gamma ray bursts: open issues brief history power short history of the paradigm: internal vs...
TRANSCRIPT
Gamma Ray Bursts: open Gamma Ray Bursts: open issuesissues
Brief historyBrief historyPowerPowerShort history of the paradigm: Short history of the paradigm:
internal vs external shocksinternal vs external shocksAfterglows: external shocksAfterglows: external shocksThe spectral-energy relationsThe spectral-energy relationsGRBs for cosmologyGRBs for cosmology
Gabriele Ghisellini – Osservatorio di Gabriele Ghisellini – Osservatorio di Brera Brera
Gamma-Ray Bursts: The story Gamma-Ray Bursts: The story beginsbegins
Treates banning nuclear tests between USA and USSR in early 60s
VELA Satellites: X and soft -ray detectors
Klebesadel R.W., Strong I.B., Olson R., 1973, Astrophysical Journal, 182, L85
`Observations of Gamma-Ray Bursts of Cosmic Origin’
Brief, intense Brief, intense flashes of flashes of -rays-rays
Shortest 6 msGRB 910711
Longest ~2000 sGRB 971208
Paciesas et al (2002)Briggs et al (2002) Koveliotou (2002)
SHORT LONG
Short – HardShort – Hard Long - SoftLong - Soft
Two flavours, long and Two flavours, long and shortshort
SpectraSpectra
Non thermal Non thermal spectraspectra
featureless continuumfeatureless continuum
power-laws - peak in power-laws - peak in FF F ~ E F ~ E
Epeak
1997: The BeppoSAX satellite
Slewing in several hoursSlewing in several hours
Italian-Dutch
“Satellite per l’ Astronomia X”
InstrumentsInstruments
Wide Field Cameras:Wide Field Cameras:
5% of sky – positioning ~ 5% of sky – positioning ~ 4’ 4’
+ +
Narrow Field InstrumentsNarrow Field Instruments
arcmin resolutionarcmin resolution
NFI
Discovery of first Discovery of first afterglow!afterglow!
GRB 28 9702
3 March3 March28 February28 February
Optical id. host galaxy: redshiftsOptical id. host galaxy: redshifts
Cosmological origin !
~120 / 3000 with z: <0.1 – 6.3~120 / 3000 with z: <0.1 – 6.3
(Batse, SAX, HETE-II, Integral, Swift, …) (Batse, SAX, HETE-II, Integral, Swift, …)
Huge Huge isotropicisotropic equivalent equivalent
energy!energy!
119 GRBs with 119 GRBs with zz
GRB typical Fluence GRB typical Fluence (i.e. time int. flux) is (i.e. time int. flux) is 1010-8 -8 – 10– 10-4 -4 erg/cmerg/cm2 2
(1keV – 10 MeV)(1keV – 10 MeV)
Assume Assume IsotropyIsotropy
Energy and PowerEnergy and Power
GRB are powerfulGRB are powerful
• AGN: L < 10AGN: L < 104848 erg/s erg/s• SN: L < 10SN: L < 104545 erg/s erg/s (in photons)(in photons)
• GRB: L < 10GRB: L < 105353 erg/s erg/s
Planck Planck power: power:
McMc22 cc55
RRgg/c /c GG
= = 3.6x10= = 3.6x105959 erg/s erg/s
“first light” & PopIII
chemical evolution
large scale structures
cover the epoch of re-ionization
Star Formation Rate
Probes of far universe
SNIa
Huge energyHuge energySmall VolumeSmall Volume
FireballFireball
Invented even before knowing that GRBs are Invented even before knowing that GRBs are cosmological….cosmological….
A short history of fireballsA short history of fireballs
19781978 Cavallo & Rees: fireball: photons trapped by their own Cavallo & Rees: fireball: photons trapped by their own pairs pairs
19781978 Rees: internal shocks in M87 to transport energy along Rees: internal shocks in M87 to transport energy along the jetthe jet
19861986 Paczynski: Cosmological GRB Paczynski: Cosmological GRB L=10 L=105151 erg/s and T~1 erg/s and T~1 MeV MeV
19861986 Goodman: T Goodman: Tobsobs remains T during expansion. Doppler remains T during expansion. Doppler
balances adiabatic cooling balances adiabatic cooling
19921992 Pure fireball made by Pure fireball made by e+e- . Focussing by e+e- . Focussing by gravitationgravitation
NS
e+e-
A short history of fireballsA short history of fireballs
19781978 Cavallo & Rees: fireball: photons trapped by their own Cavallo & Rees: fireball: photons trapped by their own pairs pairs
19781978 Rees: internal shocks in M87 to transport energy along Rees: internal shocks in M87 to transport energy along the jetthe jet
19861986 Paczynski: Cosmological GRB Paczynski: Cosmological GRB L=10 L=105151 erg/s and T~1 erg/s and T~1 MeV MeV
19861986 Goodman: T Goodman: Tobsobs remains T during expansion. Doppler remains T during expansion. Doppler
balances adiabatic cooling balances adiabatic cooling
19921992 Pure fireball made by Pure fireball made by e+e- . Focussing by e+e- . Focussing by gravitationgravitation
19921992 Dirty fireball polluted by baryons. Re-conversion of Dirty fireball polluted by baryons. Re-conversion of bulk kinetic into radiation through shocks with external bulk kinetic into radiation through shocks with external mediummedium
19941994 Internal shocks due to shells moving with different Internal shocks due to shells moving with different
Why internal shocks?Why internal shocks?
Spikes have Spikes have same same durationduration
A process A process that that repeats repeats itselfitself
Relativ. eRelativ. e-- + B: + B: synchrotron??synchrotron??
Relativ. eRelativ. e-- + + B: B:
synchrotronsynchrotron
Shell still opaqueShell still opaque
““The” model:The” model:Internal/ExternInternal/Extern
al Shocksal ShocksRees-Meszaros-Piran
ProgenitProgenitorsors
Host galaxiesHost galaxiesFaint (mFaint (mRR ~ 25 ) galaxies~ 25 ) galaxiesSites of star formation Sites of star formation Low metallicitiesLow metallicities
Blo
om
et a
l. 20
02
GRBs associated with SN (Ib,c) GRBs associated with SN (Ib,c)
SN
afterglow
Math
eson
et a
l. 20
03
Afterglow re-brightening Afterglow re-brightening A few spectroscopic ident. (underluminous?)A few spectroscopic ident. (underluminous?)
ProgenitorsProgenitors
core collapse of massive stars (M > 30 Msun) long GRBs Collapsar or Hypernova (MacFadyen &
Woosley 1999) GRB simultaneous with SN
Supranova – two-step collapse (Vietri & Stella 1998)
GRB delayed by few months-years
Discriminants: host galaxies, location within host, duration, environment, redshift distribution, ...
compact object mergers (NS-NS, NS-BH) short GRBs
?
The engineThe engine
Accreting torus
Formation of a spinning BH + dense Formation of a spinning BH + dense torus, sustaining B ~ 10torus, sustaining B ~ 101414-10-101515 G G
Extraction BH spin energy (0.29 Extraction BH spin energy (0.29 MMBHBHcc22))
Extract E > 10Extract E > 105252 erg erg
ttGRBGRB ~ 10 ~ 1044 t tdyndyn
JetsJets
Jet half opening
angle
Jet effectJet effect
, Surf.
Relativistc beaming:
emitting surface
1/
1/1/
Log(t)
Log(F)
Jet Jet breakbreak
>> 1/
Israel et al. 1999
GRB Jet measureGRB Jet measure
“Jet break”
Jet break time tbreak
Jet opening angle
““True” energeticsTrue” energeticsFra
il e
t al.
2001
Isotropic equivalent Isotropic equivalent energyenergy
EEtruetrue = E = Eiso iso (1 – cos (1 – cos ))
Blo
om
et
al.
2003
EE peakpeak
was n
ot
was n
ot
consid
e
consid
e
red…
red…
Am
ati
et
al.
2002
Am
ati
et
al.
2002
9+2 BeppoSAX GRBs
EE peak
peak
E E
iso
iso
0.5
0.5
Peak energy – Isotropic energy Peak energy – Isotropic energy CorrelationCorrelation
EEp
eak
peak(1
+z
(1+
z))
Nava e
t al.
2006;
Gh
irla
nd
a e
t al.
2007
Nava e
t al.
2006;
Gh
irla
nd
a e
t al.
2007
“Am
ati”
(62)
“Ghi
rlan
da”
(25)
1- cos 1- cos jetjet
Gh
irla
nd
a,
Gh
isellin
i, L
azzati
& F
irm
an
i 2004
Gh
irla
nd
a,
Gh
isellin
i, L
azzati
& F
irm
an
i 2004
Lu
min
osit
y
Lu
min
osit
y
dis
tan
ce
dis
tan
ce
redshiftredshiftGRBs can b
e use
d as c
osmolo
gical
GRBs can b
e use
d as c
osmolo
gical
RULERS !
RULERS !
Supernovae
GRBsGRBs
Problems:Problems: 1: Efficiency 1: Efficiency
Efficiency=Radiated/total energyEfficiency=Radiated/total energyOnly the RELATIVE kinetic energy can be used!Only the RELATIVE kinetic energy can be used!
Shells of Shells of equal equal massesmasses
Shells of Shells of equal equal energiesenergies
final final ~ (~ (1122))1/21/2
Dyn
am
ical effi
cie
ncy
(%)
5%
Pir
o a
str
o-p
h/0
001436
Pir
o a
str
o-p
h/0
001436
A lot of kinetic energy should remain to power the A lot of kinetic energy should remain to power the afterglowafterglow
SAX X-ray SAX X-ray afterglow afterglow light curvelight curve
PromptPrompt
Willin
gale
et
al.
W
illin
gale
et
al.
2007
2007
SWIFTSWIFT
EEafterglowafterglow < E < Epromptprompt
EE afterg
low
afterg
low ~
0.1 E
~ 0.1 E pro
mpt
prompt
Problems:Problems:2: Early 2: Early
“afterglow”“afterglow”
Good old timesGood old timesP
iro a
str
o-p
h/0
001436
Pir
o a
str
o-p
h/0
001436
Now: a messNow: a mess
GRB 050904GRB 050904
z=6.29z=6.29
Pan
ait
escu
2006
Pan
ait
escu
2006
XX
OptOpt..
X-ray and optical behave X-ray and optical behave differentlydifferently
X-rays: X-rays: steep-flat-steep-flat-
steepsteep
TA
Is this “real” afte
rglow? i.e. e
xternal
Is this “real” afte
rglow? i.e. e
xternal
shock?
shock?
Early (normal) prompt: Early (normal) prompt: >>1/j
Late prompt: Late prompt: >1/j
Late prompt: Late prompt: =1/j
Late prompt: Late prompt: <1/j
”real” after-glow
Ghisellini et al. Ghisellini et al. 20072007
Long lasting engine??Long lasting engine??
• RRss/c ~ 10/c ~ 10-4-4 s (for a 10 solar mass s (for a 10 solar mass
BH)BH)• Even 10 s are 10Even 10 s are 1055 dynamical times dynamical times• Two-phase accretion? Two-phase accretion?
ConclusionsConclusions
““Paradigm”: internal+external shocks, Paradigm”: internal+external shocks, synchrotron for both: synchrotron for both: it helps, but it it helps, but it is limitingis limiting
Efficiency is an issueEfficiency is an issue
Progenitors for long: done. For short: Progenitors for long: done. For short: not yetnot yet
Central engine? How long does it live?Central engine? How long does it live?
GRBs as probes of the far universe GRBs as probes of the far universe (continue…)(continue…)
There can be a Black Body … butThere can be a Black Body … but
Time resolved Time resolved spectraspectra
Time integrated Time integrated spectrumspectrum
The same The same occurs for ALL occurs for ALL GRBs detected GRBs detected by BATSE and by BATSE and with WFCwith WFCG
hir
lan
da e
t al.
G
hir
lan
da e
t al.
2007b
2007b
MemoryMemory
Epeak
=509 keV
Epeak
=503 keV Epeak
= 416 keV
Time [sec]
cts/sec
Epeak
= 390 keV
EF(E)
EF(E)
EF(E)
GRB spectrum evolves with time within GRB spectrum evolves with time within single burstssingle bursts
Ghirlanda PhD Ghirlanda PhD thesisthesis
phot
/cm
^2 s
ec
Hard to Soft Hard to Soft evolutionevolution
Epe
ak
Epeak
, t), t)
Decrease Decrease independent of the independent of the rise and decay of rise and decay of the fluxthe flux
Epeak
time
Tracking Tracking evolutionevolution
Photon Photon fluxflux
Correlated with
EEpeakpeak(t)(t), , (t) (t) ,,(t)(t)
By construction, internal shocks By construction, internal shocks should all be equal.should all be equal.
Then, why does the spectrum Then, why does the spectrum evolve?evolve?
SpectraSpectraSpectra
Fis
hm
an
& M
eeg
an
1995
Fis
hm
an
& M
eeg
an
1995
EEpeakpeak
Prompt Prompt radiation: radiation:
Synchrotron?Synchrotron?
Energy spectrum of a cooling electronEnergy spectrum of a cooling electron
Fast cooling Fast cooling + synchro: + synchro:
E() -1/2
N() -3/2
Typical synchrotron Typical synchrotron frequencyfrequency
synsyn = 3.6x10 = 3.6x1066BB22/(1+z)/(1+z)HzHz
Magnetic field from: Magnetic field from:
LLB B = = BBLLkinkin R R2222BB22c = c = BBLLshellshell
Size from:Size from:
R ~ RR ~ R002 2 (internal shock) (internal shock)
Electron energy from: Electron energy from:
mmeecc22==eemmppcc22((’-1) ~ ’-1) ~ eemmppcc22
B B LLshellshell
RR00
BB ~
1/21/2 1/21/2
~ ~ eemmpp/m/mee
Synchrotron Synchrotron -ray -ray emission?emission?
BB ee LLkin,shell,50kin,shell,50hhsynsyn ~ 400 ~ 400
keV keV
1/21/2 22 1/21/2
33 RR0,70,7 (1+z)(1+z)2
ttcoolcool ~ 10 ~ 10--
77
ee ( (/100)/100)
MeVMeV22
33
secsec
Extremely short - No way to make it longer
tcool << tdynamical ~ 10-2 sec
It must be short, if not, how can the flux vary?
0.2 0.2 msms
More than More than exponentialexponential
-2 -1 0 1 Low energy photon power law index N(E) =
kE-P
reece e
t al.
FF ~ ~ 1/31/3
FF ~ ~ -1/2-1/2
Can it be rescued Can it be rescued by:by:
Reacceleration?Reacceleration? NoNo, in ISS e- are , in ISS e- are accelerated only onceaccelerated only once
Adiabatic losses?Adiabatic losses? NoNo, too small , too small regions would be involved, too regions would be involved, too much ICmuch IC
Self absorption?Self absorption? NoNo, lots of e- , lots of e- needed, too much ICneeded, too much IC
Self Compton?Self Compton? NoNo, t, tcoolcool too small too small
even in this caseeven in this case
Clustering of the Clustering of the optical optical
luminositiesluminosities
Flux vs observed timeFlux vs observed time
=0.48=0.48
Nard
ini et
al.
2006
Nard
ini et
al.
2006
Luminosity vs rest frame Luminosity vs rest frame titimmee=0.28=0.28
Nard
ini et
al.
2006
Nard
ini et
al.
2006
Swift GRBsSwift GRBs
332121
552727
Pre-SwiftPre-Swift
+Swift+Swift
Dark??Dark??
Lx @ 12 Lx @ 12 hhoouurrss
pre-Swift (19)pre-Swift (19)
Including Including SSwwiifftt
(30)(30)
G1=100, G2=200G1=100, G2=200
Thompson, Meszaros & Rees 2007Thompson, Meszaros & Rees 2007
At R ~ RAt R ~ Rstarstar the fireball dissipates part of the fireball dissipates part of
its energy its energy BB BB
L ~L ~ 22 LLisoiso 22 ~ L/L ~ L/Lisoiso
LLisoiso ~ R ~ R22 22 T’ T’4 4
~ (~ (R/R/22 T T44
LLisoiso ~ R ~ R22 (L /L (L /Lisoiso)T)T
4 4 EEpeakpeak ~ L ~ Lisoiso1/21/2LL-1/4-1/4
A short history of fireballsA short history of fireballs
Short BurstsShort Bursts
The spectrum of short The spectrum of short burstsbursts
harder softer
Log Epeak Log Log Epeak Log
short
long
Gh
irla
nd
a e
t al.
2004
harder becausebecause
is harder, Epeak is
the same or even smaller
DensityDensity
Star forming regions are Star forming regions are densedense
GRB – Afterglow – Temporal PropertiesGRB emission in X, GRB emission in X, OpticalOpticalPanaitescu &
Kumar
Why densities a
re so
Why densities a
re so
small?
small?
Fir
man
i et
al.
2004
LL-1.5+-0.05-1.5+-0.05
No corr.No corr.
LLxx > L > Loptopt
LLoptopt more clustered than L more clustered than Lxx
vvcc between optical and X-rays between optical and X-rays
~same values of ~same values of BB, , ee, E, Ek,isok,iso
moderate cooling (small moderate cooling (small BB))
large Comptonization y large Comptonization y paraparametermeter
different pdifferent p
Universal energy Universal energy reservoir?reservoir?
Blo
om
et
al.
2003
Blo
om
et
al.
2003
Fra
il e
t al.
2001
Fra
il e
t al.
2001 Best n Best n
from fitsfrom fits
Fra
il e
t al.
Fra
il e
t al.
2001
2001
Fra
il e
t al.
2001
Same energy, different Same energy, different angles?angles?
Structured jetsStructured jets
viewview
jetjet
E()=const
E()=E0-2 L) = kLL) = kL-2-2
Universal EUniversal Epeakpeak??
Pre
ece e
t al.
~200 keV, ~200 keV, observerobserver frame frame
BATSEBATSE
HETE IIHETE II
X-ray fl
ashes
X-ray fl
ashes
Am
ati
et
al.
+Lam
b e
t A
mati
et
al.
+Lam
b e
t al.
al.
The “Amati et al.” relationThe “Amati et al.” relation
EEpeakpeak = 100 keV = 100 keV
EEiso,52 iso,52
++
EEisoiso = E = Etruetrue//22
EEpeakpeak = 1/ = 1/
1/21/2