Binary Neutron Stars: Equilibrium Models beyond Spatial Conformal Flatness

Kōji Uryū, François Limousin, John L. Friedman, Eric Gourgoulhon, and Masaru Shibata
Phys. Rev. Lett. 97, 171101 – Published 27 October 2006

Abstract

Equilibria of binary neutron stars in close circular orbits are computed numerically in a waveless formulation: the full Einstein-relativistic-Euler system is solved on an initial hypersurface to obtain an asymptotically flat form of the 4-metric and an extrinsic curvature whose time derivative vanishes in a comoving frame. Two independent numerical codes are developed, and solution sequences that model inspiraling binary neutron stars during the final several orbits are successfully computed. The binding energy of the system near its final orbit deviates from earlier results of third post-Newtonian and of spatially conformally flat calculations. The new solutions may serve as initial data for merger simulations and as members of quasiequilibrium sequences to generate gravitational-wave templates, and may improve estimates of the gravitational-wave cutoff frequency set by the last inspiral orbit.

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  • Received 25 November 2005

DOI:https://doi.org/10.1103/PhysRevLett.97.171101

©2006 American Physical Society

Authors & Affiliations

Kōji Uryū1, François Limousin2, John L. Friedman1, Eric Gourgoulhon2, and Masaru Shibata3

  • 1Department of Physics, University of Wisconsin-Milwaukee, P.O. Box 413, Milwaukee, Wisconsin 53201, USA
  • 2Laboratoire de l’Univers et de ses Théories, UMR 8102 du CNRS, Observatoire de Paris, F-92195 Meudon Cedex, France
  • 3Department of Earth Science and Astronomy, Graduate School of Arts and Sciences, University of Tokyo, Komaba, Meguro, Tokyo 153-8902, Japan

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Issue

Vol. 97, Iss. 17 — 27 October 2006

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