Neutron-Star-Merger Equation of State
Abstract
In this work, we discuss the dense matter equation of state (EOS) for the extreme range of conditions encountered in neutron stars and their mergers. The calculation of the properties of such an EOS involves modeling different degrees of freedom (such as nuclei, nucleons, hyperons, and quarks), taking into account different symmetries, and including finite density and temperature effects in a thermodynamically consistent manner. We begin by addressing subnuclear matter consisting of nucleons and a small admixture of light nuclei in the context of the excluded volume approach. We then turn our attention to supranuclear homogeneous matter as described by the Chiral Mean Field (CMF) formalism. Finally, we present results from realistic neutron-star-merger simulations performed using the CMF model that predict signatures for deconfinement to quark matter in gravitational wave signals.
Keywords
Cite
@article{arxiv.1905.12658,
title = {Neutron-Star-Merger Equation of State},
author = {Veronica Dexheimer and Constantinos Constantinou and Elias R. Most and L. Jens Papenfort and Matthias Hanauske and Stefan Schramm and Horst Stoecker and Luciano Rezzolla},
journal= {arXiv preprint arXiv:1905.12658},
year = {2019}
}
Comments
Contribution to the Special Issue "Compact Stars in the QCD Phase Diagram and in the Multi-Messenger Era of Astronomy" dedicated to the conference: Compact Stars in the QCD Phase Diagram VII