Relativistic formalism to compute quasiequilibrium configurations of nonsynchronized neutron star binaries

Silvano Bonazzola, Eric Gourgoulhon, and Jean-Alain Marck
Phys. Rev. D 56, 7740 – Published 15 December 1997
PDFExport Citation

Abstract

A general relativistic version of the Euler equation for perfect fluid hydrodynamics is applied to a system of two neutron stars orbiting each other. In the quasiequilibrium phase of the evolution of this system, a first integral of motion can be derived for certain velocity fields of the neutron star fluid including the (academic) case of corotation with respect to the orbital motion (synchronized binaries) and the realistic case of counter-rotation with respect to the orbital motion. The velocity field leading to this latter configuration can be computed by solving three-dimensional vector and scalar Poisson equations.

  • Received 7 July 1997

DOI:https://doi.org/10.1103/PhysRevD.56.7740

©1997 American Physical Society

Authors & Affiliations

Silvano Bonazzola, Eric Gourgoulhon, and Jean-Alain Marck

  • Département d’Astrophysique Relativiste et de Cosmologie, UPR 176 du C.N.R.S., Observatoire de Paris, F-92195 Meudon Cedex, France

References (Subscription Required)

Click to Expand
Issue

Vol. 56, Iss. 12 — 15 December 1997

Reuse & Permissions
Access Options
Author publication services for translation and copyediting assistance advertisement

Authorization Required


×
×

Images

×

Sign up to receive regular email alerts from Physical Review D

Log In

Cancel
×

Search


Article Lookup

Paste a citation or DOI

Enter a citation
×