Rapidly rotating neutron stars with realistic nuclear matter equation of state
Abstract
We performed a comparison of three different numerical codes for constructing equilibrium models; (I) a code for static equilibrium configurations, (II) an implementation of the Hartle--Thorne slow-rotation approximation, (III) a numerical solution of the full Einstein equations by \texttt{LORENE}. We aimed to construct sequences of uniformly rotating configurations at various rotation frequencies up to the Keplerian frequency for a hybrid hadronic--quark matter EOS where a smooth transition is provided between two separate phases. We investigated the difference of between the results computed by the implementation of Hartle--Thorne slow-rotation approximation and by \texttt{LORENE/nrotstar}, respectively. We have conclude that the codes can the difference between the slow rotating and the fast-rotating approach increase exponentially, reaching 6.67% for the maximal mass configuration rotating at the Keplerian frequency.
Keywords
Cite
@article{arxiv.2212.04885,
title = {Rapidly rotating neutron stars with realistic nuclear matter equation of state},
author = {Balázs Kacskovics and Dániel Barta and Mátyás Zsolt Vasúth},
journal= {arXiv preprint arXiv:2212.04885},
year = {2023}
}
Comments
7 pages, 4 figures, conference proceeding