Irrotational binary neutron stars in quasiequilibrium

P. Marronetti, G. J. Mathews, and J. R. Wilson
Phys. Rev. D 60, 087301 – Published 15 September 1999
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Abstract

We report on numerical results from an independent formalism to describe the quasiequilibrium structure of nonsynchronous binary neutron stars in general relativity. This is an important independent test of controversial numerical hydrodynamic simulations which suggested that nonsynchronous neutron stars in a close binary can experience compression prior to the last stable circular orbit. We show that, for compact enough stars, the interior density increases slightly as irrotational binary neutron stars approach their last orbits. The magnitude of the effect, however, is much smaller than that reported in previous hydrodynamic simulations.

  • Received 24 June 1998

DOI:https://doi.org/10.1103/PhysRevD.60.087301

©1999 American Physical Society

Authors & Affiliations

P. Marronetti and G. J. Mathews

  • Department of Physics, University of Notre Dame, Notre Dame, Indiana 46556

J. R. Wilson

  • University of California, Lawrence Livermore National Laboratory, Livermore, California 94550

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Vol. 60, Iss. 8 — 15 October 1999

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