The endpoint of massive stars in binaries: singlets, doublets?

Triplets!Maurice HPM van Putten

MIT-LIGO

Kerr Fest, August 26-28 2004, Christchurch, NZ

Amir Levinson (TAU)Eve C. Ostriker (Maryland)Tania Regimbau (CNRS,Nice)Hyun Kyu Lee (Hanyang)Michele Punturo (Virgo,INFN)Gregory M. Harry (MIT-LIGO)David Coward (UWA)Ronald Burman (UWA)

M.H.P.M. van Putten, A. Levinson, H.-K. Lee, T. Regimbau, M. Puntoro, G.M. Harry, Phys. Rev. D., 69, 044007

LIGO

LIGO

BATSE Group, NASAhttp://image.gsfc.nasa.gov/docs/science/know_l1/bursts.html

Vela/Konus (1963-1979)

Vela GRB670702 (Klebesadel & Olson)

LIGO

LIGO BATSE on CGRO (1991-2000)

LIGO

Beppo-Sax (Italian-Dutch, 1996-2002) LIGO

X-ray and optical transients toGRB970228 z=0.695

E. Costa et al. Nature 1997

J. van Paradijs et al. Nature 1997

were PREDICTED, confirming shocked fireball models or ultrarelativistic ejecta from compact sources

Paczynski and Rhoads 1993Katz 1994Rees and Meszaros 1993

Geometrical beamingLIGO

t

jj/1

j/1

E1E2E3

L

Harrison et al. 1999 Frail et al. 2001

E52-54

Harrison et al. 1999

Beaming factor about 500

E50-51

Frail et al. 2001

T. Galama et al. Nature 1998

Very dim GRB…No evidence of beaming…

GRB 980425/ SN1998bw

Stanek, K., et al., 2003Garnavich et al. 2003,Hjorth et al. 2003

GRB030329/SN2003dh(z=0.168, D=800Mpc)

GRB980425/SN1998bw (z=0.008, D=37Mpc)

GRB association to supernovae

GRBs are locked to the star-formation rate

2001) al.et (Frail 500/1 bf

0 1 2 3 4 50.0

0.1

0.2

0.3

0.4

0.5

pro

babi

lity

redshift z

observed simulated: observable simulated: total p

SFR2(z)

2003) Regimbau, &Putten (van 450 1/ rf

LIGO

Nomoto-Iwamoto-Suzuki sequence

Type IIb Type Ib Type Ic

(H-rich) (H-poor) (H,He-poor)

decreasing binary separation, removal of H-

and He-envelope

LIGO

Cappellaro, Barbon & Turatto 2003

Ia Ib/c II All

0.27(3) 0.11(3) 0.53(7) 0.91(8)

[1e-11 MSolar/100yr (H/75)^2]

SNIb/c about 1 in 5 SNII

LIGO

Porciani & Madau 20016obs 10)21()II Type SN(

)(GRB N

N

500450)GRB(

)(GRB

obs

true N

N Frail et al. 2001Van Putten & Regimbau 2001

310)42()Ib/c Type SN(

)(GRBtrue N

N

LIGO

Mirabel & Rodriques 1992

Active nuclei

LIGO

46.2

Van Putten 1996

B

Active nucleus

LIGO

“The bag”

Van Putten, Science, 1999

Bag of closed field-lines

Spin-connection by open field-lines

“turbulent shear flow in the torus resulting from the powerful torques

acting on it”

PSR+

PSR-

BH

PSR

H

Spin-up

PSR

0

Spin-down

Asy

mpto

tic

infinit

y

Spin-up and down of a torus by equivalence to PSRs

Suspended accretion: balance of competing torques on inner and outer face

van Putten & Ostriker 2001, van Putten & Levinson, 2003

Open ergotube subtended by black hole-event horizon

LIGO

van Putten Phys. Rep. 2001, van Putten & Levinson, 2003

Spin-orbit coupling to charged particles

eAJ

B

H

van Putten, 2000, PRL, 84, 3752; 2004, subm.

JE Frame-dragging * angular momentum

INT Workshop July 12-14 2004, Seattle

van Putten, 2000, PRL, 84, 3752; 2004, subm.

2

3215

47

/)(4

erg10

Hb

Mb

H

HhBE

A no-boundary mechanism for ejection of blobs (‘pancakes’)

*loop) closed(*2

1AreaRiemann

Curvature-spin coupling

dbacd

efabef

R

c

bb

dababcd

dbacd

efabefc

dccd

abab

uusRu

u

wRusR

usTAreaS

2

1

:With

2

1

2

1

/

<Wedge term>=0

Papapetrou (1951), Pirani (1956)

Spin-curvature coupling

Integral of force by curvature-spin coupling

JE

van Putten & Levinson, 2003

R

M

E

EHH

rot

j 2

1 4

Continuous Jet

erg103][

1.030.0erg104][

50

max

3/850

observedE

E

EtheoryE

rot

rot

In the Poynting-flux dominated limit of

Blandford-Znajek 1977

March 8 2002

Van Putten& Levinson

2002

LIGO

M

m

ab

m=1

Ma

mb

m

m=2

LIGO

•Theory of linear GWs agrees with obs to within 0.1% in PSR1913+16: Nobel Prize 1993

•Black-hole blob binary (b/a < 0.7506), blob-blob binary (b/a<0.3260): f=twice orbital frequency

b/a=0: Papaloizou-Pringle 1984; b/a>0: Van Putten 2002

HT

SolarHSolarirr

HSolargw

SolarHSolargw

MMMM

MMf

MMME

/

)7/)(1(2

)1.0/)(/500Hz(7

)1.0/)(7/(2.0

Modeling GRB-SNe from rotating black holes

LIGO

Plus torus winds and MeV neutrinos

Kerr line(J=M^2)

Disk line

Nucleation

Time Surge

Next?

Centered Nucleation

Van Putten, 2004

LIGO

Time

Radiatie spin-down against emission of GWs by spin-connection to non-axisymmetric torus

Synchronous BH-Torus spin

Spin-up or Spin-down

Spin-up by continuingaccretion (Bardeen 1970)

LIGO

binary period (dimensionless units)Van Putten, 2004

2

km/s100

2

km/s100.5%

10km/s)(GRB]SNIb/c[

2/3

10

2/1

cm10 s 30

kickkick

kick

Solar

off

v

vPR

r

M

Mt

Van Putten, 2004

Most Ib/c events decentered: failed GRBs!

Centered nucleation on free-fall time scale

Most black holes leave high-density core prematurely by Bekenstein’s gravitational radiation recoil mechanism (1973)

(XRFs?)

SNe with X-ray line-emissionsLIGO

1

11

1999) al.et (Hoeflich erg102]SN1998bw[

71.00.1erg102]theory[

51

251

SN

OSN

E

M

ME

1999) al.et (Hoeflich erg102]SN1998bw[

71.00.1erg102]theory[

51

251

SN

OSN

E

M

ME

Decentered Centered GRB Radiatively driven SN

Davies et al. 2002 van Putten et al. 2004

BIG MAC

‘‘ ’’29.0

~/ Hrot RE

The hunting of the snark (Lewis Carroll 1876)

Nutritional information

Serving size 1 Solar Mass

Serving size per pack 5-14

per serving per pack

Energy 6e46 J 4e47 J

Fat total 2e47 J 1e48 J

Sugars 0 0

All Else 0 0A Prime Quality New Zealand Product

Measuring nutritional content

BIG MAC

+ -

Voltage = angular velocityEnergy = angular velocity * angular momentum

Present: Measure voltages

VBATTERY

X-ray lines in disks

Wilms et al. 2001Fabian et al. 2002Miller et al. 2002, 2004Miniutti, Fabian and Miller 2004

Andy Fabian, this meeting

Soon: Perform calorimetry

BATTERY

Detect energy GWB in complete spin-down of KBH

Measure net temperature increase in water following complete discharge of battery

Van Putten & Levinson, Science, 2002

X-ray lines in disks

•Detect BH spin

•Time[measurement] << Time[BH spin down]

Calorimetry on GWB in GRB-SN

•Detect total energy (“nutritional content”)

•Time[measurement] = Time[BH spin-down]

(Fabian, this meeting)

Horizon dissipation

Radiation energiesLIGO

SN remnant X-ray emission lines

1e49erg

SN4e51erg irradiation of envelope Torus mass loss

Gravitational radiation

Torus winds

Thermal and neutrino emissions

GWB4e53erg

Torus input

EEgw 1000

Baryon poor outflows

GRB3e50erg

Black hole output

Rotational energy of black hole

LIGO Hanford

first-ever detections of gravitational radiation observe the Universe in gravitational waves (new sources, relic waves early universe,…)

probe inner engines of GRB-SNe observe ‘life’ the process of spin-down of Kerr black holes within one minute

test general relativity,…

VIRGO Pisa

ACIGA-LIGO Gingin

LIGO

S/N

(1/year)

M[GRB030329]<150MSolar(current LIGO sensitivity)

D1 D2 D1*D2

Simulation: instantaneous S/N-ratio = 0.15

LIGO

2/1/ assuming*

100Mpc within 1yrrateEvent

s of tens45s

erg104.4102erg

erg103102erg

(SN1998bw) erg102101erg

Hz250@1031

500Hz

102erg

max

1-

9013.07,

8/3-0.1

517,

21.0

_52

507,

3/81.030.0

50

517,

21.01.0

51

9

1-,70.1

7,1.053

rotrot

Hs

HX

H

HSN

B

Hgw

Hgw

EE

TMT

ME

ME

ME

Mf

ME

Theory* versus observationsTBD

TBD

TBD

GRB+SN+GWB

Endpoint of binary evolution?

“Gravitational radiation, luminous black holes and gamma-ray burst supernovae,” Cambridge University Press, to be published