Kavli Affiliate: Lijing Shao
| First 5 Authors: Yi-Han Iris Yin, Bin-Bin Zhang, Hui Sun, Jun Yang, Yacheng Kang
| Summary:
GRB 211211A is a rare burst with a genuinely long duration, yet its prominent
kilonova association provides compelling evidence that this peculiar burst was
the result of a compact binary merger. However, the exact nature of the merging
objects, whether they were neutron star pairs, neutron star–black hole
systems, or neutron star–white dwarf systems, remains unsettled. This {it
Letter} delves into the rarity of this event and the possibility of using
current and next-generation gravitational wave detectors to distinguish between
the various types of binary systems. Our research reveals an event rate density
of $gtrsim 5.67^{+13.04}_{-4.69} times 10^{-3} rm Gpc^{-3} yr^{-1}$ for
GRB 211211A-like gamma-ray bursts (GRBs), which, assuming GRB 211211A is the
only example of such a burst, is significantly smaller than that of typical
long- and short-GRB populations. We further calculated that if the origin of
GRB 211211A is a result of a neutron star–black hole merger, it would be
detectable with a significant signal-to-noise ratio (S/N), given the
LIGO-Virgo-KAGRA designed sensitivity. On the other hand, a neutron star–white
dwarf binary would also produce a considerable S/N during the inspiral phase at
decihertz and is detectable by next-generation spaceborne detectors DECIGO and
the Big Bang Observer. However, to detect this type of system with millihertz
spaceborne detectors like LISA, Taiji, and TianQin, the event must be very
close, approximately 3 Mpc in distance or smaller.
| Search Query: ArXiv Query: search_query=au:”Lijing Shao”&id_list=&start=0&max_results=3