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Does a hadron-quark phase transition in dense matter preclude the existence of massive neutron stars?

Published online by Cambridge University Press:  20 March 2013

N. Chamel ,
A. F. Fantina ,
J. M. Pearson  and
S. Goriely
N. Chamel
Affiliation:
Institut d'Astronomie et d'Astrophysique, CP-226, Université Libre de Bruxelles, 1050 Brussels, Belgium
A. F. Fantina
Affiliation:
Institut d'Astronomie et d'Astrophysique, CP-226, Université Libre de Bruxelles, 1050 Brussels, Belgium
J. M. Pearson
Affiliation:
Dépt. de Physique, Université de Montréal, Montréal (Québec), H3C 3J7Canada
S. Goriely
Affiliation:
Institut d'Astronomie et d'Astrophysique, CP-226, Université Libre de Bruxelles, 1050 Brussels, Belgium
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Abstract

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We study the impact of a hadron-quark phase transition on the maximum neutron-star mass. The hadronic part of the equation of state relies on the most up-to-date Skyrme nuclear energy density functionals, fitted to essentially all experimental nuclear mass data and constrained to reproduce the properties of infinite nuclear matter as obtained from microscopic calculations using realistic forces. We show that the softening of the dense matter equation of state due to the phase transition is not necessarily incompatible with the existence of massive neutron stars like PSR J1614–2230.

Keywords

stars: neutrondense matterequation of statestars: interiorsgravitation

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