Distinguishing double neutron star from neutron star-black hole binary populations with gravitational wave observations

Abstract

Gravitational waves from the merger of two neutron stars cannot be easily distinguished from those produced by a comparable-mass mixed binary in which one of the companions is a black hole. Low-mass black holes are interesting because they could form in the aftermath of the coalescence of two neutron stars, from the collapse of massive stars, from matter overdensities in the primordial Universe, or as the outcome of the interaction between neutron stars and dark matter. Gravitational waves carry the imprint of the internal composition of neutron stars via the so-called tidal deformability parameter, which depends on the stellar equation of state and is equal to zero for black holes. We present a new data analysis strategy powered by Bayesian inference and machine learning to identify mixed binaries, hence low-mass black holes, using the distribution of the tidal deformability parameter inferred from gravitational-wave observations.

13 pages, 6 figures - v2: matches the published version in Phys. Rev. D 102, 023025

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Cited by in corpus (4)

• Observation of gravitational waves from two neutron star-black hole coalescences
• Causal Limit of Neutron Star Maximum Mass in $f(R)$ Gravity in View of GW190814
• Modelling Neutron Star-Black Hole Binaries: Future Pulsar Surveys and Gravitational Wave Detectors
• On exotic objects made of dark energy and dark matter: Mass-to-radius profiles and tidal Love numbers