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• W2767349080 abstract "The detection of gravitational waves originating from a neutron-star merger, GW170817, by the LIGO and Virgo Collaborations has recently provided new stringent limits on the tidal deformabilities of the stars involved in the collision. Combining this measurement with the existence of two-solar-mass stars, we generate a generic family of neutron-star-matter equations of state (EOSs) that interpolate between state-of-the-art theoretical results at low and high baryon density. Comparing the results to ones obtained without the tidal-deformability constraint, we witness a dramatic reduction in the family of allowed EOSs. Based on our analysis, we conclude that the maximal radius of a 1.4-solar-mass neutron star is 13.6 km, and that the smallest allowed tidal deformability of a similar-mass star is Λ(1.4 M⊙)=120.Received 27 November 2017Revised 6 February 2018DOI:https://doi.org/10.1103/PhysRevLett.120.172703Published by the American Physical Society under the terms of the Creative Commons Attribution 4.0 International license. Further distribution of this work must maintain attribution to the author(s) and the published article’s title, journal citation, and DOI.Published by the American Physical SocietyPhysics Subject Headings (PhySH)Research AreasEquations of state of nuclear matterGravitational wave sourcesNuclear matter in neutron starsQuantum chromodynamicsPhysical SystemsNeutron stars & pulsarsNuclear PhysicsParticles & FieldsGravitation, Cosmology & Astrophysics" @default.
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• W2767349080 date "2018-04-25" @default.
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• W2767349080 title "Gravitational-Wave Constraints on the Neutron-Star-Matter Equation of State" @default.
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• W2767349080 doi "https://doi.org/10.1103/physrevlett.120.172703" @default.
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