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Journal Article

Long-duration Gamma-ray Burst and Associated Kilonova Emission from Fast-spinning Black Hole--Neutron Star Mergers


Wu,  Shichao
Observational Relativity and Cosmology, AEI-Hannover, MPI for Gravitational Physics, Max Planck Society;

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Zhu, J.-P., Wang, X. I., Sun, H., Yang, Y.-P., Li, Z., Hu, R.-C., et al. (2022). Long-duration Gamma-ray Burst and Associated Kilonova Emission from Fast-spinning Black Hole--Neutron Star Mergers. The Astrophysical Journal Letters, 936(1): L10. doi:10.3847/2041-8213/ac85ad.

Cite as: https://hdl.handle.net/21.11116/0000-000B-22CA-B
Here we collect three unique bursts, GRBs\,060614, 211211A and 211227A, all
characterized by a long-duration main emission (ME) phase and a rebrightening
extended emission (EE) phase, to study their observed properties and the
potential origin as neutron star-black hole (NSBH) mergers. NS-first-born
(BH-first-born) NSBH mergers tend to contain fast-spinning (non-spinning) BHs
that more easily (hardly) allow tidal disruption to happen with (without)
forming electromagnetic signals. We find that NS-first-born NSBH mergers can
well interpret the origins of these three GRBs, supported by that: (1) Their
X-ray MEs and EEs show unambiguous fall-back accretion signatures, decreasing
as $\propto{t}^{-5/3}$, which might account for their long duration. The EEs
can result from the fall-back accretion of $r$-process heating materials,
predicted to occur after NSBH mergers. (2) The beaming-corrected local event
rate density for this type of merger-origin long-duration GRBs is
consistent with that of NS-first-born NSBH mergers. (3) Our detailed analysis
on the EE, afterglow and kilonova of the recently high-impact event
GRB\,211211A reveals it could be a merger between a
$\sim1.23^{+0.06}_{-0.07}\,M_\odot$ NS and a
$\sim8.21^{+0.77}_{-0.75}\,M_\odot$ BH with an aligned-spin of
$\chi_{\rm{BH}}\sim0.62^{+0.06}_{-0.07}$, supporting an NS-first-born NSBH
formation channel. Long-duration burst with rebrightening fall-back accretion
signature after ME, and bright kilonova might be commonly observed features for
on-axis NSBHs. We estimate the multimessenger detection rate between
gravitational waves, GRBs and kilonovae from NSBH mergers in O4 (O5) is
$\sim0.1\,{\rm{yr}}^{-1}$ ($\sim1\,{\rm{yr}}^{-1}$).