General-Relativistic Hydrodynamics Simulation of a Neutron Star - Sub-Solar-Mass Black Hole Merger

Abstract

Over the last few years, there has been an increasing interest in sub-solar mass black holes due to their potential to provide valuable information about cosmology or the black hole population. Motivated by this, we study observable phenomena connected to the merger of a sub-solar mass black hole with a neutron star. For this purpose, we perform new numerical-relativity simulations of a binary system composed of a black hole with mass $0.5M_{\odot }$ and a neutron star with mass $1.4M_{\odot }$. We investigate the merger dynamics of this exotic system and provide information about the connected gravitational-wave and kilonova signals. Our study indicates that current gravitational-waveform models cannot adequately describe such systems and that phenomenological relations connecting the binary parameters with the ejecta and remnant properties do not apply to our system. Furthermore, we find a dependence of the kilonova signal on the azimuthal viewing angle due to the asymmetric mass ejection. This first-of-its-kind simulation opens the door for studying sub-solar mass black hole - neutron star mergers and could serve as a testing ground for future model development.

17 pages, 14 figures, published in PRD

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Cited by in corpus (7)

• New and Robust Gravitational-Waveform Model for High-Mass-Ratio Binary Neutron Star Systems with Dynamical Tidal Effects
• Using Equation of State Constraints to Classify Low-Mass Compact Binary Mergers
• Cosmology and nuclear-physics implications of a subsolar gravitational-wave event
• Modeling matter(s) in SEOBNRv5THM: Generating fast and accurate effective-one-body waveforms for spin-aligned binary neutron stars
• Eccentricity as a signature of hierarchical subsolar-mass mergers in collapsar disks
• Probing the equation of state of neutron stars with captured primordial black holes
• Challenging a binary neutron star merger interpretation of GW230529