Realistic Equations of State Informing Neutron Star Post-Merger Gravitational-Wave Frequencies

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ID: 318619
2026
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Abstract
Abstract Binary neutron star mergers are thought to produce hot, rapidly rotating neutron stars with masses that can far exceed their Tolman-Oppenheimer-Volkoff mass. The gravitational-wave emission from such remnants provides a unique opportunity to measure the nuclear equation of state at densities and temperatures not available to terrestrial experiments. Current detector design is informed by gravitational-wave signals from general relativistic hydrodynamics simulations of neutron star mergers, typically with hybrid thermal treatments for the equation of state, where a cold equation of state is modified by adding a thermal component. We use realistic equations of state based on the relativistic mean field model with consistent treatment of thermal effects to compute the distribution of expected peak gravitational-wave frequencies. Marginalising over equation of state and progenitor neutron star masses, we show the peak frequency of emission ranges from ~2.5 to 4 kHz. The width of this distribution suggests the need for broadband observatories with kHz sensitivity, and calls into question some of the so-called post-merger optimised configurations. We show the proposed KAGRA high-frequency design is well-suited to measuring post-merger remnants when compared to the KAGRA broadband design.
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Authors Spencer J. Magnall, Nilaksha Barman, Debarati Chatterjee, Paul D. Lasky, Simon Goode
Journal monthly notices of the royal astronomical society
Year 2026
DOI
10.1093/mnras/stag1184
URL
https://doi.org/10.1093/mnras/stag1184
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