Phys. Rev. Lett. 79, 1182 - 1185 (1997)Binary Neutron Stars in General Relativity: Quasiequilibrium Models |
PRL Celebrates 50 Years
This Week's Milestone Letters are from 1984: |
T. W. Baumgarte1, G. B. Cook2, M. A. Scheel2, S. L. Shapiro1,3, and S. A. Teukolsky2,4
1Department of Physics, University of Illinois at Urbana-Champaign, Urbana, Illinois 61801
2Center for Radiophysics and Space Research, Cornell University, Ithaca, New York 14853
3Department of Astronomy and NCSA, University of Illinois at Urbana-Champaign, Urbana, Illinois 61801
4Departments of Physics and Astronomy, Cornell University, Ithaca, New York 14853
Received 8 April 1997
We perform fully relativistic calculations of binary neutron stars in quasiequilibrium circular orbits. We integrate Einstein's equations together with the relativistic equation of hydrostatic equilibrium to solve the initial-value problem for equal-mass binaries of arbitrary separation. We construct sequences of constant rest mass and identify the innermost stable circular orbit and its angular velocity. We find that the quasiequilibrium maximum allowed mass of a neutron star in a close binary is slightly larger than in isolation.
©1997 The American Physical Society
URL: http://link.aps.org/abstract/PRL/v79/p1182
DOI: 10.1103/PhysRevLett.79.1182
PACS: 04.25.Dm, 04.30.Db, 04.40.Dg, 97.60.Jd
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