Gravitational-wave constraints on the neutron-star-matter Equation of State
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 .
Cite
@article{arxiv.1711.02644,
title = {Gravitational-wave constraints on the neutron-star-matter Equation of State},
author = {Eemeli Annala and Tyler Gorda and Aleksi Kurkela and Aleksi Vuorinen},
journal= {arXiv preprint arXiv:1711.02644},
year = {2018}
}
Comments
6 pages, 4 figures; v2: results and discussion updated, version accepted to PRL