Quasiequilibrium sequences of synchronized and irrotational binary neutron stars in general relativity. II. Newtonian limits

Keisuke Taniguchi, Eric Gourgoulhon, and Silvano Bonazzola
Phys. Rev. D 64, 064012 – Published 27 August 2001
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Abstract

We study equilibrium sequences of close binary systems composed of identical polytropic stars in Newtonian gravity. The solving method is a multidomain spectral method which we have recently developed. An improvement is introduced here for accurate computations of binary systems with a stiff equation of state (γ>2). The computations are performed for both cases of synchronized and irrotational binary systems with adiabatic indices γ=3,2.5,2.25,2, and 1.8. It is found that the turning points of total energy along a constant-mass sequence appear only for γ>~1.8 for synchronized binary systems and γ>~2.3 for irrotational ones. In the synchronized case, the equilibrium sequences terminate by the contact between the two stars. On the other hand, for irrotational binaries, it is found that the sequences terminate at a mass shedding limit which corresponds to a detached configuration.

  • Received 13 March 2001

DOI:https://doi.org/10.1103/PhysRevD.64.064012

©2001 American Physical Society

Authors & Affiliations

Keisuke Taniguchi, Eric Gourgoulhon, and Silvano Bonazzola

  • Département d’Astrophysique Relativiste et de Cosmologie, UMR 8629 du C.N.R.S., Observatoire de Paris, F-92195 Meudon Cedex, France

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Issue

Vol. 64, Iss. 6 — 15 September 2001

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