Role of the symmetry energy and the neutron-matter stiffness on the tidal deformability of a neutron star with unified equations of state

L. Perot, N. Chamel, and A. Sourie

Phys. Rev. C 100, 035801 – Published 4 September 2019

Abstract

The role of the symmetry energy and the neutron-matter stiffness on the tidal deformability of a cold nonaccreted neutron star is studied using a set of unified equations of state. Based on the nuclear energy-density functional theory, these equations of state provide a thermodynamically consistent treatment of all regions of the star and were calculated using functionals that were precision fitted to experimental and theoretical nuclear data. Predictions are compared to constraints inferred from the recent detection of the gravitational-wave signal GW170817 from a binary neutron-star merger and from observations of the electromagnetic counterparts.

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Received 14 June 2019

DOI:https://doi.org/10.1103/PhysRevC.100.035801

Physics Subject Headings (PhySH)

Equations of state of nuclear matter Gravitational waves Nuclear matter in neutron stars Symmetry energy

Neutron stars & pulsars

Nuclear density functional theory

Nuclear Physics

Authors & Affiliations

L. Perot¹, N. Chamel ¹, and A. Sourie^1,2

¹Institute of Astronomy and Astrophysics, Université Libre de Bruxelles, CP 226, Boulevard du Triomphe, B-1050 Brussels, Belgium
²LUTH, Observatoire de Paris, PSL Research University, CNRS, Université Paris Diderot, Sorbonne Paris Cité, 5 place Jules Janssen, 92195 Meudon, France

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Issue

Vol. 100, Iss. 3 — September 2019

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Physical Review C

covering nuclear physics