-
Collapsars
Type Masssun BH Time Scale Distance Comment
I 15-40 He prompt 20 s all z neutrino-dominated disk
II 10-40 He delayed 20 s ndash 1 hr all z black hole by fall back
III gt130 He prompt ~20 s zgt10 time dilated redshifted (1+z) very energetic pair instability low Z
A rotating massive star whose core collapses to a black hole and produces an accretion disk
Type I is what we are usually talking aboutThe 40 solar mass limit comes from assuming that all stars above 100 solar masses on the main sequence are unstable (except Pop III)
IFTwo plausible conditions occur
1 Failure of neutrino powered SN explosion
a completeb partial (fallback)
2 Rotating stellar coresj gt 3 x 1016 cm2s
THEN
Rapidly accreting black hole (M~01 Ms)fed by collapsing star (tdyn ~ 446 s frac12 ~ 10 s)Disk formation
COLLAPSAR
Collapsar Simulations
bull pre-SN 15 Msun Helium starbull Newtonian Hydrodynamics (PPM)bull alpha viscositybull rotationbull photodisintegration (NSE alpha n p)bull neutrino cooling thermal + URCA optically thinbull Ideal nucleons radiation relativistic degenerate
electrons positionsbull 2D axisymmetric spherical gridbull self gravity pseudo-Newtonian (PW)bull Rin = 9 Rs Rout = 9000 Rs
MacFadyen amp Woosley (1999)
Collapsar Disk AnimationPPM hydrodynamics Paczynski-Witta potential EOS neutrino cooling nuclear reactions viscosity
Stellar collapse w rotation
Density structure No disk no wind
Note Accretion shock funnel clearing pole to equator density contrast fluctuating polar density
Initial model 15 Msun Helium (Wolf-Rayet) star evolved with mass loss
R= 8 x 108 cm
Show inner 1 in radius disk mass = 001 M_sun
Low viscosity =001
Disk Formation Movie
Accretion Shock
Disk formation
t = 75 s
PhotodisintegrationSiOC -gt free neutronsAnd protons Enhanced neutrino cooling
neutrino coolong allows
accretion
no cooling=gt
dynamically unstable
CDAF
Could emit GWs but
maybe no GRB
= 01 ltMgt = 007 Msun s = 13 x 1053 ergs
spin
mass
Use 1D neutrino cooled
ldquoslimrdquo disk models
from Popham et al (1999)
Collapsar results
bull Sustained accretion gt10sbull Sufficient energy bull Time scale set by He core collapsebull Disk-feeding time scale not disk-drainingbull Neutrino cooling allows accretionbull Neutrino annihilation energetically
possiblendash calculable in any case
Funnel geometry
channels any fireball
Density contrasts can
be huge
Ejet = f Maccc2
MHD
T = 57 ms
E = 5 x 1050 ergs
Edep = 28 x 1048 erg
Jet BirthThermal energy deposition focused by toroidal funnel structure
fmax ~ 06 - 4
Relativistic Jet Movie
Collapsar stages1 Iron core collapse disk formation
T~1010K ~108gcm-3 photodisintegration cooling pair capture disk is free nucleons (2 s)
2 Polar density declines to allow jet birthfrac12v3 Edep (2-5 s)
3 Jet tunnels out of star (5 s) Wolf-Rayet4 Jet powered for ~10 more seconds
Evacuates polar channel and reaches asymptotic speed (10 s)
T_GRB T_collapse
Jupiter
Red Supergiant
R~1013 cm
Blue Supergiant
R~1012 cm
Wolf-Rayet Star
R~1011 cm
Type Ib or Ic
Supernova
Supernovae
Ia
WD cosmology
Type II
Hydrogen
Type I
No Hydrogen
Ib Ic
exploding WR
thermonuclear old pop E galaxies
core collapse massive stars
Nickel Wind Movie
ldquoNickel Windrdquo
T gt 5 x 109 K
Fallback in weak SN explosions
Shock reaches
surface of star but parts of star are
not ejected to infinity
Fallback accretion Mms ~ 25 Msun Same star
exploded with a range of explosion energies
Significant accretion for thousands of
seconds ndash days
If fallback fuels a jet with power
fmc2
May power ldquohypernovardquo or long duration
GRBWeak
supernova shock
Shock breakout X-Ray transient
2 ldquoBriefrdquo jet tengine tjet
Engine dies before jet breakout
Mildly relativistic shock breakout
MacFadyen (1999)
What made SN1998bw+GRB980425
1 Accretion powered hypernova w Nickel wind
MacFadyen (2002)
E~ 1052 erg M(Ni)~05 M
GRB from ~3 shock breakout (Tan et al 2001 Perna amp Vietri 2002)
Collapsars
bull Can make ldquolongrdquo GRBs in H stripped (WR) stars tengine gt tescape
bull Short bursts may be compact binary mergersbull Need SN failure amp angular momentum
ndash Low metallicity binary can help
bull Star can explode -gt SN if nickel is made Predicts GRBSN association Type Ibc
bull SNGRB ratio may depend on angular momentumbull ldquoNickel windrdquo can explode star -gt hypernova
ndash H env Type II (no GRB) no H Type I + GRB
GRBGW bull Long GRBs
ndash not brighter than SN in GW
ndash very far Gpc
ndash very rare lt 1 SN
bull Short GBsndash merging ns-bh binaries
ndash maybe closer than long bursts
ndash short delay between event and GRB
ndash good for SWIFTLIGO
Rates
bull SN 1s = 100000 day
bull GRB 1day (BATSE) = 1000day
bull GRB rate = 1 of SN rate
bull maybe more collapsars than GRBs
bull =gt more rapidly rotating SN
bull SN with collapsar engine
bull look for bright Type Ic (w broad lines)
SN GW
bull SN1998bwGRB980425
bull 40 Mpc
bull maybe dominant GRB
bull rapid rotaters
bull SNAPROTSE look for 1998bw 2003dh like SN
bull many light curves -gt better t_explode
Implications
bull Probe engine directly
bull collapse duration vs GRB duration
bull collapseGRB delay (internal vs external)
bull disk properties ndash low viscosity big disks
Issues
bull too much j =gt no GRB but bright GW
bull may need low metallicity for GRB
bull prefer high redshift
bull donrsquot know nearby rate
bull but 980425 may imply rate is high
bull look for weak GRBs like 980425
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
With decreasing metallicity the bindingenergy of the core and the size of the silicon core both increase making black hole formation more likely atlow metallicity Woosley Heger amp Weaver RMP (2002)
Black hole formation may be unavoidable for low metallicity
Solar metallicity
Low metallicity
In the absence of mass lossand magnetic fields there wouldbe abundant progenitors
Unfortunately nature has both
15 solar mass helium core born rotating rigidly at f times break up
The more difficult problem is the angular momentum Thisis a problem shared by all current GRB models that invokemassive stars
- What is a Gamma-Ray Burst
- Superbowl Burst
- Slide 3
- 135 models (1993)
- Slide 5
- Slide 6
- Slide 7
- GRB991121
- GRB030329SN2003DH
- Slide 10
- Slide 11
- Slide 12
- GRB central engine
- ldquoDelayedrdquo SN Explosion
- Pre-Supernova Density Structure
- Failure of delayed mechanism
- Stellar Rotation
- Slide 18
- Slide 19
- Collapsar Simulations
- Collapsar Disk Animation
- Disk Formation Movie
- Slide 23
- Slide 24
- Slide 25
- Collapsar results
- Slide 27
- Jet Birth
- Relativistic Jet Movie
- Collapsar stages
- Slide 31
- Slide 32
- Nickel Wind Movie
- Slide 34
- Slide 35
- Slide 36
- Slide 37
- Slide 38
- Collapsars
- GRBGW
- Rates
- SN GW
- Implications
- Issues
- Principle Results
- Slide 46
- Slide 47
-
IFTwo plausible conditions occur
1 Failure of neutrino powered SN explosion
a completeb partial (fallback)
2 Rotating stellar coresj gt 3 x 1016 cm2s
THEN
Rapidly accreting black hole (M~01 Ms)fed by collapsing star (tdyn ~ 446 s frac12 ~ 10 s)Disk formation
COLLAPSAR
Collapsar Simulations
bull pre-SN 15 Msun Helium starbull Newtonian Hydrodynamics (PPM)bull alpha viscositybull rotationbull photodisintegration (NSE alpha n p)bull neutrino cooling thermal + URCA optically thinbull Ideal nucleons radiation relativistic degenerate
electrons positionsbull 2D axisymmetric spherical gridbull self gravity pseudo-Newtonian (PW)bull Rin = 9 Rs Rout = 9000 Rs
MacFadyen amp Woosley (1999)
Collapsar Disk AnimationPPM hydrodynamics Paczynski-Witta potential EOS neutrino cooling nuclear reactions viscosity
Stellar collapse w rotation
Density structure No disk no wind
Note Accretion shock funnel clearing pole to equator density contrast fluctuating polar density
Initial model 15 Msun Helium (Wolf-Rayet) star evolved with mass loss
R= 8 x 108 cm
Show inner 1 in radius disk mass = 001 M_sun
Low viscosity =001
Disk Formation Movie
Accretion Shock
Disk formation
t = 75 s
PhotodisintegrationSiOC -gt free neutronsAnd protons Enhanced neutrino cooling
neutrino coolong allows
accretion
no cooling=gt
dynamically unstable
CDAF
Could emit GWs but
maybe no GRB
= 01 ltMgt = 007 Msun s = 13 x 1053 ergs
spin
mass
Use 1D neutrino cooled
ldquoslimrdquo disk models
from Popham et al (1999)
Collapsar results
bull Sustained accretion gt10sbull Sufficient energy bull Time scale set by He core collapsebull Disk-feeding time scale not disk-drainingbull Neutrino cooling allows accretionbull Neutrino annihilation energetically
possiblendash calculable in any case
Funnel geometry
channels any fireball
Density contrasts can
be huge
Ejet = f Maccc2
MHD
T = 57 ms
E = 5 x 1050 ergs
Edep = 28 x 1048 erg
Jet BirthThermal energy deposition focused by toroidal funnel structure
fmax ~ 06 - 4
Relativistic Jet Movie
Collapsar stages1 Iron core collapse disk formation
T~1010K ~108gcm-3 photodisintegration cooling pair capture disk is free nucleons (2 s)
2 Polar density declines to allow jet birthfrac12v3 Edep (2-5 s)
3 Jet tunnels out of star (5 s) Wolf-Rayet4 Jet powered for ~10 more seconds
Evacuates polar channel and reaches asymptotic speed (10 s)
T_GRB T_collapse
Jupiter
Red Supergiant
R~1013 cm
Blue Supergiant
R~1012 cm
Wolf-Rayet Star
R~1011 cm
Type Ib or Ic
Supernova
Supernovae
Ia
WD cosmology
Type II
Hydrogen
Type I
No Hydrogen
Ib Ic
exploding WR
thermonuclear old pop E galaxies
core collapse massive stars
Nickel Wind Movie
ldquoNickel Windrdquo
T gt 5 x 109 K
Fallback in weak SN explosions
Shock reaches
surface of star but parts of star are
not ejected to infinity
Fallback accretion Mms ~ 25 Msun Same star
exploded with a range of explosion energies
Significant accretion for thousands of
seconds ndash days
If fallback fuels a jet with power
fmc2
May power ldquohypernovardquo or long duration
GRBWeak
supernova shock
Shock breakout X-Ray transient
2 ldquoBriefrdquo jet tengine tjet
Engine dies before jet breakout
Mildly relativistic shock breakout
MacFadyen (1999)
What made SN1998bw+GRB980425
1 Accretion powered hypernova w Nickel wind
MacFadyen (2002)
E~ 1052 erg M(Ni)~05 M
GRB from ~3 shock breakout (Tan et al 2001 Perna amp Vietri 2002)
Collapsars
bull Can make ldquolongrdquo GRBs in H stripped (WR) stars tengine gt tescape
bull Short bursts may be compact binary mergersbull Need SN failure amp angular momentum
ndash Low metallicity binary can help
bull Star can explode -gt SN if nickel is made Predicts GRBSN association Type Ibc
bull SNGRB ratio may depend on angular momentumbull ldquoNickel windrdquo can explode star -gt hypernova
ndash H env Type II (no GRB) no H Type I + GRB
GRBGW bull Long GRBs
ndash not brighter than SN in GW
ndash very far Gpc
ndash very rare lt 1 SN
bull Short GBsndash merging ns-bh binaries
ndash maybe closer than long bursts
ndash short delay between event and GRB
ndash good for SWIFTLIGO
Rates
bull SN 1s = 100000 day
bull GRB 1day (BATSE) = 1000day
bull GRB rate = 1 of SN rate
bull maybe more collapsars than GRBs
bull =gt more rapidly rotating SN
bull SN with collapsar engine
bull look for bright Type Ic (w broad lines)
SN GW
bull SN1998bwGRB980425
bull 40 Mpc
bull maybe dominant GRB
bull rapid rotaters
bull SNAPROTSE look for 1998bw 2003dh like SN
bull many light curves -gt better t_explode
Implications
bull Probe engine directly
bull collapse duration vs GRB duration
bull collapseGRB delay (internal vs external)
bull disk properties ndash low viscosity big disks
Issues
bull too much j =gt no GRB but bright GW
bull may need low metallicity for GRB
bull prefer high redshift
bull donrsquot know nearby rate
bull but 980425 may imply rate is high
bull look for weak GRBs like 980425
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
With decreasing metallicity the bindingenergy of the core and the size of the silicon core both increase making black hole formation more likely atlow metallicity Woosley Heger amp Weaver RMP (2002)
Black hole formation may be unavoidable for low metallicity
Solar metallicity
Low metallicity
In the absence of mass lossand magnetic fields there wouldbe abundant progenitors
Unfortunately nature has both
15 solar mass helium core born rotating rigidly at f times break up
The more difficult problem is the angular momentum Thisis a problem shared by all current GRB models that invokemassive stars
- What is a Gamma-Ray Burst
- Superbowl Burst
- Slide 3
- 135 models (1993)
- Slide 5
- Slide 6
- Slide 7
- GRB991121
- GRB030329SN2003DH
- Slide 10
- Slide 11
- Slide 12
- GRB central engine
- ldquoDelayedrdquo SN Explosion
- Pre-Supernova Density Structure
- Failure of delayed mechanism
- Stellar Rotation
- Slide 18
- Slide 19
- Collapsar Simulations
- Collapsar Disk Animation
- Disk Formation Movie
- Slide 23
- Slide 24
- Slide 25
- Collapsar results
- Slide 27
- Jet Birth
- Relativistic Jet Movie
- Collapsar stages
- Slide 31
- Slide 32
- Nickel Wind Movie
- Slide 34
- Slide 35
- Slide 36
- Slide 37
- Slide 38
- Collapsars
- GRBGW
- Rates
- SN GW
- Implications
- Issues
- Principle Results
- Slide 46
- Slide 47
-
Collapsar Simulations
bull pre-SN 15 Msun Helium starbull Newtonian Hydrodynamics (PPM)bull alpha viscositybull rotationbull photodisintegration (NSE alpha n p)bull neutrino cooling thermal + URCA optically thinbull Ideal nucleons radiation relativistic degenerate
electrons positionsbull 2D axisymmetric spherical gridbull self gravity pseudo-Newtonian (PW)bull Rin = 9 Rs Rout = 9000 Rs
MacFadyen amp Woosley (1999)
Collapsar Disk AnimationPPM hydrodynamics Paczynski-Witta potential EOS neutrino cooling nuclear reactions viscosity
Stellar collapse w rotation
Density structure No disk no wind
Note Accretion shock funnel clearing pole to equator density contrast fluctuating polar density
Initial model 15 Msun Helium (Wolf-Rayet) star evolved with mass loss
R= 8 x 108 cm
Show inner 1 in radius disk mass = 001 M_sun
Low viscosity =001
Disk Formation Movie
Accretion Shock
Disk formation
t = 75 s
PhotodisintegrationSiOC -gt free neutronsAnd protons Enhanced neutrino cooling
neutrino coolong allows
accretion
no cooling=gt
dynamically unstable
CDAF
Could emit GWs but
maybe no GRB
= 01 ltMgt = 007 Msun s = 13 x 1053 ergs
spin
mass
Use 1D neutrino cooled
ldquoslimrdquo disk models
from Popham et al (1999)
Collapsar results
bull Sustained accretion gt10sbull Sufficient energy bull Time scale set by He core collapsebull Disk-feeding time scale not disk-drainingbull Neutrino cooling allows accretionbull Neutrino annihilation energetically
possiblendash calculable in any case
Funnel geometry
channels any fireball
Density contrasts can
be huge
Ejet = f Maccc2
MHD
T = 57 ms
E = 5 x 1050 ergs
Edep = 28 x 1048 erg
Jet BirthThermal energy deposition focused by toroidal funnel structure
fmax ~ 06 - 4
Relativistic Jet Movie
Collapsar stages1 Iron core collapse disk formation
T~1010K ~108gcm-3 photodisintegration cooling pair capture disk is free nucleons (2 s)
2 Polar density declines to allow jet birthfrac12v3 Edep (2-5 s)
3 Jet tunnels out of star (5 s) Wolf-Rayet4 Jet powered for ~10 more seconds
Evacuates polar channel and reaches asymptotic speed (10 s)
T_GRB T_collapse
Jupiter
Red Supergiant
R~1013 cm
Blue Supergiant
R~1012 cm
Wolf-Rayet Star
R~1011 cm
Type Ib or Ic
Supernova
Supernovae
Ia
WD cosmology
Type II
Hydrogen
Type I
No Hydrogen
Ib Ic
exploding WR
thermonuclear old pop E galaxies
core collapse massive stars
Nickel Wind Movie
ldquoNickel Windrdquo
T gt 5 x 109 K
Fallback in weak SN explosions
Shock reaches
surface of star but parts of star are
not ejected to infinity
Fallback accretion Mms ~ 25 Msun Same star
exploded with a range of explosion energies
Significant accretion for thousands of
seconds ndash days
If fallback fuels a jet with power
fmc2
May power ldquohypernovardquo or long duration
GRBWeak
supernova shock
Shock breakout X-Ray transient
2 ldquoBriefrdquo jet tengine tjet
Engine dies before jet breakout
Mildly relativistic shock breakout
MacFadyen (1999)
What made SN1998bw+GRB980425
1 Accretion powered hypernova w Nickel wind
MacFadyen (2002)
E~ 1052 erg M(Ni)~05 M
GRB from ~3 shock breakout (Tan et al 2001 Perna amp Vietri 2002)
Collapsars
bull Can make ldquolongrdquo GRBs in H stripped (WR) stars tengine gt tescape
bull Short bursts may be compact binary mergersbull Need SN failure amp angular momentum
ndash Low metallicity binary can help
bull Star can explode -gt SN if nickel is made Predicts GRBSN association Type Ibc
bull SNGRB ratio may depend on angular momentumbull ldquoNickel windrdquo can explode star -gt hypernova
ndash H env Type II (no GRB) no H Type I + GRB
GRBGW bull Long GRBs
ndash not brighter than SN in GW
ndash very far Gpc
ndash very rare lt 1 SN
bull Short GBsndash merging ns-bh binaries
ndash maybe closer than long bursts
ndash short delay between event and GRB
ndash good for SWIFTLIGO
Rates
bull SN 1s = 100000 day
bull GRB 1day (BATSE) = 1000day
bull GRB rate = 1 of SN rate
bull maybe more collapsars than GRBs
bull =gt more rapidly rotating SN
bull SN with collapsar engine
bull look for bright Type Ic (w broad lines)
SN GW
bull SN1998bwGRB980425
bull 40 Mpc
bull maybe dominant GRB
bull rapid rotaters
bull SNAPROTSE look for 1998bw 2003dh like SN
bull many light curves -gt better t_explode
Implications
bull Probe engine directly
bull collapse duration vs GRB duration
bull collapseGRB delay (internal vs external)
bull disk properties ndash low viscosity big disks
Issues
bull too much j =gt no GRB but bright GW
bull may need low metallicity for GRB
bull prefer high redshift
bull donrsquot know nearby rate
bull but 980425 may imply rate is high
bull look for weak GRBs like 980425
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
With decreasing metallicity the bindingenergy of the core and the size of the silicon core both increase making black hole formation more likely atlow metallicity Woosley Heger amp Weaver RMP (2002)
Black hole formation may be unavoidable for low metallicity
Solar metallicity
Low metallicity
In the absence of mass lossand magnetic fields there wouldbe abundant progenitors
Unfortunately nature has both
15 solar mass helium core born rotating rigidly at f times break up
The more difficult problem is the angular momentum Thisis a problem shared by all current GRB models that invokemassive stars
- What is a Gamma-Ray Burst
- Superbowl Burst
- Slide 3
- 135 models (1993)
- Slide 5
- Slide 6
- Slide 7
- GRB991121
- GRB030329SN2003DH
- Slide 10
- Slide 11
- Slide 12
- GRB central engine
- ldquoDelayedrdquo SN Explosion
- Pre-Supernova Density Structure
- Failure of delayed mechanism
- Stellar Rotation
- Slide 18
- Slide 19
- Collapsar Simulations
- Collapsar Disk Animation
- Disk Formation Movie
- Slide 23
- Slide 24
- Slide 25
- Collapsar results
- Slide 27
- Jet Birth
- Relativistic Jet Movie
- Collapsar stages
- Slide 31
- Slide 32
- Nickel Wind Movie
- Slide 34
- Slide 35
- Slide 36
- Slide 37
- Slide 38
- Collapsars
- GRBGW
- Rates
- SN GW
- Implications
- Issues
- Principle Results
- Slide 46
- Slide 47
-
Collapsar Disk AnimationPPM hydrodynamics Paczynski-Witta potential EOS neutrino cooling nuclear reactions viscosity
Stellar collapse w rotation
Density structure No disk no wind
Note Accretion shock funnel clearing pole to equator density contrast fluctuating polar density
Initial model 15 Msun Helium (Wolf-Rayet) star evolved with mass loss
R= 8 x 108 cm
Show inner 1 in radius disk mass = 001 M_sun
Low viscosity =001
Disk Formation Movie
Accretion Shock
Disk formation
t = 75 s
PhotodisintegrationSiOC -gt free neutronsAnd protons Enhanced neutrino cooling
neutrino coolong allows
accretion
no cooling=gt
dynamically unstable
CDAF
Could emit GWs but
maybe no GRB
= 01 ltMgt = 007 Msun s = 13 x 1053 ergs
spin
mass
Use 1D neutrino cooled
ldquoslimrdquo disk models
from Popham et al (1999)
Collapsar results
bull Sustained accretion gt10sbull Sufficient energy bull Time scale set by He core collapsebull Disk-feeding time scale not disk-drainingbull Neutrino cooling allows accretionbull Neutrino annihilation energetically
possiblendash calculable in any case
Funnel geometry
channels any fireball
Density contrasts can
be huge
Ejet = f Maccc2
MHD
T = 57 ms
E = 5 x 1050 ergs
Edep = 28 x 1048 erg
Jet BirthThermal energy deposition focused by toroidal funnel structure
fmax ~ 06 - 4
Relativistic Jet Movie
Collapsar stages1 Iron core collapse disk formation
T~1010K ~108gcm-3 photodisintegration cooling pair capture disk is free nucleons (2 s)
2 Polar density declines to allow jet birthfrac12v3 Edep (2-5 s)
3 Jet tunnels out of star (5 s) Wolf-Rayet4 Jet powered for ~10 more seconds
Evacuates polar channel and reaches asymptotic speed (10 s)
T_GRB T_collapse
Jupiter
Red Supergiant
R~1013 cm
Blue Supergiant
R~1012 cm
Wolf-Rayet Star
R~1011 cm
Type Ib or Ic
Supernova
Supernovae
Ia
WD cosmology
Type II
Hydrogen
Type I
No Hydrogen
Ib Ic
exploding WR
thermonuclear old pop E galaxies
core collapse massive stars
Nickel Wind Movie
ldquoNickel Windrdquo
T gt 5 x 109 K
Fallback in weak SN explosions
Shock reaches
surface of star but parts of star are
not ejected to infinity
Fallback accretion Mms ~ 25 Msun Same star
exploded with a range of explosion energies
Significant accretion for thousands of
seconds ndash days
If fallback fuels a jet with power
fmc2
May power ldquohypernovardquo or long duration
GRBWeak
supernova shock
Shock breakout X-Ray transient
2 ldquoBriefrdquo jet tengine tjet
Engine dies before jet breakout
Mildly relativistic shock breakout
MacFadyen (1999)
What made SN1998bw+GRB980425
1 Accretion powered hypernova w Nickel wind
MacFadyen (2002)
E~ 1052 erg M(Ni)~05 M
GRB from ~3 shock breakout (Tan et al 2001 Perna amp Vietri 2002)
Collapsars
bull Can make ldquolongrdquo GRBs in H stripped (WR) stars tengine gt tescape
bull Short bursts may be compact binary mergersbull Need SN failure amp angular momentum
ndash Low metallicity binary can help
bull Star can explode -gt SN if nickel is made Predicts GRBSN association Type Ibc
bull SNGRB ratio may depend on angular momentumbull ldquoNickel windrdquo can explode star -gt hypernova
ndash H env Type II (no GRB) no H Type I + GRB
GRBGW bull Long GRBs
ndash not brighter than SN in GW
ndash very far Gpc
ndash very rare lt 1 SN
bull Short GBsndash merging ns-bh binaries
ndash maybe closer than long bursts
ndash short delay between event and GRB
ndash good for SWIFTLIGO
Rates
bull SN 1s = 100000 day
bull GRB 1day (BATSE) = 1000day
bull GRB rate = 1 of SN rate
bull maybe more collapsars than GRBs
bull =gt more rapidly rotating SN
bull SN with collapsar engine
bull look for bright Type Ic (w broad lines)
SN GW
bull SN1998bwGRB980425
bull 40 Mpc
bull maybe dominant GRB
bull rapid rotaters
bull SNAPROTSE look for 1998bw 2003dh like SN
bull many light curves -gt better t_explode
Implications
bull Probe engine directly
bull collapse duration vs GRB duration
bull collapseGRB delay (internal vs external)
bull disk properties ndash low viscosity big disks
Issues
bull too much j =gt no GRB but bright GW
bull may need low metallicity for GRB
bull prefer high redshift
bull donrsquot know nearby rate
bull but 980425 may imply rate is high
bull look for weak GRBs like 980425
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
With decreasing metallicity the bindingenergy of the core and the size of the silicon core both increase making black hole formation more likely atlow metallicity Woosley Heger amp Weaver RMP (2002)
Black hole formation may be unavoidable for low metallicity
Solar metallicity
Low metallicity
In the absence of mass lossand magnetic fields there wouldbe abundant progenitors
Unfortunately nature has both
15 solar mass helium core born rotating rigidly at f times break up
The more difficult problem is the angular momentum Thisis a problem shared by all current GRB models that invokemassive stars
- What is a Gamma-Ray Burst
- Superbowl Burst
- Slide 3
- 135 models (1993)
- Slide 5
- Slide 6
- Slide 7
- GRB991121
- GRB030329SN2003DH
- Slide 10
- Slide 11
- Slide 12
- GRB central engine
- ldquoDelayedrdquo SN Explosion
- Pre-Supernova Density Structure
- Failure of delayed mechanism
- Stellar Rotation
- Slide 18
- Slide 19
- Collapsar Simulations
- Collapsar Disk Animation
- Disk Formation Movie
- Slide 23
- Slide 24
- Slide 25
- Collapsar results
- Slide 27
- Jet Birth
- Relativistic Jet Movie
- Collapsar stages
- Slide 31
- Slide 32
- Nickel Wind Movie
- Slide 34
- Slide 35
- Slide 36
- Slide 37
- Slide 38
- Collapsars
- GRBGW
- Rates
- SN GW
- Implications
- Issues
- Principle Results
- Slide 46
- Slide 47
-
Disk Formation Movie
Accretion Shock
Disk formation
t = 75 s
PhotodisintegrationSiOC -gt free neutronsAnd protons Enhanced neutrino cooling
neutrino coolong allows
accretion
no cooling=gt
dynamically unstable
CDAF
Could emit GWs but
maybe no GRB
= 01 ltMgt = 007 Msun s = 13 x 1053 ergs
spin
mass
Use 1D neutrino cooled
ldquoslimrdquo disk models
from Popham et al (1999)
Collapsar results
bull Sustained accretion gt10sbull Sufficient energy bull Time scale set by He core collapsebull Disk-feeding time scale not disk-drainingbull Neutrino cooling allows accretionbull Neutrino annihilation energetically
possiblendash calculable in any case
Funnel geometry
channels any fireball
Density contrasts can
be huge
Ejet = f Maccc2
MHD
T = 57 ms
E = 5 x 1050 ergs
Edep = 28 x 1048 erg
Jet BirthThermal energy deposition focused by toroidal funnel structure
fmax ~ 06 - 4
Relativistic Jet Movie
Collapsar stages1 Iron core collapse disk formation
T~1010K ~108gcm-3 photodisintegration cooling pair capture disk is free nucleons (2 s)
2 Polar density declines to allow jet birthfrac12v3 Edep (2-5 s)
3 Jet tunnels out of star (5 s) Wolf-Rayet4 Jet powered for ~10 more seconds
Evacuates polar channel and reaches asymptotic speed (10 s)
T_GRB T_collapse
Jupiter
Red Supergiant
R~1013 cm
Blue Supergiant
R~1012 cm
Wolf-Rayet Star
R~1011 cm
Type Ib or Ic
Supernova
Supernovae
Ia
WD cosmology
Type II
Hydrogen
Type I
No Hydrogen
Ib Ic
exploding WR
thermonuclear old pop E galaxies
core collapse massive stars
Nickel Wind Movie
ldquoNickel Windrdquo
T gt 5 x 109 K
Fallback in weak SN explosions
Shock reaches
surface of star but parts of star are
not ejected to infinity
Fallback accretion Mms ~ 25 Msun Same star
exploded with a range of explosion energies
Significant accretion for thousands of
seconds ndash days
If fallback fuels a jet with power
fmc2
May power ldquohypernovardquo or long duration
GRBWeak
supernova shock
Shock breakout X-Ray transient
2 ldquoBriefrdquo jet tengine tjet
Engine dies before jet breakout
Mildly relativistic shock breakout
MacFadyen (1999)
What made SN1998bw+GRB980425
1 Accretion powered hypernova w Nickel wind
MacFadyen (2002)
E~ 1052 erg M(Ni)~05 M
GRB from ~3 shock breakout (Tan et al 2001 Perna amp Vietri 2002)
Collapsars
bull Can make ldquolongrdquo GRBs in H stripped (WR) stars tengine gt tescape
bull Short bursts may be compact binary mergersbull Need SN failure amp angular momentum
ndash Low metallicity binary can help
bull Star can explode -gt SN if nickel is made Predicts GRBSN association Type Ibc
bull SNGRB ratio may depend on angular momentumbull ldquoNickel windrdquo can explode star -gt hypernova
ndash H env Type II (no GRB) no H Type I + GRB
GRBGW bull Long GRBs
ndash not brighter than SN in GW
ndash very far Gpc
ndash very rare lt 1 SN
bull Short GBsndash merging ns-bh binaries
ndash maybe closer than long bursts
ndash short delay between event and GRB
ndash good for SWIFTLIGO
Rates
bull SN 1s = 100000 day
bull GRB 1day (BATSE) = 1000day
bull GRB rate = 1 of SN rate
bull maybe more collapsars than GRBs
bull =gt more rapidly rotating SN
bull SN with collapsar engine
bull look for bright Type Ic (w broad lines)
SN GW
bull SN1998bwGRB980425
bull 40 Mpc
bull maybe dominant GRB
bull rapid rotaters
bull SNAPROTSE look for 1998bw 2003dh like SN
bull many light curves -gt better t_explode
Implications
bull Probe engine directly
bull collapse duration vs GRB duration
bull collapseGRB delay (internal vs external)
bull disk properties ndash low viscosity big disks
Issues
bull too much j =gt no GRB but bright GW
bull may need low metallicity for GRB
bull prefer high redshift
bull donrsquot know nearby rate
bull but 980425 may imply rate is high
bull look for weak GRBs like 980425
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
With decreasing metallicity the bindingenergy of the core and the size of the silicon core both increase making black hole formation more likely atlow metallicity Woosley Heger amp Weaver RMP (2002)
Black hole formation may be unavoidable for low metallicity
Solar metallicity
Low metallicity
In the absence of mass lossand magnetic fields there wouldbe abundant progenitors
Unfortunately nature has both
15 solar mass helium core born rotating rigidly at f times break up
The more difficult problem is the angular momentum Thisis a problem shared by all current GRB models that invokemassive stars
- What is a Gamma-Ray Burst
- Superbowl Burst
- Slide 3
- 135 models (1993)
- Slide 5
- Slide 6
- Slide 7
- GRB991121
- GRB030329SN2003DH
- Slide 10
- Slide 11
- Slide 12
- GRB central engine
- ldquoDelayedrdquo SN Explosion
- Pre-Supernova Density Structure
- Failure of delayed mechanism
- Stellar Rotation
- Slide 18
- Slide 19
- Collapsar Simulations
- Collapsar Disk Animation
- Disk Formation Movie
- Slide 23
- Slide 24
- Slide 25
- Collapsar results
- Slide 27
- Jet Birth
- Relativistic Jet Movie
- Collapsar stages
- Slide 31
- Slide 32
- Nickel Wind Movie
- Slide 34
- Slide 35
- Slide 36
- Slide 37
- Slide 38
- Collapsars
- GRBGW
- Rates
- SN GW
- Implications
- Issues
- Principle Results
- Slide 46
- Slide 47
-
Accretion Shock
Disk formation
t = 75 s
PhotodisintegrationSiOC -gt free neutronsAnd protons Enhanced neutrino cooling
neutrino coolong allows
accretion
no cooling=gt
dynamically unstable
CDAF
Could emit GWs but
maybe no GRB
= 01 ltMgt = 007 Msun s = 13 x 1053 ergs
spin
mass
Use 1D neutrino cooled
ldquoslimrdquo disk models
from Popham et al (1999)
Collapsar results
bull Sustained accretion gt10sbull Sufficient energy bull Time scale set by He core collapsebull Disk-feeding time scale not disk-drainingbull Neutrino cooling allows accretionbull Neutrino annihilation energetically
possiblendash calculable in any case
Funnel geometry
channels any fireball
Density contrasts can
be huge
Ejet = f Maccc2
MHD
T = 57 ms
E = 5 x 1050 ergs
Edep = 28 x 1048 erg
Jet BirthThermal energy deposition focused by toroidal funnel structure
fmax ~ 06 - 4
Relativistic Jet Movie
Collapsar stages1 Iron core collapse disk formation
T~1010K ~108gcm-3 photodisintegration cooling pair capture disk is free nucleons (2 s)
2 Polar density declines to allow jet birthfrac12v3 Edep (2-5 s)
3 Jet tunnels out of star (5 s) Wolf-Rayet4 Jet powered for ~10 more seconds
Evacuates polar channel and reaches asymptotic speed (10 s)
T_GRB T_collapse
Jupiter
Red Supergiant
R~1013 cm
Blue Supergiant
R~1012 cm
Wolf-Rayet Star
R~1011 cm
Type Ib or Ic
Supernova
Supernovae
Ia
WD cosmology
Type II
Hydrogen
Type I
No Hydrogen
Ib Ic
exploding WR
thermonuclear old pop E galaxies
core collapse massive stars
Nickel Wind Movie
ldquoNickel Windrdquo
T gt 5 x 109 K
Fallback in weak SN explosions
Shock reaches
surface of star but parts of star are
not ejected to infinity
Fallback accretion Mms ~ 25 Msun Same star
exploded with a range of explosion energies
Significant accretion for thousands of
seconds ndash days
If fallback fuels a jet with power
fmc2
May power ldquohypernovardquo or long duration
GRBWeak
supernova shock
Shock breakout X-Ray transient
2 ldquoBriefrdquo jet tengine tjet
Engine dies before jet breakout
Mildly relativistic shock breakout
MacFadyen (1999)
What made SN1998bw+GRB980425
1 Accretion powered hypernova w Nickel wind
MacFadyen (2002)
E~ 1052 erg M(Ni)~05 M
GRB from ~3 shock breakout (Tan et al 2001 Perna amp Vietri 2002)
Collapsars
bull Can make ldquolongrdquo GRBs in H stripped (WR) stars tengine gt tescape
bull Short bursts may be compact binary mergersbull Need SN failure amp angular momentum
ndash Low metallicity binary can help
bull Star can explode -gt SN if nickel is made Predicts GRBSN association Type Ibc
bull SNGRB ratio may depend on angular momentumbull ldquoNickel windrdquo can explode star -gt hypernova
ndash H env Type II (no GRB) no H Type I + GRB
GRBGW bull Long GRBs
ndash not brighter than SN in GW
ndash very far Gpc
ndash very rare lt 1 SN
bull Short GBsndash merging ns-bh binaries
ndash maybe closer than long bursts
ndash short delay between event and GRB
ndash good for SWIFTLIGO
Rates
bull SN 1s = 100000 day
bull GRB 1day (BATSE) = 1000day
bull GRB rate = 1 of SN rate
bull maybe more collapsars than GRBs
bull =gt more rapidly rotating SN
bull SN with collapsar engine
bull look for bright Type Ic (w broad lines)
SN GW
bull SN1998bwGRB980425
bull 40 Mpc
bull maybe dominant GRB
bull rapid rotaters
bull SNAPROTSE look for 1998bw 2003dh like SN
bull many light curves -gt better t_explode
Implications
bull Probe engine directly
bull collapse duration vs GRB duration
bull collapseGRB delay (internal vs external)
bull disk properties ndash low viscosity big disks
Issues
bull too much j =gt no GRB but bright GW
bull may need low metallicity for GRB
bull prefer high redshift
bull donrsquot know nearby rate
bull but 980425 may imply rate is high
bull look for weak GRBs like 980425
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
With decreasing metallicity the bindingenergy of the core and the size of the silicon core both increase making black hole formation more likely atlow metallicity Woosley Heger amp Weaver RMP (2002)
Black hole formation may be unavoidable for low metallicity
Solar metallicity
Low metallicity
In the absence of mass lossand magnetic fields there wouldbe abundant progenitors
Unfortunately nature has both
15 solar mass helium core born rotating rigidly at f times break up
The more difficult problem is the angular momentum Thisis a problem shared by all current GRB models that invokemassive stars
- What is a Gamma-Ray Burst
- Superbowl Burst
- Slide 3
- 135 models (1993)
- Slide 5
- Slide 6
- Slide 7
- GRB991121
- GRB030329SN2003DH
- Slide 10
- Slide 11
- Slide 12
- GRB central engine
- ldquoDelayedrdquo SN Explosion
- Pre-Supernova Density Structure
- Failure of delayed mechanism
- Stellar Rotation
- Slide 18
- Slide 19
- Collapsar Simulations
- Collapsar Disk Animation
- Disk Formation Movie
- Slide 23
- Slide 24
- Slide 25
- Collapsar results
- Slide 27
- Jet Birth
- Relativistic Jet Movie
- Collapsar stages
- Slide 31
- Slide 32
- Nickel Wind Movie
- Slide 34
- Slide 35
- Slide 36
- Slide 37
- Slide 38
- Collapsars
- GRBGW
- Rates
- SN GW
- Implications
- Issues
- Principle Results
- Slide 46
- Slide 47
-
= 01 ltMgt = 007 Msun s = 13 x 1053 ergs
spin
mass
Use 1D neutrino cooled
ldquoslimrdquo disk models
from Popham et al (1999)
Collapsar results
bull Sustained accretion gt10sbull Sufficient energy bull Time scale set by He core collapsebull Disk-feeding time scale not disk-drainingbull Neutrino cooling allows accretionbull Neutrino annihilation energetically
possiblendash calculable in any case
Funnel geometry
channels any fireball
Density contrasts can
be huge
Ejet = f Maccc2
MHD
T = 57 ms
E = 5 x 1050 ergs
Edep = 28 x 1048 erg
Jet BirthThermal energy deposition focused by toroidal funnel structure
fmax ~ 06 - 4
Relativistic Jet Movie
Collapsar stages1 Iron core collapse disk formation
T~1010K ~108gcm-3 photodisintegration cooling pair capture disk is free nucleons (2 s)
2 Polar density declines to allow jet birthfrac12v3 Edep (2-5 s)
3 Jet tunnels out of star (5 s) Wolf-Rayet4 Jet powered for ~10 more seconds
Evacuates polar channel and reaches asymptotic speed (10 s)
T_GRB T_collapse
Jupiter
Red Supergiant
R~1013 cm
Blue Supergiant
R~1012 cm
Wolf-Rayet Star
R~1011 cm
Type Ib or Ic
Supernova
Supernovae
Ia
WD cosmology
Type II
Hydrogen
Type I
No Hydrogen
Ib Ic
exploding WR
thermonuclear old pop E galaxies
core collapse massive stars
Nickel Wind Movie
ldquoNickel Windrdquo
T gt 5 x 109 K
Fallback in weak SN explosions
Shock reaches
surface of star but parts of star are
not ejected to infinity
Fallback accretion Mms ~ 25 Msun Same star
exploded with a range of explosion energies
Significant accretion for thousands of
seconds ndash days
If fallback fuels a jet with power
fmc2
May power ldquohypernovardquo or long duration
GRBWeak
supernova shock
Shock breakout X-Ray transient
2 ldquoBriefrdquo jet tengine tjet
Engine dies before jet breakout
Mildly relativistic shock breakout
MacFadyen (1999)
What made SN1998bw+GRB980425
1 Accretion powered hypernova w Nickel wind
MacFadyen (2002)
E~ 1052 erg M(Ni)~05 M
GRB from ~3 shock breakout (Tan et al 2001 Perna amp Vietri 2002)
Collapsars
bull Can make ldquolongrdquo GRBs in H stripped (WR) stars tengine gt tescape
bull Short bursts may be compact binary mergersbull Need SN failure amp angular momentum
ndash Low metallicity binary can help
bull Star can explode -gt SN if nickel is made Predicts GRBSN association Type Ibc
bull SNGRB ratio may depend on angular momentumbull ldquoNickel windrdquo can explode star -gt hypernova
ndash H env Type II (no GRB) no H Type I + GRB
GRBGW bull Long GRBs
ndash not brighter than SN in GW
ndash very far Gpc
ndash very rare lt 1 SN
bull Short GBsndash merging ns-bh binaries
ndash maybe closer than long bursts
ndash short delay between event and GRB
ndash good for SWIFTLIGO
Rates
bull SN 1s = 100000 day
bull GRB 1day (BATSE) = 1000day
bull GRB rate = 1 of SN rate
bull maybe more collapsars than GRBs
bull =gt more rapidly rotating SN
bull SN with collapsar engine
bull look for bright Type Ic (w broad lines)
SN GW
bull SN1998bwGRB980425
bull 40 Mpc
bull maybe dominant GRB
bull rapid rotaters
bull SNAPROTSE look for 1998bw 2003dh like SN
bull many light curves -gt better t_explode
Implications
bull Probe engine directly
bull collapse duration vs GRB duration
bull collapseGRB delay (internal vs external)
bull disk properties ndash low viscosity big disks
Issues
bull too much j =gt no GRB but bright GW
bull may need low metallicity for GRB
bull prefer high redshift
bull donrsquot know nearby rate
bull but 980425 may imply rate is high
bull look for weak GRBs like 980425
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
With decreasing metallicity the bindingenergy of the core and the size of the silicon core both increase making black hole formation more likely atlow metallicity Woosley Heger amp Weaver RMP (2002)
Black hole formation may be unavoidable for low metallicity
Solar metallicity
Low metallicity
In the absence of mass lossand magnetic fields there wouldbe abundant progenitors
Unfortunately nature has both
15 solar mass helium core born rotating rigidly at f times break up
The more difficult problem is the angular momentum Thisis a problem shared by all current GRB models that invokemassive stars
- What is a Gamma-Ray Burst
- Superbowl Burst
- Slide 3
- 135 models (1993)
- Slide 5
- Slide 6
- Slide 7
- GRB991121
- GRB030329SN2003DH
- Slide 10
- Slide 11
- Slide 12
- GRB central engine
- ldquoDelayedrdquo SN Explosion
- Pre-Supernova Density Structure
- Failure of delayed mechanism
- Stellar Rotation
- Slide 18
- Slide 19
- Collapsar Simulations
- Collapsar Disk Animation
- Disk Formation Movie
- Slide 23
- Slide 24
- Slide 25
- Collapsar results
- Slide 27
- Jet Birth
- Relativistic Jet Movie
- Collapsar stages
- Slide 31
- Slide 32
- Nickel Wind Movie
- Slide 34
- Slide 35
- Slide 36
- Slide 37
- Slide 38
- Collapsars
- GRBGW
- Rates
- SN GW
- Implications
- Issues
- Principle Results
- Slide 46
- Slide 47
-
spin
mass
Use 1D neutrino cooled
ldquoslimrdquo disk models
from Popham et al (1999)
Collapsar results
bull Sustained accretion gt10sbull Sufficient energy bull Time scale set by He core collapsebull Disk-feeding time scale not disk-drainingbull Neutrino cooling allows accretionbull Neutrino annihilation energetically
possiblendash calculable in any case
Funnel geometry
channels any fireball
Density contrasts can
be huge
Ejet = f Maccc2
MHD
T = 57 ms
E = 5 x 1050 ergs
Edep = 28 x 1048 erg
Jet BirthThermal energy deposition focused by toroidal funnel structure
fmax ~ 06 - 4
Relativistic Jet Movie
Collapsar stages1 Iron core collapse disk formation
T~1010K ~108gcm-3 photodisintegration cooling pair capture disk is free nucleons (2 s)
2 Polar density declines to allow jet birthfrac12v3 Edep (2-5 s)
3 Jet tunnels out of star (5 s) Wolf-Rayet4 Jet powered for ~10 more seconds
Evacuates polar channel and reaches asymptotic speed (10 s)
T_GRB T_collapse
Jupiter
Red Supergiant
R~1013 cm
Blue Supergiant
R~1012 cm
Wolf-Rayet Star
R~1011 cm
Type Ib or Ic
Supernova
Supernovae
Ia
WD cosmology
Type II
Hydrogen
Type I
No Hydrogen
Ib Ic
exploding WR
thermonuclear old pop E galaxies
core collapse massive stars
Nickel Wind Movie
ldquoNickel Windrdquo
T gt 5 x 109 K
Fallback in weak SN explosions
Shock reaches
surface of star but parts of star are
not ejected to infinity
Fallback accretion Mms ~ 25 Msun Same star
exploded with a range of explosion energies
Significant accretion for thousands of
seconds ndash days
If fallback fuels a jet with power
fmc2
May power ldquohypernovardquo or long duration
GRBWeak
supernova shock
Shock breakout X-Ray transient
2 ldquoBriefrdquo jet tengine tjet
Engine dies before jet breakout
Mildly relativistic shock breakout
MacFadyen (1999)
What made SN1998bw+GRB980425
1 Accretion powered hypernova w Nickel wind
MacFadyen (2002)
E~ 1052 erg M(Ni)~05 M
GRB from ~3 shock breakout (Tan et al 2001 Perna amp Vietri 2002)
Collapsars
bull Can make ldquolongrdquo GRBs in H stripped (WR) stars tengine gt tescape
bull Short bursts may be compact binary mergersbull Need SN failure amp angular momentum
ndash Low metallicity binary can help
bull Star can explode -gt SN if nickel is made Predicts GRBSN association Type Ibc
bull SNGRB ratio may depend on angular momentumbull ldquoNickel windrdquo can explode star -gt hypernova
ndash H env Type II (no GRB) no H Type I + GRB
GRBGW bull Long GRBs
ndash not brighter than SN in GW
ndash very far Gpc
ndash very rare lt 1 SN
bull Short GBsndash merging ns-bh binaries
ndash maybe closer than long bursts
ndash short delay between event and GRB
ndash good for SWIFTLIGO
Rates
bull SN 1s = 100000 day
bull GRB 1day (BATSE) = 1000day
bull GRB rate = 1 of SN rate
bull maybe more collapsars than GRBs
bull =gt more rapidly rotating SN
bull SN with collapsar engine
bull look for bright Type Ic (w broad lines)
SN GW
bull SN1998bwGRB980425
bull 40 Mpc
bull maybe dominant GRB
bull rapid rotaters
bull SNAPROTSE look for 1998bw 2003dh like SN
bull many light curves -gt better t_explode
Implications
bull Probe engine directly
bull collapse duration vs GRB duration
bull collapseGRB delay (internal vs external)
bull disk properties ndash low viscosity big disks
Issues
bull too much j =gt no GRB but bright GW
bull may need low metallicity for GRB
bull prefer high redshift
bull donrsquot know nearby rate
bull but 980425 may imply rate is high
bull look for weak GRBs like 980425
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
With decreasing metallicity the bindingenergy of the core and the size of the silicon core both increase making black hole formation more likely atlow metallicity Woosley Heger amp Weaver RMP (2002)
Black hole formation may be unavoidable for low metallicity
Solar metallicity
Low metallicity
In the absence of mass lossand magnetic fields there wouldbe abundant progenitors
Unfortunately nature has both
15 solar mass helium core born rotating rigidly at f times break up
The more difficult problem is the angular momentum Thisis a problem shared by all current GRB models that invokemassive stars
- What is a Gamma-Ray Burst
- Superbowl Burst
- Slide 3
- 135 models (1993)
- Slide 5
- Slide 6
- Slide 7
- GRB991121
- GRB030329SN2003DH
- Slide 10
- Slide 11
- Slide 12
- GRB central engine
- ldquoDelayedrdquo SN Explosion
- Pre-Supernova Density Structure
- Failure of delayed mechanism
- Stellar Rotation
- Slide 18
- Slide 19
- Collapsar Simulations
- Collapsar Disk Animation
- Disk Formation Movie
- Slide 23
- Slide 24
- Slide 25
- Collapsar results
- Slide 27
- Jet Birth
- Relativistic Jet Movie
- Collapsar stages
- Slide 31
- Slide 32
- Nickel Wind Movie
- Slide 34
- Slide 35
- Slide 36
- Slide 37
- Slide 38
- Collapsars
- GRBGW
- Rates
- SN GW
- Implications
- Issues
- Principle Results
- Slide 46
- Slide 47
-
Collapsar results
bull Sustained accretion gt10sbull Sufficient energy bull Time scale set by He core collapsebull Disk-feeding time scale not disk-drainingbull Neutrino cooling allows accretionbull Neutrino annihilation energetically
possiblendash calculable in any case
Funnel geometry
channels any fireball
Density contrasts can
be huge
Ejet = f Maccc2
MHD
T = 57 ms
E = 5 x 1050 ergs
Edep = 28 x 1048 erg
Jet BirthThermal energy deposition focused by toroidal funnel structure
fmax ~ 06 - 4
Relativistic Jet Movie
Collapsar stages1 Iron core collapse disk formation
T~1010K ~108gcm-3 photodisintegration cooling pair capture disk is free nucleons (2 s)
2 Polar density declines to allow jet birthfrac12v3 Edep (2-5 s)
3 Jet tunnels out of star (5 s) Wolf-Rayet4 Jet powered for ~10 more seconds
Evacuates polar channel and reaches asymptotic speed (10 s)
T_GRB T_collapse
Jupiter
Red Supergiant
R~1013 cm
Blue Supergiant
R~1012 cm
Wolf-Rayet Star
R~1011 cm
Type Ib or Ic
Supernova
Supernovae
Ia
WD cosmology
Type II
Hydrogen
Type I
No Hydrogen
Ib Ic
exploding WR
thermonuclear old pop E galaxies
core collapse massive stars
Nickel Wind Movie
ldquoNickel Windrdquo
T gt 5 x 109 K
Fallback in weak SN explosions
Shock reaches
surface of star but parts of star are
not ejected to infinity
Fallback accretion Mms ~ 25 Msun Same star
exploded with a range of explosion energies
Significant accretion for thousands of
seconds ndash days
If fallback fuels a jet with power
fmc2
May power ldquohypernovardquo or long duration
GRBWeak
supernova shock
Shock breakout X-Ray transient
2 ldquoBriefrdquo jet tengine tjet
Engine dies before jet breakout
Mildly relativistic shock breakout
MacFadyen (1999)
What made SN1998bw+GRB980425
1 Accretion powered hypernova w Nickel wind
MacFadyen (2002)
E~ 1052 erg M(Ni)~05 M
GRB from ~3 shock breakout (Tan et al 2001 Perna amp Vietri 2002)
Collapsars
bull Can make ldquolongrdquo GRBs in H stripped (WR) stars tengine gt tescape
bull Short bursts may be compact binary mergersbull Need SN failure amp angular momentum
ndash Low metallicity binary can help
bull Star can explode -gt SN if nickel is made Predicts GRBSN association Type Ibc
bull SNGRB ratio may depend on angular momentumbull ldquoNickel windrdquo can explode star -gt hypernova
ndash H env Type II (no GRB) no H Type I + GRB
GRBGW bull Long GRBs
ndash not brighter than SN in GW
ndash very far Gpc
ndash very rare lt 1 SN
bull Short GBsndash merging ns-bh binaries
ndash maybe closer than long bursts
ndash short delay between event and GRB
ndash good for SWIFTLIGO
Rates
bull SN 1s = 100000 day
bull GRB 1day (BATSE) = 1000day
bull GRB rate = 1 of SN rate
bull maybe more collapsars than GRBs
bull =gt more rapidly rotating SN
bull SN with collapsar engine
bull look for bright Type Ic (w broad lines)
SN GW
bull SN1998bwGRB980425
bull 40 Mpc
bull maybe dominant GRB
bull rapid rotaters
bull SNAPROTSE look for 1998bw 2003dh like SN
bull many light curves -gt better t_explode
Implications
bull Probe engine directly
bull collapse duration vs GRB duration
bull collapseGRB delay (internal vs external)
bull disk properties ndash low viscosity big disks
Issues
bull too much j =gt no GRB but bright GW
bull may need low metallicity for GRB
bull prefer high redshift
bull donrsquot know nearby rate
bull but 980425 may imply rate is high
bull look for weak GRBs like 980425
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
With decreasing metallicity the bindingenergy of the core and the size of the silicon core both increase making black hole formation more likely atlow metallicity Woosley Heger amp Weaver RMP (2002)
Black hole formation may be unavoidable for low metallicity
Solar metallicity
Low metallicity
In the absence of mass lossand magnetic fields there wouldbe abundant progenitors
Unfortunately nature has both
15 solar mass helium core born rotating rigidly at f times break up
The more difficult problem is the angular momentum Thisis a problem shared by all current GRB models that invokemassive stars
- What is a Gamma-Ray Burst
- Superbowl Burst
- Slide 3
- 135 models (1993)
- Slide 5
- Slide 6
- Slide 7
- GRB991121
- GRB030329SN2003DH
- Slide 10
- Slide 11
- Slide 12
- GRB central engine
- ldquoDelayedrdquo SN Explosion
- Pre-Supernova Density Structure
- Failure of delayed mechanism
- Stellar Rotation
- Slide 18
- Slide 19
- Collapsar Simulations
- Collapsar Disk Animation
- Disk Formation Movie
- Slide 23
- Slide 24
- Slide 25
- Collapsar results
- Slide 27
- Jet Birth
- Relativistic Jet Movie
- Collapsar stages
- Slide 31
- Slide 32
- Nickel Wind Movie
- Slide 34
- Slide 35
- Slide 36
- Slide 37
- Slide 38
- Collapsars
- GRBGW
- Rates
- SN GW
- Implications
- Issues
- Principle Results
- Slide 46
- Slide 47
-
Funnel geometry
channels any fireball
Density contrasts can
be huge
Ejet = f Maccc2
MHD
T = 57 ms
E = 5 x 1050 ergs
Edep = 28 x 1048 erg
Jet BirthThermal energy deposition focused by toroidal funnel structure
fmax ~ 06 - 4
Relativistic Jet Movie
Collapsar stages1 Iron core collapse disk formation
T~1010K ~108gcm-3 photodisintegration cooling pair capture disk is free nucleons (2 s)
2 Polar density declines to allow jet birthfrac12v3 Edep (2-5 s)
3 Jet tunnels out of star (5 s) Wolf-Rayet4 Jet powered for ~10 more seconds
Evacuates polar channel and reaches asymptotic speed (10 s)
T_GRB T_collapse
Jupiter
Red Supergiant
R~1013 cm
Blue Supergiant
R~1012 cm
Wolf-Rayet Star
R~1011 cm
Type Ib or Ic
Supernova
Supernovae
Ia
WD cosmology
Type II
Hydrogen
Type I
No Hydrogen
Ib Ic
exploding WR
thermonuclear old pop E galaxies
core collapse massive stars
Nickel Wind Movie
ldquoNickel Windrdquo
T gt 5 x 109 K
Fallback in weak SN explosions
Shock reaches
surface of star but parts of star are
not ejected to infinity
Fallback accretion Mms ~ 25 Msun Same star
exploded with a range of explosion energies
Significant accretion for thousands of
seconds ndash days
If fallback fuels a jet with power
fmc2
May power ldquohypernovardquo or long duration
GRBWeak
supernova shock
Shock breakout X-Ray transient
2 ldquoBriefrdquo jet tengine tjet
Engine dies before jet breakout
Mildly relativistic shock breakout
MacFadyen (1999)
What made SN1998bw+GRB980425
1 Accretion powered hypernova w Nickel wind
MacFadyen (2002)
E~ 1052 erg M(Ni)~05 M
GRB from ~3 shock breakout (Tan et al 2001 Perna amp Vietri 2002)
Collapsars
bull Can make ldquolongrdquo GRBs in H stripped (WR) stars tengine gt tescape
bull Short bursts may be compact binary mergersbull Need SN failure amp angular momentum
ndash Low metallicity binary can help
bull Star can explode -gt SN if nickel is made Predicts GRBSN association Type Ibc
bull SNGRB ratio may depend on angular momentumbull ldquoNickel windrdquo can explode star -gt hypernova
ndash H env Type II (no GRB) no H Type I + GRB
GRBGW bull Long GRBs
ndash not brighter than SN in GW
ndash very far Gpc
ndash very rare lt 1 SN
bull Short GBsndash merging ns-bh binaries
ndash maybe closer than long bursts
ndash short delay between event and GRB
ndash good for SWIFTLIGO
Rates
bull SN 1s = 100000 day
bull GRB 1day (BATSE) = 1000day
bull GRB rate = 1 of SN rate
bull maybe more collapsars than GRBs
bull =gt more rapidly rotating SN
bull SN with collapsar engine
bull look for bright Type Ic (w broad lines)
SN GW
bull SN1998bwGRB980425
bull 40 Mpc
bull maybe dominant GRB
bull rapid rotaters
bull SNAPROTSE look for 1998bw 2003dh like SN
bull many light curves -gt better t_explode
Implications
bull Probe engine directly
bull collapse duration vs GRB duration
bull collapseGRB delay (internal vs external)
bull disk properties ndash low viscosity big disks
Issues
bull too much j =gt no GRB but bright GW
bull may need low metallicity for GRB
bull prefer high redshift
bull donrsquot know nearby rate
bull but 980425 may imply rate is high
bull look for weak GRBs like 980425
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
With decreasing metallicity the bindingenergy of the core and the size of the silicon core both increase making black hole formation more likely atlow metallicity Woosley Heger amp Weaver RMP (2002)
Black hole formation may be unavoidable for low metallicity
Solar metallicity
Low metallicity
In the absence of mass lossand magnetic fields there wouldbe abundant progenitors
Unfortunately nature has both
15 solar mass helium core born rotating rigidly at f times break up
The more difficult problem is the angular momentum Thisis a problem shared by all current GRB models that invokemassive stars
- What is a Gamma-Ray Burst
- Superbowl Burst
- Slide 3
- 135 models (1993)
- Slide 5
- Slide 6
- Slide 7
- GRB991121
- GRB030329SN2003DH
- Slide 10
- Slide 11
- Slide 12
- GRB central engine
- ldquoDelayedrdquo SN Explosion
- Pre-Supernova Density Structure
- Failure of delayed mechanism
- Stellar Rotation
- Slide 18
- Slide 19
- Collapsar Simulations
- Collapsar Disk Animation
- Disk Formation Movie
- Slide 23
- Slide 24
- Slide 25
- Collapsar results
- Slide 27
- Jet Birth
- Relativistic Jet Movie
- Collapsar stages
- Slide 31
- Slide 32
- Nickel Wind Movie
- Slide 34
- Slide 35
- Slide 36
- Slide 37
- Slide 38
- Collapsars
- GRBGW
- Rates
- SN GW
- Implications
- Issues
- Principle Results
- Slide 46
- Slide 47
-
Ejet = f Maccc2
MHD
T = 57 ms
E = 5 x 1050 ergs
Edep = 28 x 1048 erg
Jet BirthThermal energy deposition focused by toroidal funnel structure
fmax ~ 06 - 4
Relativistic Jet Movie
Collapsar stages1 Iron core collapse disk formation
T~1010K ~108gcm-3 photodisintegration cooling pair capture disk is free nucleons (2 s)
2 Polar density declines to allow jet birthfrac12v3 Edep (2-5 s)
3 Jet tunnels out of star (5 s) Wolf-Rayet4 Jet powered for ~10 more seconds
Evacuates polar channel and reaches asymptotic speed (10 s)
T_GRB T_collapse
Jupiter
Red Supergiant
R~1013 cm
Blue Supergiant
R~1012 cm
Wolf-Rayet Star
R~1011 cm
Type Ib or Ic
Supernova
Supernovae
Ia
WD cosmology
Type II
Hydrogen
Type I
No Hydrogen
Ib Ic
exploding WR
thermonuclear old pop E galaxies
core collapse massive stars
Nickel Wind Movie
ldquoNickel Windrdquo
T gt 5 x 109 K
Fallback in weak SN explosions
Shock reaches
surface of star but parts of star are
not ejected to infinity
Fallback accretion Mms ~ 25 Msun Same star
exploded with a range of explosion energies
Significant accretion for thousands of
seconds ndash days
If fallback fuels a jet with power
fmc2
May power ldquohypernovardquo or long duration
GRBWeak
supernova shock
Shock breakout X-Ray transient
2 ldquoBriefrdquo jet tengine tjet
Engine dies before jet breakout
Mildly relativistic shock breakout
MacFadyen (1999)
What made SN1998bw+GRB980425
1 Accretion powered hypernova w Nickel wind
MacFadyen (2002)
E~ 1052 erg M(Ni)~05 M
GRB from ~3 shock breakout (Tan et al 2001 Perna amp Vietri 2002)
Collapsars
bull Can make ldquolongrdquo GRBs in H stripped (WR) stars tengine gt tescape
bull Short bursts may be compact binary mergersbull Need SN failure amp angular momentum
ndash Low metallicity binary can help
bull Star can explode -gt SN if nickel is made Predicts GRBSN association Type Ibc
bull SNGRB ratio may depend on angular momentumbull ldquoNickel windrdquo can explode star -gt hypernova
ndash H env Type II (no GRB) no H Type I + GRB
GRBGW bull Long GRBs
ndash not brighter than SN in GW
ndash very far Gpc
ndash very rare lt 1 SN
bull Short GBsndash merging ns-bh binaries
ndash maybe closer than long bursts
ndash short delay between event and GRB
ndash good for SWIFTLIGO
Rates
bull SN 1s = 100000 day
bull GRB 1day (BATSE) = 1000day
bull GRB rate = 1 of SN rate
bull maybe more collapsars than GRBs
bull =gt more rapidly rotating SN
bull SN with collapsar engine
bull look for bright Type Ic (w broad lines)
SN GW
bull SN1998bwGRB980425
bull 40 Mpc
bull maybe dominant GRB
bull rapid rotaters
bull SNAPROTSE look for 1998bw 2003dh like SN
bull many light curves -gt better t_explode
Implications
bull Probe engine directly
bull collapse duration vs GRB duration
bull collapseGRB delay (internal vs external)
bull disk properties ndash low viscosity big disks
Issues
bull too much j =gt no GRB but bright GW
bull may need low metallicity for GRB
bull prefer high redshift
bull donrsquot know nearby rate
bull but 980425 may imply rate is high
bull look for weak GRBs like 980425
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
With decreasing metallicity the bindingenergy of the core and the size of the silicon core both increase making black hole formation more likely atlow metallicity Woosley Heger amp Weaver RMP (2002)
Black hole formation may be unavoidable for low metallicity
Solar metallicity
Low metallicity
In the absence of mass lossand magnetic fields there wouldbe abundant progenitors
Unfortunately nature has both
15 solar mass helium core born rotating rigidly at f times break up
The more difficult problem is the angular momentum Thisis a problem shared by all current GRB models that invokemassive stars
- What is a Gamma-Ray Burst
- Superbowl Burst
- Slide 3
- 135 models (1993)
- Slide 5
- Slide 6
- Slide 7
- GRB991121
- GRB030329SN2003DH
- Slide 10
- Slide 11
- Slide 12
- GRB central engine
- ldquoDelayedrdquo SN Explosion
- Pre-Supernova Density Structure
- Failure of delayed mechanism
- Stellar Rotation
- Slide 18
- Slide 19
- Collapsar Simulations
- Collapsar Disk Animation
- Disk Formation Movie
- Slide 23
- Slide 24
- Slide 25
- Collapsar results
- Slide 27
- Jet Birth
- Relativistic Jet Movie
- Collapsar stages
- Slide 31
- Slide 32
- Nickel Wind Movie
- Slide 34
- Slide 35
- Slide 36
- Slide 37
- Slide 38
- Collapsars
- GRBGW
- Rates
- SN GW
- Implications
- Issues
- Principle Results
- Slide 46
- Slide 47
-
Relativistic Jet Movie
Collapsar stages1 Iron core collapse disk formation
T~1010K ~108gcm-3 photodisintegration cooling pair capture disk is free nucleons (2 s)
2 Polar density declines to allow jet birthfrac12v3 Edep (2-5 s)
3 Jet tunnels out of star (5 s) Wolf-Rayet4 Jet powered for ~10 more seconds
Evacuates polar channel and reaches asymptotic speed (10 s)
T_GRB T_collapse
Jupiter
Red Supergiant
R~1013 cm
Blue Supergiant
R~1012 cm
Wolf-Rayet Star
R~1011 cm
Type Ib or Ic
Supernova
Supernovae
Ia
WD cosmology
Type II
Hydrogen
Type I
No Hydrogen
Ib Ic
exploding WR
thermonuclear old pop E galaxies
core collapse massive stars
Nickel Wind Movie
ldquoNickel Windrdquo
T gt 5 x 109 K
Fallback in weak SN explosions
Shock reaches
surface of star but parts of star are
not ejected to infinity
Fallback accretion Mms ~ 25 Msun Same star
exploded with a range of explosion energies
Significant accretion for thousands of
seconds ndash days
If fallback fuels a jet with power
fmc2
May power ldquohypernovardquo or long duration
GRBWeak
supernova shock
Shock breakout X-Ray transient
2 ldquoBriefrdquo jet tengine tjet
Engine dies before jet breakout
Mildly relativistic shock breakout
MacFadyen (1999)
What made SN1998bw+GRB980425
1 Accretion powered hypernova w Nickel wind
MacFadyen (2002)
E~ 1052 erg M(Ni)~05 M
GRB from ~3 shock breakout (Tan et al 2001 Perna amp Vietri 2002)
Collapsars
bull Can make ldquolongrdquo GRBs in H stripped (WR) stars tengine gt tescape
bull Short bursts may be compact binary mergersbull Need SN failure amp angular momentum
ndash Low metallicity binary can help
bull Star can explode -gt SN if nickel is made Predicts GRBSN association Type Ibc
bull SNGRB ratio may depend on angular momentumbull ldquoNickel windrdquo can explode star -gt hypernova
ndash H env Type II (no GRB) no H Type I + GRB
GRBGW bull Long GRBs
ndash not brighter than SN in GW
ndash very far Gpc
ndash very rare lt 1 SN
bull Short GBsndash merging ns-bh binaries
ndash maybe closer than long bursts
ndash short delay between event and GRB
ndash good for SWIFTLIGO
Rates
bull SN 1s = 100000 day
bull GRB 1day (BATSE) = 1000day
bull GRB rate = 1 of SN rate
bull maybe more collapsars than GRBs
bull =gt more rapidly rotating SN
bull SN with collapsar engine
bull look for bright Type Ic (w broad lines)
SN GW
bull SN1998bwGRB980425
bull 40 Mpc
bull maybe dominant GRB
bull rapid rotaters
bull SNAPROTSE look for 1998bw 2003dh like SN
bull many light curves -gt better t_explode
Implications
bull Probe engine directly
bull collapse duration vs GRB duration
bull collapseGRB delay (internal vs external)
bull disk properties ndash low viscosity big disks
Issues
bull too much j =gt no GRB but bright GW
bull may need low metallicity for GRB
bull prefer high redshift
bull donrsquot know nearby rate
bull but 980425 may imply rate is high
bull look for weak GRBs like 980425
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
With decreasing metallicity the bindingenergy of the core and the size of the silicon core both increase making black hole formation more likely atlow metallicity Woosley Heger amp Weaver RMP (2002)
Black hole formation may be unavoidable for low metallicity
Solar metallicity
Low metallicity
In the absence of mass lossand magnetic fields there wouldbe abundant progenitors
Unfortunately nature has both
15 solar mass helium core born rotating rigidly at f times break up
The more difficult problem is the angular momentum Thisis a problem shared by all current GRB models that invokemassive stars
- What is a Gamma-Ray Burst
- Superbowl Burst
- Slide 3
- 135 models (1993)
- Slide 5
- Slide 6
- Slide 7
- GRB991121
- GRB030329SN2003DH
- Slide 10
- Slide 11
- Slide 12
- GRB central engine
- ldquoDelayedrdquo SN Explosion
- Pre-Supernova Density Structure
- Failure of delayed mechanism
- Stellar Rotation
- Slide 18
- Slide 19
- Collapsar Simulations
- Collapsar Disk Animation
- Disk Formation Movie
- Slide 23
- Slide 24
- Slide 25
- Collapsar results
- Slide 27
- Jet Birth
- Relativistic Jet Movie
- Collapsar stages
- Slide 31
- Slide 32
- Nickel Wind Movie
- Slide 34
- Slide 35
- Slide 36
- Slide 37
- Slide 38
- Collapsars
- GRBGW
- Rates
- SN GW
- Implications
- Issues
- Principle Results
- Slide 46
- Slide 47
-
Collapsar stages1 Iron core collapse disk formation
T~1010K ~108gcm-3 photodisintegration cooling pair capture disk is free nucleons (2 s)
2 Polar density declines to allow jet birthfrac12v3 Edep (2-5 s)
3 Jet tunnels out of star (5 s) Wolf-Rayet4 Jet powered for ~10 more seconds
Evacuates polar channel and reaches asymptotic speed (10 s)
T_GRB T_collapse
Jupiter
Red Supergiant
R~1013 cm
Blue Supergiant
R~1012 cm
Wolf-Rayet Star
R~1011 cm
Type Ib or Ic
Supernova
Supernovae
Ia
WD cosmology
Type II
Hydrogen
Type I
No Hydrogen
Ib Ic
exploding WR
thermonuclear old pop E galaxies
core collapse massive stars
Nickel Wind Movie
ldquoNickel Windrdquo
T gt 5 x 109 K
Fallback in weak SN explosions
Shock reaches
surface of star but parts of star are
not ejected to infinity
Fallback accretion Mms ~ 25 Msun Same star
exploded with a range of explosion energies
Significant accretion for thousands of
seconds ndash days
If fallback fuels a jet with power
fmc2
May power ldquohypernovardquo or long duration
GRBWeak
supernova shock
Shock breakout X-Ray transient
2 ldquoBriefrdquo jet tengine tjet
Engine dies before jet breakout
Mildly relativistic shock breakout
MacFadyen (1999)
What made SN1998bw+GRB980425
1 Accretion powered hypernova w Nickel wind
MacFadyen (2002)
E~ 1052 erg M(Ni)~05 M
GRB from ~3 shock breakout (Tan et al 2001 Perna amp Vietri 2002)
Collapsars
bull Can make ldquolongrdquo GRBs in H stripped (WR) stars tengine gt tescape
bull Short bursts may be compact binary mergersbull Need SN failure amp angular momentum
ndash Low metallicity binary can help
bull Star can explode -gt SN if nickel is made Predicts GRBSN association Type Ibc
bull SNGRB ratio may depend on angular momentumbull ldquoNickel windrdquo can explode star -gt hypernova
ndash H env Type II (no GRB) no H Type I + GRB
GRBGW bull Long GRBs
ndash not brighter than SN in GW
ndash very far Gpc
ndash very rare lt 1 SN
bull Short GBsndash merging ns-bh binaries
ndash maybe closer than long bursts
ndash short delay between event and GRB
ndash good for SWIFTLIGO
Rates
bull SN 1s = 100000 day
bull GRB 1day (BATSE) = 1000day
bull GRB rate = 1 of SN rate
bull maybe more collapsars than GRBs
bull =gt more rapidly rotating SN
bull SN with collapsar engine
bull look for bright Type Ic (w broad lines)
SN GW
bull SN1998bwGRB980425
bull 40 Mpc
bull maybe dominant GRB
bull rapid rotaters
bull SNAPROTSE look for 1998bw 2003dh like SN
bull many light curves -gt better t_explode
Implications
bull Probe engine directly
bull collapse duration vs GRB duration
bull collapseGRB delay (internal vs external)
bull disk properties ndash low viscosity big disks
Issues
bull too much j =gt no GRB but bright GW
bull may need low metallicity for GRB
bull prefer high redshift
bull donrsquot know nearby rate
bull but 980425 may imply rate is high
bull look for weak GRBs like 980425
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
With decreasing metallicity the bindingenergy of the core and the size of the silicon core both increase making black hole formation more likely atlow metallicity Woosley Heger amp Weaver RMP (2002)
Black hole formation may be unavoidable for low metallicity
Solar metallicity
Low metallicity
In the absence of mass lossand magnetic fields there wouldbe abundant progenitors
Unfortunately nature has both
15 solar mass helium core born rotating rigidly at f times break up
The more difficult problem is the angular momentum Thisis a problem shared by all current GRB models that invokemassive stars
- What is a Gamma-Ray Burst
- Superbowl Burst
- Slide 3
- 135 models (1993)
- Slide 5
- Slide 6
- Slide 7
- GRB991121
- GRB030329SN2003DH
- Slide 10
- Slide 11
- Slide 12
- GRB central engine
- ldquoDelayedrdquo SN Explosion
- Pre-Supernova Density Structure
- Failure of delayed mechanism
- Stellar Rotation
- Slide 18
- Slide 19
- Collapsar Simulations
- Collapsar Disk Animation
- Disk Formation Movie
- Slide 23
- Slide 24
- Slide 25
- Collapsar results
- Slide 27
- Jet Birth
- Relativistic Jet Movie
- Collapsar stages
- Slide 31
- Slide 32
- Nickel Wind Movie
- Slide 34
- Slide 35
- Slide 36
- Slide 37
- Slide 38
- Collapsars
- GRBGW
- Rates
- SN GW
- Implications
- Issues
- Principle Results
- Slide 46
- Slide 47
-
Jupiter
Red Supergiant
R~1013 cm
Blue Supergiant
R~1012 cm
Wolf-Rayet Star
R~1011 cm
Type Ib or Ic
Supernova
Supernovae
Ia
WD cosmology
Type II
Hydrogen
Type I
No Hydrogen
Ib Ic
exploding WR
thermonuclear old pop E galaxies
core collapse massive stars
Nickel Wind Movie
ldquoNickel Windrdquo
T gt 5 x 109 K
Fallback in weak SN explosions
Shock reaches
surface of star but parts of star are
not ejected to infinity
Fallback accretion Mms ~ 25 Msun Same star
exploded with a range of explosion energies
Significant accretion for thousands of
seconds ndash days
If fallback fuels a jet with power
fmc2
May power ldquohypernovardquo or long duration
GRBWeak
supernova shock
Shock breakout X-Ray transient
2 ldquoBriefrdquo jet tengine tjet
Engine dies before jet breakout
Mildly relativistic shock breakout
MacFadyen (1999)
What made SN1998bw+GRB980425
1 Accretion powered hypernova w Nickel wind
MacFadyen (2002)
E~ 1052 erg M(Ni)~05 M
GRB from ~3 shock breakout (Tan et al 2001 Perna amp Vietri 2002)
Collapsars
bull Can make ldquolongrdquo GRBs in H stripped (WR) stars tengine gt tescape
bull Short bursts may be compact binary mergersbull Need SN failure amp angular momentum
ndash Low metallicity binary can help
bull Star can explode -gt SN if nickel is made Predicts GRBSN association Type Ibc
bull SNGRB ratio may depend on angular momentumbull ldquoNickel windrdquo can explode star -gt hypernova
ndash H env Type II (no GRB) no H Type I + GRB
GRBGW bull Long GRBs
ndash not brighter than SN in GW
ndash very far Gpc
ndash very rare lt 1 SN
bull Short GBsndash merging ns-bh binaries
ndash maybe closer than long bursts
ndash short delay between event and GRB
ndash good for SWIFTLIGO
Rates
bull SN 1s = 100000 day
bull GRB 1day (BATSE) = 1000day
bull GRB rate = 1 of SN rate
bull maybe more collapsars than GRBs
bull =gt more rapidly rotating SN
bull SN with collapsar engine
bull look for bright Type Ic (w broad lines)
SN GW
bull SN1998bwGRB980425
bull 40 Mpc
bull maybe dominant GRB
bull rapid rotaters
bull SNAPROTSE look for 1998bw 2003dh like SN
bull many light curves -gt better t_explode
Implications
bull Probe engine directly
bull collapse duration vs GRB duration
bull collapseGRB delay (internal vs external)
bull disk properties ndash low viscosity big disks
Issues
bull too much j =gt no GRB but bright GW
bull may need low metallicity for GRB
bull prefer high redshift
bull donrsquot know nearby rate
bull but 980425 may imply rate is high
bull look for weak GRBs like 980425
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
With decreasing metallicity the bindingenergy of the core and the size of the silicon core both increase making black hole formation more likely atlow metallicity Woosley Heger amp Weaver RMP (2002)
Black hole formation may be unavoidable for low metallicity
Solar metallicity
Low metallicity
In the absence of mass lossand magnetic fields there wouldbe abundant progenitors
Unfortunately nature has both
15 solar mass helium core born rotating rigidly at f times break up
The more difficult problem is the angular momentum Thisis a problem shared by all current GRB models that invokemassive stars
- What is a Gamma-Ray Burst
- Superbowl Burst
- Slide 3
- 135 models (1993)
- Slide 5
- Slide 6
- Slide 7
- GRB991121
- GRB030329SN2003DH
- Slide 10
- Slide 11
- Slide 12
- GRB central engine
- ldquoDelayedrdquo SN Explosion
- Pre-Supernova Density Structure
- Failure of delayed mechanism
- Stellar Rotation
- Slide 18
- Slide 19
- Collapsar Simulations
- Collapsar Disk Animation
- Disk Formation Movie
- Slide 23
- Slide 24
- Slide 25
- Collapsar results
- Slide 27
- Jet Birth
- Relativistic Jet Movie
- Collapsar stages
- Slide 31
- Slide 32
- Nickel Wind Movie
- Slide 34
- Slide 35
- Slide 36
- Slide 37
- Slide 38
- Collapsars
- GRBGW
- Rates
- SN GW
- Implications
- Issues
- Principle Results
- Slide 46
- Slide 47
-
Supernovae
Ia
WD cosmology
Type II
Hydrogen
Type I
No Hydrogen
Ib Ic
exploding WR
thermonuclear old pop E galaxies
core collapse massive stars
Nickel Wind Movie
ldquoNickel Windrdquo
T gt 5 x 109 K
Fallback in weak SN explosions
Shock reaches
surface of star but parts of star are
not ejected to infinity
Fallback accretion Mms ~ 25 Msun Same star
exploded with a range of explosion energies
Significant accretion for thousands of
seconds ndash days
If fallback fuels a jet with power
fmc2
May power ldquohypernovardquo or long duration
GRBWeak
supernova shock
Shock breakout X-Ray transient
2 ldquoBriefrdquo jet tengine tjet
Engine dies before jet breakout
Mildly relativistic shock breakout
MacFadyen (1999)
What made SN1998bw+GRB980425
1 Accretion powered hypernova w Nickel wind
MacFadyen (2002)
E~ 1052 erg M(Ni)~05 M
GRB from ~3 shock breakout (Tan et al 2001 Perna amp Vietri 2002)
Collapsars
bull Can make ldquolongrdquo GRBs in H stripped (WR) stars tengine gt tescape
bull Short bursts may be compact binary mergersbull Need SN failure amp angular momentum
ndash Low metallicity binary can help
bull Star can explode -gt SN if nickel is made Predicts GRBSN association Type Ibc
bull SNGRB ratio may depend on angular momentumbull ldquoNickel windrdquo can explode star -gt hypernova
ndash H env Type II (no GRB) no H Type I + GRB
GRBGW bull Long GRBs
ndash not brighter than SN in GW
ndash very far Gpc
ndash very rare lt 1 SN
bull Short GBsndash merging ns-bh binaries
ndash maybe closer than long bursts
ndash short delay between event and GRB
ndash good for SWIFTLIGO
Rates
bull SN 1s = 100000 day
bull GRB 1day (BATSE) = 1000day
bull GRB rate = 1 of SN rate
bull maybe more collapsars than GRBs
bull =gt more rapidly rotating SN
bull SN with collapsar engine
bull look for bright Type Ic (w broad lines)
SN GW
bull SN1998bwGRB980425
bull 40 Mpc
bull maybe dominant GRB
bull rapid rotaters
bull SNAPROTSE look for 1998bw 2003dh like SN
bull many light curves -gt better t_explode
Implications
bull Probe engine directly
bull collapse duration vs GRB duration
bull collapseGRB delay (internal vs external)
bull disk properties ndash low viscosity big disks
Issues
bull too much j =gt no GRB but bright GW
bull may need low metallicity for GRB
bull prefer high redshift
bull donrsquot know nearby rate
bull but 980425 may imply rate is high
bull look for weak GRBs like 980425
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
With decreasing metallicity the bindingenergy of the core and the size of the silicon core both increase making black hole formation more likely atlow metallicity Woosley Heger amp Weaver RMP (2002)
Black hole formation may be unavoidable for low metallicity
Solar metallicity
Low metallicity
In the absence of mass lossand magnetic fields there wouldbe abundant progenitors
Unfortunately nature has both
15 solar mass helium core born rotating rigidly at f times break up
The more difficult problem is the angular momentum Thisis a problem shared by all current GRB models that invokemassive stars
- What is a Gamma-Ray Burst
- Superbowl Burst
- Slide 3
- 135 models (1993)
- Slide 5
- Slide 6
- Slide 7
- GRB991121
- GRB030329SN2003DH
- Slide 10
- Slide 11
- Slide 12
- GRB central engine
- ldquoDelayedrdquo SN Explosion
- Pre-Supernova Density Structure
- Failure of delayed mechanism
- Stellar Rotation
- Slide 18
- Slide 19
- Collapsar Simulations
- Collapsar Disk Animation
- Disk Formation Movie
- Slide 23
- Slide 24
- Slide 25
- Collapsar results
- Slide 27
- Jet Birth
- Relativistic Jet Movie
- Collapsar stages
- Slide 31
- Slide 32
- Nickel Wind Movie
- Slide 34
- Slide 35
- Slide 36
- Slide 37
- Slide 38
- Collapsars
- GRBGW
- Rates
- SN GW
- Implications
- Issues
- Principle Results
- Slide 46
- Slide 47
-
Nickel Wind Movie
ldquoNickel Windrdquo
T gt 5 x 109 K
Fallback in weak SN explosions
Shock reaches
surface of star but parts of star are
not ejected to infinity
Fallback accretion Mms ~ 25 Msun Same star
exploded with a range of explosion energies
Significant accretion for thousands of
seconds ndash days
If fallback fuels a jet with power
fmc2
May power ldquohypernovardquo or long duration
GRBWeak
supernova shock
Shock breakout X-Ray transient
2 ldquoBriefrdquo jet tengine tjet
Engine dies before jet breakout
Mildly relativistic shock breakout
MacFadyen (1999)
What made SN1998bw+GRB980425
1 Accretion powered hypernova w Nickel wind
MacFadyen (2002)
E~ 1052 erg M(Ni)~05 M
GRB from ~3 shock breakout (Tan et al 2001 Perna amp Vietri 2002)
Collapsars
bull Can make ldquolongrdquo GRBs in H stripped (WR) stars tengine gt tescape
bull Short bursts may be compact binary mergersbull Need SN failure amp angular momentum
ndash Low metallicity binary can help
bull Star can explode -gt SN if nickel is made Predicts GRBSN association Type Ibc
bull SNGRB ratio may depend on angular momentumbull ldquoNickel windrdquo can explode star -gt hypernova
ndash H env Type II (no GRB) no H Type I + GRB
GRBGW bull Long GRBs
ndash not brighter than SN in GW
ndash very far Gpc
ndash very rare lt 1 SN
bull Short GBsndash merging ns-bh binaries
ndash maybe closer than long bursts
ndash short delay between event and GRB
ndash good for SWIFTLIGO
Rates
bull SN 1s = 100000 day
bull GRB 1day (BATSE) = 1000day
bull GRB rate = 1 of SN rate
bull maybe more collapsars than GRBs
bull =gt more rapidly rotating SN
bull SN with collapsar engine
bull look for bright Type Ic (w broad lines)
SN GW
bull SN1998bwGRB980425
bull 40 Mpc
bull maybe dominant GRB
bull rapid rotaters
bull SNAPROTSE look for 1998bw 2003dh like SN
bull many light curves -gt better t_explode
Implications
bull Probe engine directly
bull collapse duration vs GRB duration
bull collapseGRB delay (internal vs external)
bull disk properties ndash low viscosity big disks
Issues
bull too much j =gt no GRB but bright GW
bull may need low metallicity for GRB
bull prefer high redshift
bull donrsquot know nearby rate
bull but 980425 may imply rate is high
bull look for weak GRBs like 980425
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
With decreasing metallicity the bindingenergy of the core and the size of the silicon core both increase making black hole formation more likely atlow metallicity Woosley Heger amp Weaver RMP (2002)
Black hole formation may be unavoidable for low metallicity
Solar metallicity
Low metallicity
In the absence of mass lossand magnetic fields there wouldbe abundant progenitors
Unfortunately nature has both
15 solar mass helium core born rotating rigidly at f times break up
The more difficult problem is the angular momentum Thisis a problem shared by all current GRB models that invokemassive stars
- What is a Gamma-Ray Burst
- Superbowl Burst
- Slide 3
- 135 models (1993)
- Slide 5
- Slide 6
- Slide 7
- GRB991121
- GRB030329SN2003DH
- Slide 10
- Slide 11
- Slide 12
- GRB central engine
- ldquoDelayedrdquo SN Explosion
- Pre-Supernova Density Structure
- Failure of delayed mechanism
- Stellar Rotation
- Slide 18
- Slide 19
- Collapsar Simulations
- Collapsar Disk Animation
- Disk Formation Movie
- Slide 23
- Slide 24
- Slide 25
- Collapsar results
- Slide 27
- Jet Birth
- Relativistic Jet Movie
- Collapsar stages
- Slide 31
- Slide 32
- Nickel Wind Movie
- Slide 34
- Slide 35
- Slide 36
- Slide 37
- Slide 38
- Collapsars
- GRBGW
- Rates
- SN GW
- Implications
- Issues
- Principle Results
- Slide 46
- Slide 47
-
Fallback in weak SN explosions
Shock reaches
surface of star but parts of star are
not ejected to infinity
Fallback accretion Mms ~ 25 Msun Same star
exploded with a range of explosion energies
Significant accretion for thousands of
seconds ndash days
If fallback fuels a jet with power
fmc2
May power ldquohypernovardquo or long duration
GRBWeak
supernova shock
Shock breakout X-Ray transient
2 ldquoBriefrdquo jet tengine tjet
Engine dies before jet breakout
Mildly relativistic shock breakout
MacFadyen (1999)
What made SN1998bw+GRB980425
1 Accretion powered hypernova w Nickel wind
MacFadyen (2002)
E~ 1052 erg M(Ni)~05 M
GRB from ~3 shock breakout (Tan et al 2001 Perna amp Vietri 2002)
Collapsars
bull Can make ldquolongrdquo GRBs in H stripped (WR) stars tengine gt tescape
bull Short bursts may be compact binary mergersbull Need SN failure amp angular momentum
ndash Low metallicity binary can help
bull Star can explode -gt SN if nickel is made Predicts GRBSN association Type Ibc
bull SNGRB ratio may depend on angular momentumbull ldquoNickel windrdquo can explode star -gt hypernova
ndash H env Type II (no GRB) no H Type I + GRB
GRBGW bull Long GRBs
ndash not brighter than SN in GW
ndash very far Gpc
ndash very rare lt 1 SN
bull Short GBsndash merging ns-bh binaries
ndash maybe closer than long bursts
ndash short delay between event and GRB
ndash good for SWIFTLIGO
Rates
bull SN 1s = 100000 day
bull GRB 1day (BATSE) = 1000day
bull GRB rate = 1 of SN rate
bull maybe more collapsars than GRBs
bull =gt more rapidly rotating SN
bull SN with collapsar engine
bull look for bright Type Ic (w broad lines)
SN GW
bull SN1998bwGRB980425
bull 40 Mpc
bull maybe dominant GRB
bull rapid rotaters
bull SNAPROTSE look for 1998bw 2003dh like SN
bull many light curves -gt better t_explode
Implications
bull Probe engine directly
bull collapse duration vs GRB duration
bull collapseGRB delay (internal vs external)
bull disk properties ndash low viscosity big disks
Issues
bull too much j =gt no GRB but bright GW
bull may need low metallicity for GRB
bull prefer high redshift
bull donrsquot know nearby rate
bull but 980425 may imply rate is high
bull look for weak GRBs like 980425
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
With decreasing metallicity the bindingenergy of the core and the size of the silicon core both increase making black hole formation more likely atlow metallicity Woosley Heger amp Weaver RMP (2002)
Black hole formation may be unavoidable for low metallicity
Solar metallicity
Low metallicity
In the absence of mass lossand magnetic fields there wouldbe abundant progenitors
Unfortunately nature has both
15 solar mass helium core born rotating rigidly at f times break up
The more difficult problem is the angular momentum Thisis a problem shared by all current GRB models that invokemassive stars
- What is a Gamma-Ray Burst
- Superbowl Burst
- Slide 3
- 135 models (1993)
- Slide 5
- Slide 6
- Slide 7
- GRB991121
- GRB030329SN2003DH
- Slide 10
- Slide 11
- Slide 12
- GRB central engine
- ldquoDelayedrdquo SN Explosion
- Pre-Supernova Density Structure
- Failure of delayed mechanism
- Stellar Rotation
- Slide 18
- Slide 19
- Collapsar Simulations
- Collapsar Disk Animation
- Disk Formation Movie
- Slide 23
- Slide 24
- Slide 25
- Collapsar results
- Slide 27
- Jet Birth
- Relativistic Jet Movie
- Collapsar stages
- Slide 31
- Slide 32
- Nickel Wind Movie
- Slide 34
- Slide 35
- Slide 36
- Slide 37
- Slide 38
- Collapsars
- GRBGW
- Rates
- SN GW
- Implications
- Issues
- Principle Results
- Slide 46
- Slide 47
-
Fallback accretion Mms ~ 25 Msun Same star
exploded with a range of explosion energies
Significant accretion for thousands of
seconds ndash days
If fallback fuels a jet with power
fmc2
May power ldquohypernovardquo or long duration
GRBWeak
supernova shock
Shock breakout X-Ray transient
2 ldquoBriefrdquo jet tengine tjet
Engine dies before jet breakout
Mildly relativistic shock breakout
MacFadyen (1999)
What made SN1998bw+GRB980425
1 Accretion powered hypernova w Nickel wind
MacFadyen (2002)
E~ 1052 erg M(Ni)~05 M
GRB from ~3 shock breakout (Tan et al 2001 Perna amp Vietri 2002)
Collapsars
bull Can make ldquolongrdquo GRBs in H stripped (WR) stars tengine gt tescape
bull Short bursts may be compact binary mergersbull Need SN failure amp angular momentum
ndash Low metallicity binary can help
bull Star can explode -gt SN if nickel is made Predicts GRBSN association Type Ibc
bull SNGRB ratio may depend on angular momentumbull ldquoNickel windrdquo can explode star -gt hypernova
ndash H env Type II (no GRB) no H Type I + GRB
GRBGW bull Long GRBs
ndash not brighter than SN in GW
ndash very far Gpc
ndash very rare lt 1 SN
bull Short GBsndash merging ns-bh binaries
ndash maybe closer than long bursts
ndash short delay between event and GRB
ndash good for SWIFTLIGO
Rates
bull SN 1s = 100000 day
bull GRB 1day (BATSE) = 1000day
bull GRB rate = 1 of SN rate
bull maybe more collapsars than GRBs
bull =gt more rapidly rotating SN
bull SN with collapsar engine
bull look for bright Type Ic (w broad lines)
SN GW
bull SN1998bwGRB980425
bull 40 Mpc
bull maybe dominant GRB
bull rapid rotaters
bull SNAPROTSE look for 1998bw 2003dh like SN
bull many light curves -gt better t_explode
Implications
bull Probe engine directly
bull collapse duration vs GRB duration
bull collapseGRB delay (internal vs external)
bull disk properties ndash low viscosity big disks
Issues
bull too much j =gt no GRB but bright GW
bull may need low metallicity for GRB
bull prefer high redshift
bull donrsquot know nearby rate
bull but 980425 may imply rate is high
bull look for weak GRBs like 980425
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
With decreasing metallicity the bindingenergy of the core and the size of the silicon core both increase making black hole formation more likely atlow metallicity Woosley Heger amp Weaver RMP (2002)
Black hole formation may be unavoidable for low metallicity
Solar metallicity
Low metallicity
In the absence of mass lossand magnetic fields there wouldbe abundant progenitors
Unfortunately nature has both
15 solar mass helium core born rotating rigidly at f times break up
The more difficult problem is the angular momentum Thisis a problem shared by all current GRB models that invokemassive stars
- What is a Gamma-Ray Burst
- Superbowl Burst
- Slide 3
- 135 models (1993)
- Slide 5
- Slide 6
- Slide 7
- GRB991121
- GRB030329SN2003DH
- Slide 10
- Slide 11
- Slide 12
- GRB central engine
- ldquoDelayedrdquo SN Explosion
- Pre-Supernova Density Structure
- Failure of delayed mechanism
- Stellar Rotation
- Slide 18
- Slide 19
- Collapsar Simulations
- Collapsar Disk Animation
- Disk Formation Movie
- Slide 23
- Slide 24
- Slide 25
- Collapsar results
- Slide 27
- Jet Birth
- Relativistic Jet Movie
- Collapsar stages
- Slide 31
- Slide 32
- Nickel Wind Movie
- Slide 34
- Slide 35
- Slide 36
- Slide 37
- Slide 38
- Collapsars
- GRBGW
- Rates
- SN GW
- Implications
- Issues
- Principle Results
- Slide 46
- Slide 47
-
If fallback fuels a jet with power
fmc2
May power ldquohypernovardquo or long duration
GRBWeak
supernova shock
Shock breakout X-Ray transient
2 ldquoBriefrdquo jet tengine tjet
Engine dies before jet breakout
Mildly relativistic shock breakout
MacFadyen (1999)
What made SN1998bw+GRB980425
1 Accretion powered hypernova w Nickel wind
MacFadyen (2002)
E~ 1052 erg M(Ni)~05 M
GRB from ~3 shock breakout (Tan et al 2001 Perna amp Vietri 2002)
Collapsars
bull Can make ldquolongrdquo GRBs in H stripped (WR) stars tengine gt tescape
bull Short bursts may be compact binary mergersbull Need SN failure amp angular momentum
ndash Low metallicity binary can help
bull Star can explode -gt SN if nickel is made Predicts GRBSN association Type Ibc
bull SNGRB ratio may depend on angular momentumbull ldquoNickel windrdquo can explode star -gt hypernova
ndash H env Type II (no GRB) no H Type I + GRB
GRBGW bull Long GRBs
ndash not brighter than SN in GW
ndash very far Gpc
ndash very rare lt 1 SN
bull Short GBsndash merging ns-bh binaries
ndash maybe closer than long bursts
ndash short delay between event and GRB
ndash good for SWIFTLIGO
Rates
bull SN 1s = 100000 day
bull GRB 1day (BATSE) = 1000day
bull GRB rate = 1 of SN rate
bull maybe more collapsars than GRBs
bull =gt more rapidly rotating SN
bull SN with collapsar engine
bull look for bright Type Ic (w broad lines)
SN GW
bull SN1998bwGRB980425
bull 40 Mpc
bull maybe dominant GRB
bull rapid rotaters
bull SNAPROTSE look for 1998bw 2003dh like SN
bull many light curves -gt better t_explode
Implications
bull Probe engine directly
bull collapse duration vs GRB duration
bull collapseGRB delay (internal vs external)
bull disk properties ndash low viscosity big disks
Issues
bull too much j =gt no GRB but bright GW
bull may need low metallicity for GRB
bull prefer high redshift
bull donrsquot know nearby rate
bull but 980425 may imply rate is high
bull look for weak GRBs like 980425
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
With decreasing metallicity the bindingenergy of the core and the size of the silicon core both increase making black hole formation more likely atlow metallicity Woosley Heger amp Weaver RMP (2002)
Black hole formation may be unavoidable for low metallicity
Solar metallicity
Low metallicity
In the absence of mass lossand magnetic fields there wouldbe abundant progenitors
Unfortunately nature has both
15 solar mass helium core born rotating rigidly at f times break up
The more difficult problem is the angular momentum Thisis a problem shared by all current GRB models that invokemassive stars
- What is a Gamma-Ray Burst
- Superbowl Burst
- Slide 3
- 135 models (1993)
- Slide 5
- Slide 6
- Slide 7
- GRB991121
- GRB030329SN2003DH
- Slide 10
- Slide 11
- Slide 12
- GRB central engine
- ldquoDelayedrdquo SN Explosion
- Pre-Supernova Density Structure
- Failure of delayed mechanism
- Stellar Rotation
- Slide 18
- Slide 19
- Collapsar Simulations
- Collapsar Disk Animation
- Disk Formation Movie
- Slide 23
- Slide 24
- Slide 25
- Collapsar results
- Slide 27
- Jet Birth
- Relativistic Jet Movie
- Collapsar stages
- Slide 31
- Slide 32
- Nickel Wind Movie
- Slide 34
- Slide 35
- Slide 36
- Slide 37
- Slide 38
- Collapsars
- GRBGW
- Rates
- SN GW
- Implications
- Issues
- Principle Results
- Slide 46
- Slide 47
-
Shock breakout X-Ray transient
2 ldquoBriefrdquo jet tengine tjet
Engine dies before jet breakout
Mildly relativistic shock breakout
MacFadyen (1999)
What made SN1998bw+GRB980425
1 Accretion powered hypernova w Nickel wind
MacFadyen (2002)
E~ 1052 erg M(Ni)~05 M
GRB from ~3 shock breakout (Tan et al 2001 Perna amp Vietri 2002)
Collapsars
bull Can make ldquolongrdquo GRBs in H stripped (WR) stars tengine gt tescape
bull Short bursts may be compact binary mergersbull Need SN failure amp angular momentum
ndash Low metallicity binary can help
bull Star can explode -gt SN if nickel is made Predicts GRBSN association Type Ibc
bull SNGRB ratio may depend on angular momentumbull ldquoNickel windrdquo can explode star -gt hypernova
ndash H env Type II (no GRB) no H Type I + GRB
GRBGW bull Long GRBs
ndash not brighter than SN in GW
ndash very far Gpc
ndash very rare lt 1 SN
bull Short GBsndash merging ns-bh binaries
ndash maybe closer than long bursts
ndash short delay between event and GRB
ndash good for SWIFTLIGO
Rates
bull SN 1s = 100000 day
bull GRB 1day (BATSE) = 1000day
bull GRB rate = 1 of SN rate
bull maybe more collapsars than GRBs
bull =gt more rapidly rotating SN
bull SN with collapsar engine
bull look for bright Type Ic (w broad lines)
SN GW
bull SN1998bwGRB980425
bull 40 Mpc
bull maybe dominant GRB
bull rapid rotaters
bull SNAPROTSE look for 1998bw 2003dh like SN
bull many light curves -gt better t_explode
Implications
bull Probe engine directly
bull collapse duration vs GRB duration
bull collapseGRB delay (internal vs external)
bull disk properties ndash low viscosity big disks
Issues
bull too much j =gt no GRB but bright GW
bull may need low metallicity for GRB
bull prefer high redshift
bull donrsquot know nearby rate
bull but 980425 may imply rate is high
bull look for weak GRBs like 980425
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
With decreasing metallicity the bindingenergy of the core and the size of the silicon core both increase making black hole formation more likely atlow metallicity Woosley Heger amp Weaver RMP (2002)
Black hole formation may be unavoidable for low metallicity
Solar metallicity
Low metallicity
In the absence of mass lossand magnetic fields there wouldbe abundant progenitors
Unfortunately nature has both
15 solar mass helium core born rotating rigidly at f times break up
The more difficult problem is the angular momentum Thisis a problem shared by all current GRB models that invokemassive stars
- What is a Gamma-Ray Burst
- Superbowl Burst
- Slide 3
- 135 models (1993)
- Slide 5
- Slide 6
- Slide 7
- GRB991121
- GRB030329SN2003DH
- Slide 10
- Slide 11
- Slide 12
- GRB central engine
- ldquoDelayedrdquo SN Explosion
- Pre-Supernova Density Structure
- Failure of delayed mechanism
- Stellar Rotation
- Slide 18
- Slide 19
- Collapsar Simulations
- Collapsar Disk Animation
- Disk Formation Movie
- Slide 23
- Slide 24
- Slide 25
- Collapsar results
- Slide 27
- Jet Birth
- Relativistic Jet Movie
- Collapsar stages
- Slide 31
- Slide 32
- Nickel Wind Movie
- Slide 34
- Slide 35
- Slide 36
- Slide 37
- Slide 38
- Collapsars
- GRBGW
- Rates
- SN GW
- Implications
- Issues
- Principle Results
- Slide 46
- Slide 47
-
2 ldquoBriefrdquo jet tengine tjet
Engine dies before jet breakout
Mildly relativistic shock breakout
MacFadyen (1999)
What made SN1998bw+GRB980425
1 Accretion powered hypernova w Nickel wind
MacFadyen (2002)
E~ 1052 erg M(Ni)~05 M
GRB from ~3 shock breakout (Tan et al 2001 Perna amp Vietri 2002)
Collapsars
bull Can make ldquolongrdquo GRBs in H stripped (WR) stars tengine gt tescape
bull Short bursts may be compact binary mergersbull Need SN failure amp angular momentum
ndash Low metallicity binary can help
bull Star can explode -gt SN if nickel is made Predicts GRBSN association Type Ibc
bull SNGRB ratio may depend on angular momentumbull ldquoNickel windrdquo can explode star -gt hypernova
ndash H env Type II (no GRB) no H Type I + GRB
GRBGW bull Long GRBs
ndash not brighter than SN in GW
ndash very far Gpc
ndash very rare lt 1 SN
bull Short GBsndash merging ns-bh binaries
ndash maybe closer than long bursts
ndash short delay between event and GRB
ndash good for SWIFTLIGO
Rates
bull SN 1s = 100000 day
bull GRB 1day (BATSE) = 1000day
bull GRB rate = 1 of SN rate
bull maybe more collapsars than GRBs
bull =gt more rapidly rotating SN
bull SN with collapsar engine
bull look for bright Type Ic (w broad lines)
SN GW
bull SN1998bwGRB980425
bull 40 Mpc
bull maybe dominant GRB
bull rapid rotaters
bull SNAPROTSE look for 1998bw 2003dh like SN
bull many light curves -gt better t_explode
Implications
bull Probe engine directly
bull collapse duration vs GRB duration
bull collapseGRB delay (internal vs external)
bull disk properties ndash low viscosity big disks
Issues
bull too much j =gt no GRB but bright GW
bull may need low metallicity for GRB
bull prefer high redshift
bull donrsquot know nearby rate
bull but 980425 may imply rate is high
bull look for weak GRBs like 980425
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
With decreasing metallicity the bindingenergy of the core and the size of the silicon core both increase making black hole formation more likely atlow metallicity Woosley Heger amp Weaver RMP (2002)
Black hole formation may be unavoidable for low metallicity
Solar metallicity
Low metallicity
In the absence of mass lossand magnetic fields there wouldbe abundant progenitors
Unfortunately nature has both
15 solar mass helium core born rotating rigidly at f times break up
The more difficult problem is the angular momentum Thisis a problem shared by all current GRB models that invokemassive stars
- What is a Gamma-Ray Burst
- Superbowl Burst
- Slide 3
- 135 models (1993)
- Slide 5
- Slide 6
- Slide 7
- GRB991121
- GRB030329SN2003DH
- Slide 10
- Slide 11
- Slide 12
- GRB central engine
- ldquoDelayedrdquo SN Explosion
- Pre-Supernova Density Structure
- Failure of delayed mechanism
- Stellar Rotation
- Slide 18
- Slide 19
- Collapsar Simulations
- Collapsar Disk Animation
- Disk Formation Movie
- Slide 23
- Slide 24
- Slide 25
- Collapsar results
- Slide 27
- Jet Birth
- Relativistic Jet Movie
- Collapsar stages
- Slide 31
- Slide 32
- Nickel Wind Movie
- Slide 34
- Slide 35
- Slide 36
- Slide 37
- Slide 38
- Collapsars
- GRBGW
- Rates
- SN GW
- Implications
- Issues
- Principle Results
- Slide 46
- Slide 47
-
Collapsars
bull Can make ldquolongrdquo GRBs in H stripped (WR) stars tengine gt tescape
bull Short bursts may be compact binary mergersbull Need SN failure amp angular momentum
ndash Low metallicity binary can help
bull Star can explode -gt SN if nickel is made Predicts GRBSN association Type Ibc
bull SNGRB ratio may depend on angular momentumbull ldquoNickel windrdquo can explode star -gt hypernova
ndash H env Type II (no GRB) no H Type I + GRB
GRBGW bull Long GRBs
ndash not brighter than SN in GW
ndash very far Gpc
ndash very rare lt 1 SN
bull Short GBsndash merging ns-bh binaries
ndash maybe closer than long bursts
ndash short delay between event and GRB
ndash good for SWIFTLIGO
Rates
bull SN 1s = 100000 day
bull GRB 1day (BATSE) = 1000day
bull GRB rate = 1 of SN rate
bull maybe more collapsars than GRBs
bull =gt more rapidly rotating SN
bull SN with collapsar engine
bull look for bright Type Ic (w broad lines)
SN GW
bull SN1998bwGRB980425
bull 40 Mpc
bull maybe dominant GRB
bull rapid rotaters
bull SNAPROTSE look for 1998bw 2003dh like SN
bull many light curves -gt better t_explode
Implications
bull Probe engine directly
bull collapse duration vs GRB duration
bull collapseGRB delay (internal vs external)
bull disk properties ndash low viscosity big disks
Issues
bull too much j =gt no GRB but bright GW
bull may need low metallicity for GRB
bull prefer high redshift
bull donrsquot know nearby rate
bull but 980425 may imply rate is high
bull look for weak GRBs like 980425
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
With decreasing metallicity the bindingenergy of the core and the size of the silicon core both increase making black hole formation more likely atlow metallicity Woosley Heger amp Weaver RMP (2002)
Black hole formation may be unavoidable for low metallicity
Solar metallicity
Low metallicity
In the absence of mass lossand magnetic fields there wouldbe abundant progenitors
Unfortunately nature has both
15 solar mass helium core born rotating rigidly at f times break up
The more difficult problem is the angular momentum Thisis a problem shared by all current GRB models that invokemassive stars
- What is a Gamma-Ray Burst
- Superbowl Burst
- Slide 3
- 135 models (1993)
- Slide 5
- Slide 6
- Slide 7
- GRB991121
- GRB030329SN2003DH
- Slide 10
- Slide 11
- Slide 12
- GRB central engine
- ldquoDelayedrdquo SN Explosion
- Pre-Supernova Density Structure
- Failure of delayed mechanism
- Stellar Rotation
- Slide 18
- Slide 19
- Collapsar Simulations
- Collapsar Disk Animation
- Disk Formation Movie
- Slide 23
- Slide 24
- Slide 25
- Collapsar results
- Slide 27
- Jet Birth
- Relativistic Jet Movie
- Collapsar stages
- Slide 31
- Slide 32
- Nickel Wind Movie
- Slide 34
- Slide 35
- Slide 36
- Slide 37
- Slide 38
- Collapsars
- GRBGW
- Rates
- SN GW
- Implications
- Issues
- Principle Results
- Slide 46
- Slide 47
-
GRBGW bull Long GRBs
ndash not brighter than SN in GW
ndash very far Gpc
ndash very rare lt 1 SN
bull Short GBsndash merging ns-bh binaries
ndash maybe closer than long bursts
ndash short delay between event and GRB
ndash good for SWIFTLIGO
Rates
bull SN 1s = 100000 day
bull GRB 1day (BATSE) = 1000day
bull GRB rate = 1 of SN rate
bull maybe more collapsars than GRBs
bull =gt more rapidly rotating SN
bull SN with collapsar engine
bull look for bright Type Ic (w broad lines)
SN GW
bull SN1998bwGRB980425
bull 40 Mpc
bull maybe dominant GRB
bull rapid rotaters
bull SNAPROTSE look for 1998bw 2003dh like SN
bull many light curves -gt better t_explode
Implications
bull Probe engine directly
bull collapse duration vs GRB duration
bull collapseGRB delay (internal vs external)
bull disk properties ndash low viscosity big disks
Issues
bull too much j =gt no GRB but bright GW
bull may need low metallicity for GRB
bull prefer high redshift
bull donrsquot know nearby rate
bull but 980425 may imply rate is high
bull look for weak GRBs like 980425
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
With decreasing metallicity the bindingenergy of the core and the size of the silicon core both increase making black hole formation more likely atlow metallicity Woosley Heger amp Weaver RMP (2002)
Black hole formation may be unavoidable for low metallicity
Solar metallicity
Low metallicity
In the absence of mass lossand magnetic fields there wouldbe abundant progenitors
Unfortunately nature has both
15 solar mass helium core born rotating rigidly at f times break up
The more difficult problem is the angular momentum Thisis a problem shared by all current GRB models that invokemassive stars
- What is a Gamma-Ray Burst
- Superbowl Burst
- Slide 3
- 135 models (1993)
- Slide 5
- Slide 6
- Slide 7
- GRB991121
- GRB030329SN2003DH
- Slide 10
- Slide 11
- Slide 12
- GRB central engine
- ldquoDelayedrdquo SN Explosion
- Pre-Supernova Density Structure
- Failure of delayed mechanism
- Stellar Rotation
- Slide 18
- Slide 19
- Collapsar Simulations
- Collapsar Disk Animation
- Disk Formation Movie
- Slide 23
- Slide 24
- Slide 25
- Collapsar results
- Slide 27
- Jet Birth
- Relativistic Jet Movie
- Collapsar stages
- Slide 31
- Slide 32
- Nickel Wind Movie
- Slide 34
- Slide 35
- Slide 36
- Slide 37
- Slide 38
- Collapsars
- GRBGW
- Rates
- SN GW
- Implications
- Issues
- Principle Results
- Slide 46
- Slide 47
-
Rates
bull SN 1s = 100000 day
bull GRB 1day (BATSE) = 1000day
bull GRB rate = 1 of SN rate
bull maybe more collapsars than GRBs
bull =gt more rapidly rotating SN
bull SN with collapsar engine
bull look for bright Type Ic (w broad lines)
SN GW
bull SN1998bwGRB980425
bull 40 Mpc
bull maybe dominant GRB
bull rapid rotaters
bull SNAPROTSE look for 1998bw 2003dh like SN
bull many light curves -gt better t_explode
Implications
bull Probe engine directly
bull collapse duration vs GRB duration
bull collapseGRB delay (internal vs external)
bull disk properties ndash low viscosity big disks
Issues
bull too much j =gt no GRB but bright GW
bull may need low metallicity for GRB
bull prefer high redshift
bull donrsquot know nearby rate
bull but 980425 may imply rate is high
bull look for weak GRBs like 980425
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
With decreasing metallicity the bindingenergy of the core and the size of the silicon core both increase making black hole formation more likely atlow metallicity Woosley Heger amp Weaver RMP (2002)
Black hole formation may be unavoidable for low metallicity
Solar metallicity
Low metallicity
In the absence of mass lossand magnetic fields there wouldbe abundant progenitors
Unfortunately nature has both
15 solar mass helium core born rotating rigidly at f times break up
The more difficult problem is the angular momentum Thisis a problem shared by all current GRB models that invokemassive stars
- What is a Gamma-Ray Burst
- Superbowl Burst
- Slide 3
- 135 models (1993)
- Slide 5
- Slide 6
- Slide 7
- GRB991121
- GRB030329SN2003DH
- Slide 10
- Slide 11
- Slide 12
- GRB central engine
- ldquoDelayedrdquo SN Explosion
- Pre-Supernova Density Structure
- Failure of delayed mechanism
- Stellar Rotation
- Slide 18
- Slide 19
- Collapsar Simulations
- Collapsar Disk Animation
- Disk Formation Movie
- Slide 23
- Slide 24
- Slide 25
- Collapsar results
- Slide 27
- Jet Birth
- Relativistic Jet Movie
- Collapsar stages
- Slide 31
- Slide 32
- Nickel Wind Movie
- Slide 34
- Slide 35
- Slide 36
- Slide 37
- Slide 38
- Collapsars
- GRBGW
- Rates
- SN GW
- Implications
- Issues
- Principle Results
- Slide 46
- Slide 47
-
SN GW
bull SN1998bwGRB980425
bull 40 Mpc
bull maybe dominant GRB
bull rapid rotaters
bull SNAPROTSE look for 1998bw 2003dh like SN
bull many light curves -gt better t_explode
Implications
bull Probe engine directly
bull collapse duration vs GRB duration
bull collapseGRB delay (internal vs external)
bull disk properties ndash low viscosity big disks
Issues
bull too much j =gt no GRB but bright GW
bull may need low metallicity for GRB
bull prefer high redshift
bull donrsquot know nearby rate
bull but 980425 may imply rate is high
bull look for weak GRBs like 980425
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
With decreasing metallicity the bindingenergy of the core and the size of the silicon core both increase making black hole formation more likely atlow metallicity Woosley Heger amp Weaver RMP (2002)
Black hole formation may be unavoidable for low metallicity
Solar metallicity
Low metallicity
In the absence of mass lossand magnetic fields there wouldbe abundant progenitors
Unfortunately nature has both
15 solar mass helium core born rotating rigidly at f times break up
The more difficult problem is the angular momentum Thisis a problem shared by all current GRB models that invokemassive stars
- What is a Gamma-Ray Burst
- Superbowl Burst
- Slide 3
- 135 models (1993)
- Slide 5
- Slide 6
- Slide 7
- GRB991121
- GRB030329SN2003DH
- Slide 10
- Slide 11
- Slide 12
- GRB central engine
- ldquoDelayedrdquo SN Explosion
- Pre-Supernova Density Structure
- Failure of delayed mechanism
- Stellar Rotation
- Slide 18
- Slide 19
- Collapsar Simulations
- Collapsar Disk Animation
- Disk Formation Movie
- Slide 23
- Slide 24
- Slide 25
- Collapsar results
- Slide 27
- Jet Birth
- Relativistic Jet Movie
- Collapsar stages
- Slide 31
- Slide 32
- Nickel Wind Movie
- Slide 34
- Slide 35
- Slide 36
- Slide 37
- Slide 38
- Collapsars
- GRBGW
- Rates
- SN GW
- Implications
- Issues
- Principle Results
- Slide 46
- Slide 47
-
Implications
bull Probe engine directly
bull collapse duration vs GRB duration
bull collapseGRB delay (internal vs external)
bull disk properties ndash low viscosity big disks
Issues
bull too much j =gt no GRB but bright GW
bull may need low metallicity for GRB
bull prefer high redshift
bull donrsquot know nearby rate
bull but 980425 may imply rate is high
bull look for weak GRBs like 980425
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
With decreasing metallicity the bindingenergy of the core and the size of the silicon core both increase making black hole formation more likely atlow metallicity Woosley Heger amp Weaver RMP (2002)
Black hole formation may be unavoidable for low metallicity
Solar metallicity
Low metallicity
In the absence of mass lossand magnetic fields there wouldbe abundant progenitors
Unfortunately nature has both
15 solar mass helium core born rotating rigidly at f times break up
The more difficult problem is the angular momentum Thisis a problem shared by all current GRB models that invokemassive stars
- What is a Gamma-Ray Burst
- Superbowl Burst
- Slide 3
- 135 models (1993)
- Slide 5
- Slide 6
- Slide 7
- GRB991121
- GRB030329SN2003DH
- Slide 10
- Slide 11
- Slide 12
- GRB central engine
- ldquoDelayedrdquo SN Explosion
- Pre-Supernova Density Structure
- Failure of delayed mechanism
- Stellar Rotation
- Slide 18
- Slide 19
- Collapsar Simulations
- Collapsar Disk Animation
- Disk Formation Movie
- Slide 23
- Slide 24
- Slide 25
- Collapsar results
- Slide 27
- Jet Birth
- Relativistic Jet Movie
- Collapsar stages
- Slide 31
- Slide 32
- Nickel Wind Movie
- Slide 34
- Slide 35
- Slide 36
- Slide 37
- Slide 38
- Collapsars
- GRBGW
- Rates
- SN GW
- Implications
- Issues
- Principle Results
- Slide 46
- Slide 47
-
Issues
bull too much j =gt no GRB but bright GW
bull may need low metallicity for GRB
bull prefer high redshift
bull donrsquot know nearby rate
bull but 980425 may imply rate is high
bull look for weak GRBs like 980425
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
With decreasing metallicity the bindingenergy of the core and the size of the silicon core both increase making black hole formation more likely atlow metallicity Woosley Heger amp Weaver RMP (2002)
Black hole formation may be unavoidable for low metallicity
Solar metallicity
Low metallicity
In the absence of mass lossand magnetic fields there wouldbe abundant progenitors
Unfortunately nature has both
15 solar mass helium core born rotating rigidly at f times break up
The more difficult problem is the angular momentum Thisis a problem shared by all current GRB models that invokemassive stars
- What is a Gamma-Ray Burst
- Superbowl Burst
- Slide 3
- 135 models (1993)
- Slide 5
- Slide 6
- Slide 7
- GRB991121
- GRB030329SN2003DH
- Slide 10
- Slide 11
- Slide 12
- GRB central engine
- ldquoDelayedrdquo SN Explosion
- Pre-Supernova Density Structure
- Failure of delayed mechanism
- Stellar Rotation
- Slide 18
- Slide 19
- Collapsar Simulations
- Collapsar Disk Animation
- Disk Formation Movie
- Slide 23
- Slide 24
- Slide 25
- Collapsar results
- Slide 27
- Jet Birth
- Relativistic Jet Movie
- Collapsar stages
- Slide 31
- Slide 32
- Nickel Wind Movie
- Slide 34
- Slide 35
- Slide 36
- Slide 37
- Slide 38
- Collapsars
- GRBGW
- Rates
- SN GW
- Implications
- Issues
- Principle Results
- Slide 46
- Slide 47
-
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
With decreasing metallicity the bindingenergy of the core and the size of the silicon core both increase making black hole formation more likely atlow metallicity Woosley Heger amp Weaver RMP (2002)
Black hole formation may be unavoidable for low metallicity
Solar metallicity
Low metallicity
In the absence of mass lossand magnetic fields there wouldbe abundant progenitors
Unfortunately nature has both
15 solar mass helium core born rotating rigidly at f times break up
The more difficult problem is the angular momentum Thisis a problem shared by all current GRB models that invokemassive stars
- What is a Gamma-Ray Burst
- Superbowl Burst
- Slide 3
- 135 models (1993)
- Slide 5
- Slide 6
- Slide 7
- GRB991121
- GRB030329SN2003DH
- Slide 10
- Slide 11
- Slide 12
- GRB central engine
- ldquoDelayedrdquo SN Explosion
- Pre-Supernova Density Structure
- Failure of delayed mechanism
- Stellar Rotation
- Slide 18
- Slide 19
- Collapsar Simulations
- Collapsar Disk Animation
- Disk Formation Movie
- Slide 23
- Slide 24
- Slide 25
- Collapsar results
- Slide 27
- Jet Birth
- Relativistic Jet Movie
- Collapsar stages
- Slide 31
- Slide 32
- Nickel Wind Movie
- Slide 34
- Slide 35
- Slide 36
- Slide 37
- Slide 38
- Collapsars
- GRBGW
- Rates
- SN GW
- Implications
- Issues
- Principle Results
- Slide 46
- Slide 47
-
With decreasing metallicity the bindingenergy of the core and the size of the silicon core both increase making black hole formation more likely atlow metallicity Woosley Heger amp Weaver RMP (2002)
Black hole formation may be unavoidable for low metallicity
Solar metallicity
Low metallicity
In the absence of mass lossand magnetic fields there wouldbe abundant progenitors
Unfortunately nature has both
15 solar mass helium core born rotating rigidly at f times break up
The more difficult problem is the angular momentum Thisis a problem shared by all current GRB models that invokemassive stars
- What is a Gamma-Ray Burst
- Superbowl Burst
- Slide 3
- 135 models (1993)
- Slide 5
- Slide 6
- Slide 7
- GRB991121
- GRB030329SN2003DH
- Slide 10
- Slide 11
- Slide 12
- GRB central engine
- ldquoDelayedrdquo SN Explosion
- Pre-Supernova Density Structure
- Failure of delayed mechanism
- Stellar Rotation
- Slide 18
- Slide 19
- Collapsar Simulations
- Collapsar Disk Animation
- Disk Formation Movie
- Slide 23
- Slide 24
- Slide 25
- Collapsar results
- Slide 27
- Jet Birth
- Relativistic Jet Movie
- Collapsar stages
- Slide 31
- Slide 32
- Nickel Wind Movie
- Slide 34
- Slide 35
- Slide 36
- Slide 37
- Slide 38
- Collapsars
- GRBGW
- Rates
- SN GW
- Implications
- Issues
- Principle Results
- Slide 46
- Slide 47
-
In the absence of mass lossand magnetic fields there wouldbe abundant progenitors
Unfortunately nature has both
15 solar mass helium core born rotating rigidly at f times break up
The more difficult problem is the angular momentum Thisis a problem shared by all current GRB models that invokemassive stars
- What is a Gamma-Ray Burst
- Superbowl Burst
- Slide 3
- 135 models (1993)
- Slide 5
- Slide 6
- Slide 7
- GRB991121
- GRB030329SN2003DH
- Slide 10
- Slide 11
- Slide 12
- GRB central engine
- ldquoDelayedrdquo SN Explosion
- Pre-Supernova Density Structure
- Failure of delayed mechanism
- Stellar Rotation
- Slide 18
- Slide 19
- Collapsar Simulations
- Collapsar Disk Animation
- Disk Formation Movie
- Slide 23
- Slide 24
- Slide 25
- Collapsar results
- Slide 27
- Jet Birth
- Relativistic Jet Movie
- Collapsar stages
- Slide 31
- Slide 32
- Nickel Wind Movie
- Slide 34
- Slide 35
- Slide 36
- Slide 37
- Slide 38
- Collapsars
- GRBGW
- Rates
- SN GW
- Implications
- Issues
- Principle Results
- Slide 46
- Slide 47
-