Possible binary neutron star merger history of the primary of GW230529

Mahapatra, Parthapratim, Chattopadhyay, Debatri, Gupta, Anuradha, Antonini, Fabio ORCID: https://orcid.org/0000-0003-3138-6199, Favata, Marc, Sathyaprakash, B. S. ORCID: https://orcid.org/0000-0003-3845-7586 and Arun, K. G. 2025. Possible binary neutron star merger history of the primary of GW230529. Physical Review D (particles, fields, gravitation, and cosmology) 111 (12) , 123030. 10.1103/c9l3-gw6w

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Abstract

Black holes (BHs) with masses between ∼3–5M⊙, produced by a binary neutron star (BNS) merger, can further pair up with a neutron star or BH and merge again within a Hubble time. However, the astrophysical environments in which this can happen and the rate of such mergers are open questions in astrophysics. Gravitational waves may play an important role in answering these questions. In this context, we discuss the possibility that the primary of the recent LIGO-Virgo-KAGRA binary GW230529_181500 (GW230529, in short) is the product of a previous BNS merger. Invoking numerical relativity (NR)-based fitting formulas that map the binary constituents’ masses and tidal deformabilities to the mass, spin, and kick velocity of the remnant BH, we investigate the potential parents of GW230529’s primary. Our calculations using NR fits based on BNS simulations reveal that the remnant of a high-mass BNS merger similar to GW190425 is consistent with the primary of GW230529. This argument is further strengthened by the gravitational wave-based merger rate estimation of GW190425-like and GW230529-like populations. We show that around 18% (median) of the GW190425-like remnants could become the primary component in GW230529-like mergers. The dimensionless tidal deformability parameter of the heavier neutron star in the parent binary is constrained to 67−61+163 at 90% credibility. Using estimates of the gravitational-wave kick imparted to the remnant, we also discuss the astrophysical environments in which these types of mergers can take place and the implications for their future observations. Published by the American Physical Society 2025

Item Type:	Article
Date Type:	Published Online
Status:	Published
Schools:	Schools > Physics and Astronomy
Additional Information:	License information from Publisher: LICENSE 1: URL: https://creativecommons.org/licenses/by/4.0/, Start Date: 2025-06-20
Publisher:	American Physical Society
ISSN:	2470-0010
Date of First Compliant Deposit:	3 July 2025
Date of Acceptance:	20 May 2025
Last Modified:	03 Jul 2025 13:15
URI:	https://orca.cardiff.ac.uk/id/eprint/179519

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