Revised Relativistic Hydrodynamical Model for Neutron-Star Binaries

Details Revised Relativistic Hydrodynamical Model for Neutron-Star Binaries Revised Relativistic Hydrodynamical Model for Neutron-Star Binaries

1999-11-11

arxiv.org/abs/gr-qc/9911047v1

Phys.Rev. D61 (2000) 127304

Astronomy and Astrophysics

Astrophysics

General Relativity and Quantum Cosmology

Submitted to Phys. Rev. D

Scientific paper

10.1103/PhysRevD.61.127304

We report on numerical results from a revised hydrodynamic simulation of binary neutron-star orbits near merger. We find that the correction recently identified by Flanagan significantly reduces but does not eliminate the neutron-star compression effect. Although results of the revised simulations show that the compression is reduced for a given total orbital angular momentum, the inner most stable circular orbit moves to closer separation distances. At these closer orbits significant compression and even collapse is still possible prior to merger for a sufficiently soft EOS. The reduced compression in the corrected simulation is consistent with other recent studies of rigid irrotational binaries in quasiequilibrium in which the compression effect is observed to be small. Another significant effect of this correction is that the derived binary orbital frequencies are now in closer agreement with post-Newtonian expectations.

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