GRBs and their contribution to the GRBs and their contribution to the stochastic background radiation in stochastic background radiation in

gravitational wavesgravitational waves

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

LIGO-G030145-00-ZLIGO-G030145-00-Z

LSC March 2003

GRB-durations and energies GRB-SNe association

Frail et al. ‘01

Kouvelioutou et al. ‘93

Van Putten ‘02

GRB 011211 (z=2.41) Reeves et al. ‘02

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 pSFR2(z)

Regimbau & Van Putten2003, in preparation

Formation of counter-oriented current rings in core-Formation of counter-oriented current rings in core-collapsecollapse

Van Putten & Levinson, ApJ, 2003

Topology of flux-surfaces of a uniformly magnetized Topology of flux-surfaces of a uniformly magnetized torus torus

(vacuum case)(vacuum case)

separatrix

Van Putten & Levinson, ApJ 2003

Magnetic stability

Van Putten & Levinson, ApJ 2003

buckling]1/15[tilt 12/1/ kB EE

0 BU

0 BU bR

tilt

G-dominant

B-dominant

Potential energy (magnetic+tidal)

Van Putten-Levinson stability criterion:

Black hole luminosity from horizon Maxwell stresses:

Perturbative limit: Ruffini & Wilson (PRD 1975) Non-perturbative: Blandford & Znajek (MNRAS 1977) but: causality unresolved (Punsly & Coroniti ApJ 1989) Causality by topological equivalence to PSRs: van Putten (Science 1999): (a) Most of the black hole luminosity is incident onto the inner face of the torus (b) Most of the black hole-spin energy is dissipated in the horizon

Topological Equivalence to Pulsars

H

PSR+

PSR-

BH

PSR PSR

H 0

Spin-up Spin-down

Asym

ptot

ic in

finity

40

13/84900

10 few :

03.0/

1.0/ in

)03.0/()1.0/(104 /

parameter Large

Observed

MM

PT

HT

HT

Long durationsHT

SSH

rots MM

MM

MR

ST

ET / ,

7603.0s40

41

Van Putten & Levinson ApJ 2003

Creation of open magnetic flux-tubesCreation of open magnetic flux-tubes

2MeV

Baryon-poor inner tube Baryon-rich

Outer tube

Energy in baryon-poor outflowsEnergy in baryon-poor outflows

)/6(10

surfaces-flux of curvature Poloidal

axisrotation along Outflow

22

2290

RM

BMA

ATE

HH

HH

Hj

Van Putten ApJ 2003Van Putten & Levinson APJ 2003

H

j

)16.0/(105 :

1.0/102

parameter Small

141

1

8/341

rot

rot

j

EE

Observed

EE

Van Putten ApJ 2003Van Putten & Levinson APJ 2003

Small GRB-energies

T90 and GRB-energiesT90 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

Stability diagram of multipole mass-Stability diagram of multipole mass-moments moments

(1986) al.et Goldreich

(1984) Pringle-Papaloizou0~/ as 3 abqc

Van Putten, 2002

Slenderness ->

]2,23[)(

qrar

q

a

US

Balance in angular momentum and energy transport for atorus around a black hole with a quadrupole mass moment

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

Van Putten, 2001

S

TT

S

HGW

MM

M

MM

E

1.0 %200

7 erg 104 53

In practical terms…

Gravitational radiation by catalytic conversion of spin-energy

~~~ 42

32rot

diss

rot

w

rot

gw

EE

EE

EE

Energy emissions from the torus

Asymptotic results for small slenderness

CalorimetryCalorimetry

)2( 7

erg104Hz470

2/3

52

mMME

f Owgw

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

GRBs

SN remnant X-ray emission lines

43

2

SN irradiation of envelope

1

erg 104

2002) ,Ghisillini (G. erg 104

52

52

W

r

E

E

)144( 1200Hz-1807

Hz4702/3

SS

GW MMMM

f

Emission lines in GRB 011211 (Reeves et al., 2002)

Van Putten, ApJ, 2003

Observational opportunities in astronomyObservational opportunities in astronomy

Calorimetry on SNRs of GRB-remnants: constrain wind energies and frequency in gwsCalorimetry on SNRs of GRB-remnants: constrain wind energies and frequency in gws

Morphology of GRB-remants: black hole in a binary with optical companion Morphology of GRB-remants: black hole in a binary with optical companion surrounded by SNRsurrounded by SNR

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

RX J050736-6847.8

Stochastic background radiation

],[,)7(/,)()(

||||/)(Hz470

)7(erg104

)7( 109)(

21

/7

/7

32

1

539

1

2

MMMMffxdyyDyxxf

fxfMfME

f

H

xMM

xMM

Sgw

SgwSgwB

S

S

B

BB

Van Putten (2003), in preparation

(lower) 85(upper) 144

(dashed) Hz1000)7(

(line) Hz470)7(

SH

SH

Sgw

Sgw

MMMM

Mf

Mf

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

Observational opportunities for LIGOObservational opportunities for LIGO

Radiation from GRB-SNe, point sources:Radiation from GRB-SNe, point sources:

Associated with SNe, test t0[gw-burst]=t0[SN]Associated with SNe, test t0[gw-burst]=t0[SN]

Radiation from GRB-SNe, stochastic background Radiation from GRB-SNe, stochastic background radiation:radiation:

SH

SH

LS

H

Sgw

Sgwh

MM

MM

NS

dMM

MfMES

NS

85over averaged 7

144over averaged 18

Mpc1407)7(

Hz470erg104

)7(104

Hz)500(8

2/522/1

53

1

24

2/1

2/12/11

530

2

24

2/1

year)7(Hz470

erg104104Hz)500(

)85( 2)144( 10

TMf

ESMMMM

NS

Sgw

h

SH

SH

Van Putten (2003), in preparation

A line-detection algorithm

Van Putten & van Putten, in prep

)2/3(4/1)1(2

21)()(

)()()(

)5.1sin()sin()(

)2,1()()()(

4

2

2/12

0

21

NMM

dtthth

tbtath

itnthth

T

s

isi

Model:Model: GRB-SNe from rotating black holes in dimensionless GRB-SNe from rotating black holes in dimensionless gamma parametersgamma parameters as a function of as a function of normalized angular velocity normalized angular velocity etaeta, slenderness , slenderness deltadelta and mass and mass mumu of the surrounding torus of the surrounding torus

Long durations (Long durations (largelarge gamma0~1e4gamma0~1e4) stem from lifetime black hole-spin, subject to the Van Putten-) stem from lifetime black hole-spin, subject to the Van Putten-Levinson stability criterion for the torus.Levinson stability criterion for the torus.

GRB-energies (GRB-energies (smallsmall gamma1~1e-3gamma1~1e-3) derive from a BPJ produced by the black hole, regulated by ) derive from a BPJ produced by the black hole, regulated by poloidal curvature in torus magnetospherepoloidal curvature in torus magnetosphere

Gravitational radiation during the GRB-SNe event of energies of a few times 0.1MSolar (Gravitational radiation during the GRB-SNe event of energies of a few times 0.1MSolar (gamma2~0.1gamma2~0.1) ) at an expected nominal frequency around 470Hzat an expected nominal frequency around 470Hz

Expect spectral closure density of about 1e-8 @100-300HzExpect spectral closure density of about 1e-8 @100-300Hz Observational opportunities for HF in Advanced LIGO with 3 detectorsObservational opportunities for HF in Advanced LIGO with 3 detectors

GRB remnants: black hole-binaries in SNRsGRB remnants: black hole-binaries in SNRs Gravitational radiation in GRB-SNe (1/yr within D=100Mpc) Gravitational radiation in GRB-SNe (1/yr within D=100Mpc) LIGO GRB-sensitivity range LIGO GRB-sensitivity range presentlypresently: 1Mpc@500Hz: 1Mpc@500Hz Multiple lines in stochastic background radiation (1 yr obs LIGO-II)Multiple lines in stochastic background radiation (1 yr obs LIGO-II)

ConclusionsConclusions