A relativistic formalism to compute quasi-equilibrium configurations of non-synchronized neutron star binaries
arXiv:gr-qc/9710031 · doi:10.1103/PhysRevD.56.7740
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.
14 pages, 1 PostScript figure, RevTeX, accepted for publication in Physical Review D
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