On the possible gamma-ray burst–gravitational wave association in GW150914 |
| |
| Institution: | 1. Center for Theoretical Physics, Polish Academy of Sciences, Al. Lotników 32/46, 02–668 Warsaw, Poland;2. Copernicus Astronomical Center, Polish Academy of Sciences, Bartycka 18, 00–716 Warsaw, Poland;3. Chair of Mathematical Methods in Physics, University of Warsaw, Pasteura 5, 02–093 Warsaw, Poland;1. Astronomy Department, Faculty of Science, King Abdulaziz University, 21589 Jeddah, Saudi Arabia;2. Sousse University, ESSTHS, Lamine Abbassi street, 4011 H. Sousse, Tunisia |
| |
| Abstract: | Data from the Fermi Gamma-ray Burst Monitor satellite observatory suggested that the recently discovered gravitational wave source, a pair of two coalescing black holes, was related to a gamma-ray burst. The observed high-energy electromagnetic radiation (above 50 keV) originated from a weak transient source and lasted for about 1 s. Its localization is consistent with the direction to GW150914. We speculate about the possible scenario for the formation of a gamma-ray burst accompanied by the gravitational-wave signal. Our model invokes a tight binary system consisting of a massive star and a black hole which leads to the triggering of a collapse of the star’s nucleus, the formation of a second black hole, and finally to the binary black hole merger. For the most-likely configuration of the binary spin vectors with respect to the orbital angular momentum in the GW150914 event, the recoil speed (kick velocity) acquired by the final black hole through gravitational wave emission is of the order of a few hundred km/s and this might be sufficient to get it closer to the envelope of surrounding material and capture a small fraction of matter from the remnant of the host star. The gamma-ray burst is produced by the accretion of this remnant matter onto the final black hole. The moderate spin of the final black hole suggests that the gamma-ray burst jet is powered by weak neutrino emission rather than the Blandford–Znajek mechanism, and hence explains the low power available for the observed GRB signal. |
| |
| Keywords: | |
| 本文献已被 ScienceDirect 等数据库收录！ |
|
