Diogo Belloni (CAMK, Warsaw)
Based on Schreiber et al., MNRAS (2016)
Dominik Gronkiewicz (CAMK, Warsaw)
Based on Phillips et al. ApJ 809 (2015).
Miljenko Cemeljic (CAMK, Warsaw)
Based on Cabral and Lobo, arXiv:1603.08157
Agnieszka Janiuk (CFT, Warsaw)
We speculate on the possible scenario for the formation of a gamma-ray burst accompanied by the GW signal. Our model invokes a close binary system consisting of a massive star and a black hole, which leads to triggering of a collapse of the star's nucleus, 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 velocity acquired by the final black hole through gravitational waves emission allows it to take only a small fraction of matter from the host star. The gamma-ray burst is produced on the cost of accretion of this remnant matter onto the final black hole. The moderate spin of the final black hole accounts for the gamma-ray burst jet to be powered by a weak neutrino emission rather than the Blandford-Znajek mechanism, and hence explains low power available for the observed GRB signal.
