2003/01/30 by Maurice H. P. M. van Putten, van Putten, Maurice H. P. M.
Physics and Astronomy · #Astrophysical Phenomena and Observations #Astrophysics (astro-ph) #FOS: Physical sciences #Gamma-ray bursts and supernovae #Pulsars and Gravitational Waves Research #astro-ph
paper · pdf · doi:10.48550/arxiv.astro-ph/0301607
Invited talk at GRBs in the Afterglow Era: 3rd Workshop, Rome 2002
arxiv created 2003/01/30 · openalex publication_date 2003/01/30 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
We present a mechanism for long bursts of gravitational radiation from Kerr black holes surrounded by a torus. These systems are believed to form in core-collapse of massive stars in association with gamma-ray bursts. The torus catalyzes black hole-spin energy mostly into gravitational radiation, with a minor output in winds, thermal and neutrino emissions. Torus winds impact the remnant envelope of the progenitor star from within, which may account for X-ray emission lines and leaves a supernova remnant. The frequency in gravitational radiation satisfies fgw=470Hz (ESNR/4× 1051)1/2(0.1/β)1/2(7M_\odot/MH)3/2, where ESNR is the kinetic energy in the SNR, MH is the black hole mass and β≃0.1 the initial ejection velocity, as detected in GRB 011211. Ultimately, this leaves a black hole binary surrounded by a SNR, which is conceivably illustrated by RX J050736-6847.8.