Binary Neutron Stars in Quasi-equilibrium

Details Binary Neutron Stars in Quasi-equilibrium Binary Neutron Stars in Quasi-equilibrium

2010-05-06

arxiv.org/abs/1005.0958v1

Astrophysical Journal Supplement Series, 188 (2010) 187

Astronomy and Astrophysics

Astrophysics

Solar and Stellar Astrophysics

66 pages, 26 figures, 6 tables, aastex

Scientific paper

Quasi-equilibrium sequences of binary neutron stars are constructed for a variety of equations of state in general relativity. Einstein's constraint equations in the Isenberg-Wilson-Mathews approximation are solved together with the relativistic equations of hydrostationary equilibrium under the assumption of irrotational flow. We focus on unequal-mass sequences as well as equal-mass sequences, and compare those results. We investigate the behavior of the binding energy and total angular momentum along a quasi-equilibrium sequence, the endpoint of sequences, and the orbital angular velocity as a function of time, changing the mass ratio, the total mass of the binary system, and the equation of state of a neutron star. It is found that the orbital angular velocity at the mass-shedding limit can be determined by an empirical formula derived from an analytic estimation. We also provide tables for 160 sequences which will be useful as a guideline of numerical simulations for the inspiral and merger performed in the near future.

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