Binary Neutron Stars in Quasi-Equilibrium Circular Orbit: A Fully Relativistic Treatment

Details Binary Neutron Stars in Quasi-Equilibrium Circular Orbit: A Fully Relativistic Treatment Binary Neutron Stars in Quasi-Equilibrium Circular Orbit: A Fully Relativistic Treatment

1997-01-14

arxiv.org/abs/gr-qc/9701033v1

Astronomy and Astrophysics

Astrophysics

General Relativity and Quantum Cosmology

3 pages LaTeX using sprocl.sty, 2 figures, to appear in: Proceedings of the 18th Texas Symposium on Relativistic Astrophysics

Scientific paper

We present a numerical scheme that solves the initial value problem in full general relativity for a binary neutron star in quasi-equilibrium. While Newtonian gravity allows for a strict equilibrium, a relativistic binary system emits gravitational radiation, causing the system to lose energy and slowly spiral inwards. However, since inspiral occurs on a time scale much longer than the orbital period, we can adopt a quasi-equilibrium approximation. In this approximation, we integrate a subset of the Einstein equations coupled to the equations of relativistic hydrodynamics to solve the initial value problem for binaries of arbitrary separation, down to the innermost stable orbit.

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