Origin of Black Hole Spin in Lower-Mass-Gap Black Hole-Neutron Star Binaries

Abstract

During the fourth observing run, the LIGO-Virgo-KAGRA Collaboration reported the detection of a coalescing compact binary (GW230529${}_{-}$181500) with component masses estimated at $2.5-4.5M_{\odot }$ and $1.2-2.0M_{\odot }$ with 90\% credibility. Given the current constraints on the maximum neutron star (NS) mass, this event is most likely a lower-mass-gap (LMG) black hole-neutron star (BHNS) binary. The spin magnitude of the BH, especially when aligned with the orbital angular momentum, is critical in determining whether the NS is tidally disrupted. An LMG BHNS merger with a rapidly spinning BH is an ideal candidate for producing electromagnetic counterparts. However, no such signals have been detected. In this study, we employ a detailed binary evolution model, incorporating new dynamical tide implementations, to explore the origin of BH spin in an LMG BHNS binary. If the NS forms first, the BH progenitor (He-rich star) must begin in orbit shorter than 0.35 days to spin up efficiently, potentially achieving a spin magnitude of ${\chi }_{\mathrm{BH}}>0.3$. Alternatively, if a non-spinning BH (e.g., $M_{\mathrm{BH}}=3.6M_{\odot }$) forms first, it can accrete up to $\sim 0.2M_{\odot }$ via Case BA mass transfer (MT), reaching a spin magnitude of ${\chi }_{\mathrm{BH}}\sim 0.18$ under Eddington-limited accretion. With a higher Eddington accretion limit (i.e., 10.0 $\Dot{M}_{\rm Edd}$), the BH can attain a significantly higher spin magnitude of ${\chi }_{\mathrm{BH}}\sim 0.65$ by accreting approximately $1.0M_{\odot }$ during Case BA MT phase.

arXiv commentAccepted by A&A Letters (09/11/2024)

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• Possible binary neutron star merger history of the primary of GW230529
• Reassessing the Spin of Second-born Black Holes in Coalescing Binary Black Holes and Its Connection to the chi_eff-q Correlation
• Characterizing Compact-object Binaries in the Lower Mass Gap with Gravitational Waves
• Diagnosing the Properties and Evolutionary Fates of Black Hole and Wolf-Rayet X-ray Binaries as Potential Gravitational Wave Sources for the LIGO-Virgo-KAGRA Network