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arXiv · 1711.02644

Gravitational-wave constraints on the neutron-star-matter Equation of State

Eemeli Annala·Tyler Gorda·Aleksi Kurkela·Aleksi Vuorinen
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Abstract

The LIGO/Virgo detection of gravitational waves originating from a neutron-star merger, GW170817, 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 smallest allowed tidal deformability of a similar-mass star is $\Lambda(1.4 M_\odot) = 120$.

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Eemeli Annala, Tyler Gorda, Aleksi Kurkela, Aleksi Vuorinen. 2017-11-07. Gravitational-wave constraints on the neutron-star-matter Equation of State. https://doi.org/10.1103/physrevlett.120.172703

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