A Channel to Form Fast-spinning Black Hole–Neutron Star Binary Mergers as Multimessenger Sources

Hu, Rui-Chong; Zhu, Jin-Ping; Qin, Ying; Zhang, Bing; Liang, En‐Wei; Shao, Yong

doi:10.3847/1538-4357/ac573f

Cited by 22 publications

(25 citation statements)

References 85 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Similar evolutionary scenarios to those shown in Fig. 1 can also occur at lower masses and produce neutron star-black hole binaries, where the (more massive) black hole is formed second (Chattopadhyay et al 2021;Broekgaarden et al 2021;Hu et al 2022). In the context of radio astronomy, this can be important for determining if the neutron star can be born first and recycled (Chattopadhyay et al 2021).…”

Section: Neutron Star-black Hole Binariessupporting

confidence: 69%

Signatures of mass ratio reversal in gravitational waves from merging binary black holes

Broekgaarden¹,

Stevenson²,

Thrane³

2022

Preprint

View full text Add to dashboard Cite

The spins of merging binary black holes offer insights into their formation history. Recently it has been argued that in isolated binary evolution of two massive stars the firstborn black hole is slowly rotating, whilst the progenitor of the second-born black hole can be tidally spun up if the binary is tight enough. Naively, one might therefore expect that only the less massive black hole in merging binaries exhibits non-negligible spin. However, if the mass ratio of the binary is "reversed" (typically during the first mass transfer episode), it is possible for the tidally spun up second-born to become the more massive black hole. We study the properties of such mass-ratio reversed (MRR) binary black hole mergers using a large set of 560 population synthesis models. We find that the more massive black hole is formed second in 70% of binary black holes observable by LIGO, Virgo, and KAGRA for most model variations we consider, with typical total masses 20 M and mass ratios q = m 2 /m 1 ∼ 0.7 (where m 1 > m 2 ). The formation history of these systems typically involves only stable mass transfer episodes. The second-born black hole has non-negligible spin (χ > 0.05) in up to 25% of binary black holes, with among those the more (less) massive black hole spinning in 0%-80% (20%-100%) of cases, varying greatly in our models. We discuss our models in the context of several observed gravitational-wave events and the observed mass ratio -effective spin correlation.

show abstract

Section: Neutron Star-black Hole Binariessupporting

confidence: 69%

Signatures of mass ratio reversal in gravitational waves from merging binary black holes

Broekgaarden¹,

Stevenson²,

Thrane³

2022

Preprint

View full text Add to dashboard Cite

show abstract

“…In particular, since the more massive star at ZAMS will almost always evolve off the main sequence first, it will be the first to overflow its Roche lobe and transfer material onto its companion. The fraction of transferred mass deposited onto the companion depends on an uncertain MT accretion efficiency (Bouffanais et al 2021b), and can potentially lead to a mass ratio reversal (MRR), where the star that was originally less massive at ZAMS has its mass inflated from the accreted material and leads to a more massive remnant (e.g., Olejak & Belczynski 2021;Hu et al 2022). The originally more massive star will still proceed through the remainder of its evolution quicker, and create the first compact object in the binary.…”

Section: Introductionmentioning

confidence: 99%

Suspicious Siblings: The Distribution of Mass and Spin across Component Black Holes in Isolated Binary Evolution

Zevin

Bavera

2022

ApJ

View full text Add to dashboard Cite

The LIGO and Virgo gravitational-wave detectors have uncovered binary black hole systems with definitively nonzero spins, as well as systems with significant spin residing in the more massive black hole of the pair. We investigate the ability of isolated binary evolution in forming such highly spinning, asymmetric-mass systems through both accretion onto the first-born black hole and tidal spin-up of the second-born black hole using a rapid population synthesis approach with detailed considerations of spin-up through tidal interactions. Even with the most optimistic assumptions regarding the efficiency at which an accreting star receives material from a donor, we find that it is difficult to form systems with significant mass asymmetry and moderate or high spins in the primary black hole component. Assuming efficient angular momentum transport within massive stars and Eddington-limited accretion onto black holes, we find that >1.5% of systems in the underlying binary black hole population have a primary black hole spin greater than 0.2 and a mass asymmetry of greater than 2:1 in our most optimistic models, with most models finding that this criteria is only met in ∼0.01% of systems. The production of systems with significant mass asymmetries and spin in the primary black hole component is thus an unlikely byproduct of isolated evolution unless highly super-Eddington accretion is invoked or angular momentum transport in massive stars is less efficient than typically assumed.

show abstract

“…However, the beaming-corrected rate density of mergerorigin lGRBs is consistent with that of NS-first-born NSBH merger ( 20% of total NSBH populations; Román-Garza et al 2021; Chattopadhyay et al 2022). By investigating the parameter space of forming NSfirst-born NSBH binaries, Hu et al (2022) found that most of NSBH binaries that can merge within Hubble time would have BHs with projected aligned spins χ BH 0.8 and, hence, can certainly make tidal disruptions to produce electromagnetic counterparts. Only a small fractional low-mass BHs with χ BH ∼ 0.2 − 0.8 can merge with an NS within Hubble time and can still allow tidal disruption to happen if NSs are not really massive (i.e., M NS 1.6 − 2.0 M ).…”

Section: Event Rate Densitymentioning

confidence: 62%

“…In this scenario, the primary BHs are usually born first and have negligible spins consistent with the properties of LVC NSBH candidates Zhu et al 2021a). Conversely, if the NSs are born first, the progenitors of the BHs would be tidally spun up efficiently by the NSs in close binaries (orbital periods 2 d) and finally form fastspinning BHs (Hu et al 2022). A fractional of these NS-first-born NSBH systems formed in close binaries can merge within Hubble time.…”

Section: Introductionmentioning

confidence: 84%

“…In Section 2.2, we suspected that GRB 211211A can be originated from NS-first-born NSBH mergers based on the estimations of the event rate density. Hu et al (2022) found that for a NS-first-born NSBH binary system, the companion helium star would be tidally spun up efficiently by the NS, and would thus finally form a fast-spinning BH whose aligned-spin is always χ BH 0.8. Thus, the mass and spin of the BH component for GRB 211211A are essentially consistent with those of NS-first-born NSBH merger predicted by Hu et al (2022).…”

Section: Origins Of Grb 211211a and Associated Kilonovamentioning

confidence: 99%

See 1 more Smart Citation

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

Zhu¹,

Wang²,

Yang³

et al. 2022

Preprint

Self Cite

View full text Add to dashboard Cite

Gamma-ray bursts (GRBs) have been phenomenologically divided into long-and short-duration populations, generally corresponding to the collapsar and compact merger origin, respectively. 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 (BHfirst-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-firstborn 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 ∝ 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 R 0 ∼ 2.4 +2.3 −1.3 Gpc −3 yr −1 , 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 ∼ 1.23 +0.06 −0.07 M NS and a ∼ 8.21 +0.77 −0.75 M BH with an aligned-spin of χ BH ∼ 0.62 +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 NSBH mergers. We estimate the multimessenger detection rate between gravitational waves, GRB and kilonova emissions from NSBH mergers in O4 (O5) is ∼ 0.1 yr −1 (∼ 1 yr −1 ).

show abstract

A Channel to Form Fast-spinning Black Hole–Neutron Star Binary Mergers as Multimessenger Sources

Cited by 22 publications

References 85 publications

Signatures of mass ratio reversal in gravitational waves from merging binary black holes

Signatures of mass ratio reversal in gravitational waves from merging binary black holes

Suspicious Siblings: The Distribution of Mass and Spin across Component Black Holes in Isolated Binary Evolution

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

Contact Info

Product

Resources

About