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Neutron Star Equation of State in light of GW190814
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The observation of gravitational waves from an asymmetric binary opens the possibility for heavy neutron stars, but these pose challenges to models of the neutron star equation of state. We construct heavy neutron stars by introducing non-trivial structure in the speed of sound sourced by deconfined QCD matter, which cannot be well recovered by spectral representations. Their moment of inertia, Love number and quadrupole moment are very small, so a tenfold increase in sensitivity may be needed to test this possibility with gravitational waves, which is feasible with third generation detectors.
Forward citations
Cited by 3 Pith papers
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NNStar: An end-to-end AI agent for nuclear matter and neutron star physics
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Quark Phase Space Distributions in Nuclei
Using Wigner distributions, the authors find that the fraction of baryons with quark phase-space occupancy above the Pauli bound tends to a constant for heavy nuclei, supporting the plausibility of low-momentum suppression.
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The equation of state for neutron stars
A textbook-style review of the neutron-star equation of state covering the models, experimental and observational constraints, and open questions, with no new result claimed or derived.
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