Binary Neutron Stars in Quasi-equilibrium
Abstract
Quasi-equilibrium sequences of binary neutron stars are constructed for a variety of equations of state in general relativity. Einstein's constraint equations in the Isenberg-Wilson-Mathews approximation are solved together with the relativistic equations of hydrostationary equilibrium under the assumption of irrotational flow. We focus on unequal-mass sequences as well as equal-mass sequences, and compare those results. We investigate the behavior of the binding energy and total angular momentum along a quasi-equilibrium sequence, the endpoint of sequences, and the orbital angular velocity as a function of time, changing the mass ratio, the total mass of the binary system, and the equation of state of a neutron star. It is found that the orbital angular velocity at the mass-shedding limit can be determined by an empirical formula derived from an analytic estimation. We also provide tables for 160 sequences which will be useful as a guideline of numerical simulations for the inspiral and merger performed in the near future.
Cite
@article{arxiv.1005.0958,
title = {Binary Neutron Stars in Quasi-equilibrium},
author = {Keisuke Taniguchi and Masaru Shibata},
journal= {arXiv preprint arXiv:1005.0958},
year = {2015}
}
Comments
66 pages, 26 figures, 6 tables, aastex