Hypernovae: GRB-supernovae as Hypernovae: GRB-supernovae as LIGO/VIRGO sources of gravitational LIGO/VIRGO sources of gravitational

radiationradiation

Maurice H.P.M. van Putten (MIT-LIGO)Maurice H.P.M. van Putten (MIT-LIGO)

in collaboration within collaboration with

Amir Levinson (Tel Aviv)Amir Levinson (Tel Aviv) Stephen Eikenberry (U Florida)Stephen Eikenberry (U Florida)Tania Regimbau (MIT-LIGO)Tania Regimbau (MIT-LIGO)

Eve Ostriker (U Maryland)Eve Ostriker (U Maryland)Hyun Kyu Lee (Hanyang U)Hyun Kyu Lee (Hanyang U)David Coward (U of WA)David Coward (U of WA)

Ronald Burman (U of WA)Ronald Burman (U of WA)Paris 2003 LIGO-G030269-00-R

Star-formation in a molecular cloud

Molecular cloud

Core-collapse in a rotating massive star in a binary

Molecular cloud

Core-collapse(Woosley-Paczynski-Brown)

Active stellar nuclei

Molecular cloud

Core-collapse(Woosley-Paczynski-Brown)

Active nucleus inside remnant stellar envelope

Hypernovae: GRB-supernovae from rotating black holes

Jet through remnant envelope (McFadyen & Woosley’98)

Hypernovae: GRB-supernovae from rotating black holes

Jet through remnant envelope (McFadyen & Woosley’98)

Torus produces winds & radiation:

Ejection of remnant stellar envelopeExcitation of X-ray line-emissions

van Putten (2003)

wr EE

GRB-SNe in 011211 and 030329

2002) Ghisellini (G. 104 52rE Stanek, K., et al., 2003 astro-ph/0304173

GRB 011211 (z=2.41) Reeves et al. ‘02

Outline

1. Quantitative phenomenology of GRB-supernovae

2. A causal spin-connection in active stellar nuclei

3. Durations of tens of seconds of long bursts

4. Calorimetry on radiation energies

5. Observational opportunities for Adv LIGO/VIRGO

6. Conclusions

GRBs with redshifts (33) and opening angles (16)

GRB redshift angle instrument

GRB970228 0.695 SAX/WFCGRB970508 0.835 0.293 SAX/WFCGRB970828 0.9578 0.072 RXTE/ASMGRB971214 3.42 >0.056 SAX/WFCGRB980425 0.0085 SAX/WFCGRB980613 1.096 >0.127 SAX/WFCGRB980703 0.996 0.135 RXTE/ASMGRB990123 1.6 0.050 SAX/WFCGRB990506 1.3 BAT/PCAGRB990510 1.619 0.053 SAX/WFCGRB990705 0.86 0.054 SAX/WFCGRB990712 0.434 >0.411 SAX/WFCGRB991208 0.706 <0.079 Uly/KO/NEGRB991216 1.02 0.051 BAT/PCAGRB000131 4.5 <0.047 Uly/KO/NEGRB000210 0.846 SAX/WFCGRB000131C 0.42 0.105 ASM/UlyGRB000214 2.03 SAX/WFCGRB000418 1.118 0.198 Uly/KO/NEGRB000911 1.058 Uly/KO/NEGRB000926 2.066 0.051 Uly/KO/NEGRB010222 1.477 SAX/WFCGRB010921 0.45 HE/Uly/SAXGRB011121 0.36 SAX/WFCGRB011211 2.14 SAX/WFCGRB020405 0.69 Uly/MO/SAXGRB020813 1.25 HETEGRB021004 2.3 HETEGRB021211 1.01 HETEGRB030226 1.98 HETEGRB030328 1.52 HETEGRB030329 0.168 HETE

Barthelmy’s IPNhttp://gcn.gsfc.nasa.gov/gcn/Greiner’s cataloguehttp://www.mpe.mpg.de/jcg/grbgeb.htmland Frail et al. (2001)

<- very nearby!

<- most nearby!

Durations of GRB-SNe True energy in gamma-rays

Frail et al. ‘01

erg103

s 10 few

50

90

E

T

Van Putten ‘02

The true-but-unseen GRB-event rate

2001) al.et (Frail 500/1

:emissions-GRBin factor beaming lGeometrica

bf

0 1 2 3 4 50.0

0.1

0.2

0.3

0.4

0.5

prob

abili

ty

redshift z

observed simulated: observable simulated: total p

SFR2(z)

year/105.0 rateevent GRB True 6

Van Putten & Regimbau2003, submitted

Unseen event rate = 1/fb or 1/fr times observed event rate

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

:SFR the tolocked sample limited-fluxin rate-lossEvent

rf

Phenomenology of GRB-SNe from rotating black holes

100MpcDn year withiper event 1

107/

101/

51

4900

rotEE

PT

erg104 :holeblack theofenergy Rotational

ms4 : torus theof periodKeplerian

:holeblack masssolar 7 aFor

54

rotE

P

Magnetized nucleus in core-collapseMagnetized nucleus in core-collapse

Goldreich and Julian (1969) (spin-down of pulsars (magnetized neutron stars))

Ruffini & Wilson (1975) (spin-down of black holes, but: weak fields)

Blandford & Znajek (1977) (strong fields, but: causality not addressed, Punsly & Coroniti 1990)…Van Putten (1999) (idem, with causality by topological equivalence to PSRs)…

A causal spin-connection to Kerr black holes

HVan Putten & Levinson, ApJ 2003; Science 2002Van Putten, Phys Rep, 2001; Science 1999

PSR+

PSR-

BH

PSR PSR

H 0

Spin-up Spin-down

Asy

mpto

tic

infinit

y

Topology of inner and outer torus Topology of inner and outer torus magnetospheres magnetospheres

(vacuum case)(vacuum case)

separatrix

Van Putten & Levinson, ApJ 2003

New magnetic stability criterion

0 BU

0 BU bR

Tidal dominated

Magnetic dominated

Sum of magnetic and tidal interaction

tilt

y]instabilit bucklingfor 1/15[ 12/1/ kB EE

Van Putten & Levinson, ApJ 2003

Durations of long bursts

SS

T

H

rotspin M

M

M

RMM

ST

ET

7630

/s40

4

Van Putten & Levinson, ApJ 2003

Most of the spin-energy is dissipated “unseen” in the event horizon of the black hole

spinTT 90

Long durations

40

13/840

900

10 1 ][

03.0/

1.0/

)03.0/()1.0/(102][

/ parameter Large

observed

MM

theory

PT

HT

HT

Critical point analysis in baryon-rich torus windCritical point analysis in baryon-rich torus wind

115

3/152

3/12/1

2 1.007.0

3

16surface] on torus[

p

S

T

p

lA BL

M

M

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pM

1-2-3/252

1

2/17

3/22/1

17 scmg1.010

10 Lr

rM

M

M

Mc

c

cc

S

T

S

Hsbc

1-30 sg101M

6/1

6/15210 1.0

2

S

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MLT

MeV-torus cools by neutrino emission (electron-positron capture on nuclei)

Van Putten & Levinson ApJ 2003

2MeV

Baryon-poor inner tube

Baryon-richOuter tube

Torus winds create open magnetic flux-tubes

Van Putten & Levinson, submitted; Science 2002Van Putten, Phys Rep, 2001; Science 1999

PSR+

PSR-BH Magnetic wall

The active stellar nucleus: a black hole in suspended accretion

Equilibrium charge distribution Equilibrium charge distribution

topolo

gy

Q>0Q>0 Q<0Q<0

Rapidly rotating black hole

Energy in baryon-poor outflowsEnergy in baryon-poor outflows

)2/(/

surfaces-flux of curvature Poloidal

4/

axisrotation along tube-fluxopen in Outflow

3/2

22

2290

RM

BMA

ATE

HH

HH

Hj

Van Putten & Levinson ApJ 2003

H

j

107][

)15.0/(1.0/101][

parameter Small

51

8/341

1

observed

theory

E

E

rot

Small GRB-energies

Durations and GRB-energiesDurations and GRB-energies

0

1

Rotational energy of black hole

Horizon dissipation Black hole output

Torus input Baryon poor outflows

GRBs

tens of seconds

0

Linearized stability analysis for the torus Linearized stability analysis for the torus

m=2 buckling mode

Free surface waves on inner and outerboundaries mutually interact

(Papaloizou-Pringle 1984)

Waves in a differentially rotating and incompressible toroidal fluid Waves in a differentially rotating and incompressible toroidal fluid

.0 conditionsboundary enthalpy zero subject to

),(',/,(variable) )2(2 where

)(2)(2

1986) al.et (Goldreichmotion ofequationsEulerLinearized (C)

'frequency corotation and number mode azimuthal of

0,)(

2002)Putten (van onsperturbati alirrotation ible,incompressfor potentialVelocity (B)

]2,23[)(

:criterion) sRayleigh' andKepler (between torusdunperturbean for analysis

stability linearized heconsider t (1984), Pringle-Papaloizou Following (A)

'

22

h

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m

zrae

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1986) al.et (Goldreich 0)(at conditionsBoundary (C)

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),(2

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40

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01

02212

rer

e

pp

r

rr

khBik

rh

mqqprra

zOar

qza

z

aqrarmr

A free boundary value problem

Multipole mass-moments in toriMultipole mass-moments in tori

(1986) al.et Goldreich

(1984) Pringle-Papaloizou

0~/ as 3 abqc

Van Putten, 2002

Slenderness ->

]2,23[)(

qr

ar

q

a

US

Gravitational radiation-reaction force (m=2) Gravitational radiation-reaction force (m=2)

45

332

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10~)(101

with

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Gravitational radiation-reaction force on quadrupole emissionsGravitational radiation-reaction force on quadrupole emissions

4102

‘

‘

Complex plane of corotation frequency

Increase in imaginary value: backreation promotes instability

Balance in angular momentum and energy flux

with the constitutive ansatz for dissipation

by turbulent MHD stresses, into thermal emissions and MeV-neutrino emissions

22 )( rAP

Prad

rad

Gravitational radiation in suspended accretion

~ ~ ~ 42

32rot

diss

rot

w

rot

gw

E

E

E

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Black hole-beauty: emissions from the torus

Asymptotic results for small slenderness

4e53 erg in gravitational radiation

4e52 erg in torus winds producing SNe

6e52 erg inMeV-neutrinos

torusof radiusmajor -to-minor21

%10/

HT

Remnants of beautyRemnants of beautyMorphology of GRB-supernova remnant:Morphology of GRB-supernova remnant:

Black hole in a binary with optical companion surrounded by SNRBlack hole in a binary with optical companion surrounded by SNR

Chu, Kim, Points et al., ApJ, 2000

RX J050736-6847.8RX J050736-6847.8

(Candidate GRB-SN remnant)

Rotational energy of black hole

Horizon dissipation Black hole output

Torus input Baryon poor outflows

Gravitational radiation

Torus winds

Thermal and neutrino emissions

Torus mass loss

GRB3e50erg

SN remnant X-ray emission lines

SN4e51erg

43

2

irradiation of envelope

GWB4e53erg

1e49erg

Calorimetry on active stellar nuclei

)2( 7

erg1065.3Hz455

2/3

52

mM

MEf Owgw

Observational constraint on gravitational wave-frequency from wind-energy

(scaling value of wind energy corresponds to eta=0.1)

iaq

coscos)cos(sinsincos

)2sin(cos4

)2cos()cos1(2

00

1

21

t

trh

trh

LT

T

T

0

Phase-modulation of observed radiation by Lense-Thirring precession

Van Putten, Lee, Lee & Kim,2003, in preparation

Line-of-sight

torus

n-torus

Phase-modulated wave-forms

6/

2/,4/,8/,00

Stochastic background radiation in gravitational waves

Van Putten, in preparation (2003)

D=100Mpc

h(f)-diagram in matched filtering

Stochastic background radiation in gravitational waves

Coward, van Putten & Burman 2002Van Putten et al., in preparation (2003)

Observational opportunities for Adv Observational opportunities for Adv LIGOLIGO

SH

SH

H

D

h

D

h

cs

MM

MM

N

S

BdMSS

N

S

85over averaged 2.1

144over averaged 5.8

Hz104

Hz)500(

Hz104

Hz)500(5.1 4/1

03.011.0

28

57

3/51.0

1

2

1/2-24

2/11

1

1/2-24

2/1

Van Putten (2003), in preparation

12/52/31

1/2-24

2/1

Mpc14071.0Hz104

Hz)500(8

d

M

MS

N

S

Solar

Hh

mf

Matched filtering

Correlating two detectors

Lower bound on black hole-mass in GRB Lower bound on black hole-mass in GRB 030329030329

Van Putten, Burst Digest (2003), LIGO DCC 030230-00-D

SolarH

Solar

H

mf

h

MM

M

M

N

S

S

25

1)Mpc800/Mpc140(7

201.08

01.0Hz104

Hz)500( :ysensitivit LivingstonCurrent

0.2: torusrotatingrapidly a ofy possibilit theEntertain

2/5

2/3

1

1/2-24

2/1

Spp we use matched filtering and define “no detection”: S/N<1

ConclusionsConclusionsGRB-SNe from rotating black holes have long durations (gamma0=1e4), small true

GRB-energies (gamma1=1e-4) and an true event rate of 1 per year in D=100Mpc

Durations of tens of seconds correspond to the lifetime of rapid spin of the black hole (gamma0[theory]=gamma0[observation]). Most of black hole spin-energy is dissipated in the event horizon.

GRB-SNe produce 4e53 erg in gravitational radiation via a causal spin-connection between the black hole and a surrounding torus in suspended accretion (gamma2=0.1)

The true GRB-energies represent a small fraction of black hole-spin energy, released through an open tube with finite horizon angle (gamma1[theory]=gamma1[observation])

Matched filtering gives (formally) rise to a current LIGO sensitivity range of 1Mpc, and a (formal) upper bound of 25 Solar masses in GRB 030329

The sensitivity range of Adv LIGO using matched filtering is 100Mpc

Correlation between two detectors may apply to searches for individual events, as well as searches for the contribution of GRB-SNe to the stochastic background radiation in gravitational waves (Omega-B=6e-8)

Opportunity: gravitational radiation from hypernovae: LIGO/VIRGO detections coincident (in position on the sky) with the expected wide-angle optical emissions from an associated supernova and non-coincident with the associated GRB-emissions