Gravitational radiation from gamma-ray bursts as observational opportunities for LIGO and VIRGO
Aug, 2003
41 pages
Published in:
- Phys.Rev.D 69 (2004) 044007
e-Print:
- gr-qc/0308016 [gr-qc]
Report number:
- LIGO-P030041-00-D
View in:
Citations per year
Abstract: (arXiv)
Gamma-ray bursts are believed to originate in core-collapse of massive stars. This produces an active nucleus containing a rapidly rotating Kerr black hole surrounded by a uniformly magnetized torus represented by two counter-oriented current rings. We quantify black hole spin-interactions with the torus and charged particles along open magnetic flux-tubes subtended by the event horizon. A major output of Egw=4e53 erg is radiated in gravitational waves of frequency fgw=500 Hz by a quadrupole mass-moment in the torus. Consistent with GRB-SNe, we find (i) Ts=90s (tens of s, Kouveliotou et al. 1993), (ii) aspherical SNe of kinetic energy Esn=2e51 erg (2e51 erg in SN1998bw, Hoeflich et al. 1999) and (iii) GRB-energies Egamma=2e50 erg (3e50erg in Frail et al. 2001). GRB-SNe occur perhaps about once a year within D=100Mpc. Correlating LIGO/Virgo detectors enables searches for nearby events and their spectral closure density 6e-9 around 250Hz in the stochastic background radiation in gravitational waves. At current sensitivity, LIGO-Hanford may place an upper bound around 150MSolar in GRB030329. Detection of Egw thus provides a method for identifying Kerr black holes by calorimetry.Note:
- to appear in PRD, 49p
- 98.70.Rz
- 04.30.Db
- gravitational radiation: particle source
- gamma ray: burst
- black hole: rotation
- gravitational radiation detector: correlation
- velocity: torus
- background: stochastic
- supernova
- data analysis method
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