Kavli Affiliate: Renxin Xu
| First 5 Authors: Shuang Du, Tingting Lin, Shujin Hou, Renxin Xu,
| Summary:
It seems that the wealth of information revealed by the multi-messenger
observations of the binary neutron star (NS) merger event, GW170817/GRB
170817A/kilonova AT2017gfo, places irreconcilable constraints to models of the
prompt emission of this gamma-ray burst (GRB). The observed time delay between
the merger of the two NSs and the trigger of the GRB and the thermal tail of
the prompt emission can hardly be reproduced by these models simultaneously. We
argue that the merger remnant should be an NS (last for, at least, a large
fraction of 1s), and that the difficulty can be alleviated by the delayed
formation of the accretion disk due to the absorption of high-energy neutrinos
emitted by the NS and the delayed emergence of an effective viscous in the
disk. Further, we extend the consideration of the effect of the energy
deposition of neutrinos emitted from the NS. If the NS is the central object of
a GRB with a distance and duration similar to that of GRB 170817A, thermal
emission of the thermal bubble inflated by the NS after the termination of
accretion may be detectable. If our scenario is verified, it would be of
interest to investigate the cooling of nascent NSs.
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