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A relativistic formalism to compute quasi-equilibrium configurations of non-synchronized neutron star binaries

S. Bonazzola·E. Gourgoulhon·J. -A. Marck
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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 quasi-equilibrium 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 co-rotation 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.

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BibTeXRIS

S. Bonazzola, E. Gourgoulhon, J. -A. Marck. 1997-10-06. A relativistic formalism to compute quasi-equilibrium configurations of non-synchronized neutron star binaries. https://doi.org/10.1103/physrevd.56.7740

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