Kavli Affiliate: Lijing Shao
| First 5 Authors: Jin-Ping Zhu, Rui-Chong Hu, Yacheng Kang, Bing Zhang, Hui Tong
| Summary:
In this {em Letter}, we explore the formation of the mass-gap black
hole-neutron star (mgBHNS) merger detected in gravitational wave (GW) event,
i.e., GW230529, from the isolated binary evolution channel, and study potential
signatures of its electromagnetic signals. By adopting the `delayed’ supernova
prescription and reasonable model realizations, our population synthesis
simulation results can simultaneously match the inferred event rate densities
of GW230529-like mgBHNS and total BHNS mergers, as well as the population
distribution of the BH mass in BHNS mergers reported by the LIGO-Virgo-KAGRA
Collaboration. Thus, we conclude that the recently-discovered mgBHNS merger,
GW230529, can be explained through the isolated binary evolution channel.
Considering the equation of states of AP4 and DD2, the probabilities that
GW230529 can make tidal disruption are $12.8%$ and $63.2%$, respectively. If
GW230529 is a disrupted event, the associated kilonova is predicted to have an
apparent magnitude of $sim23-24,{rm{mag}}$, and hence, can be detected by
the present survey projects and LSST. Since GW230529 could be an off-axis event
inferred from the GW observation, its associated gamma-ray burst (GRB) might be
too dim to be observed by $gamma$-ray detectors, interpreting the lack of GRB
observations. The detection of GW230529 confirms the existence of mgBHNS
mergers formed through the isolated binary evolution channel, suggesting that
BHNS mergers are still likely to be multimessenger sources that emit GWs, GRBs,
and kilonovae. Although mgBHNS mergers account for $sim60%$ cosmological BHNS
population, we find that $gtrsim90%$ disrupted BHNS mergers are expected to
originate from mgBHNS mergers.
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