期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 392, 期 4, 页码 1451-1455出版社
OXFORD UNIV PRESS
DOI: 10.1111/j.1365-2966.2008.14139.x
关键词
accretion, accretion discs; black hole physics
资金
- NASA though Chandra Postdoctoral Fellowship [PF5-60040]
- Chandra X-ray Center
- Smithsonian Astrophysical Observatory for NASA
- NASA Astrophysics Theory [NNG06GI06G]
- [NASA8-03060]
When double neutron star or neutron star-black hole binaries merge, the final remnant may comprise a central solar-mass black hole surrounded by a similar to 0.01-0.1M circle dot torus. The subsequent evolution of this disc may be responsible for short. gamma-ray bursts (SGRBs). A comparable amount of mass is ejected into eccentric orbits and will eventually fallback to the merger site after similar to 0.01 s. In this paper, we investigate analytically the fate of the fallback matter, which may provide a luminous signal long after the disc is exhausted. We find that matter in the eccentric tail returns at a super-Eddington rate and eventually (greater than or similar to 0.1 s) is unable to cool via neutrino emission and accrete all the way to the black hole. Therefore, contrary to previous claims, our analysis suggests that fallback matter is not an efficient source of late-time accretion power and unlikely to cause the late-flaring activity observed in SGRB afterglows. The fallback matter rather forms a radiation-driven wind or a bound atmosphere. In both the cases, the emitting plasma is very opaque and photons are released with a degraded energy in the X-ray band. We therefore suggest that compact binary mergers could be followed by an 'X-ray renaissance', as late as several days to weeks after the merger. This might be observed by the next generation of X-ray detectors.
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