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APS » Journals » Phys. Rev. D » Volume 57 » Issue 10
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Phys. Rev. D 57, 6181–6184 (1998)

Stability of relativistic neutron stars in binary orbit

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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 12 May 1997; published in the issue dated 15 May 1998

We analyze the stability of relativistic, quasi-equilibrium binary neutron stars in synchronized circular orbit. We explore stability against radial collapse to black holes prior to merger, and against orbital plunge. We apply theorems based on turning points along uniformly rotating sequences of constant angular momentum and rest mass to locate the onset of secular instabilities. We find that inspiraling binary neutron stars are stable against radial collapse to black holes all the way down to the innermost stable circular orbit.

© 1998 The American Physical Society

URL:
http://link.aps.org/doi/10.1103/PhysRevD.57.6181
DOI:
10.1103/PhysRevD.57.6181
PACS:
04.40.Dg, 04.20.Ex, 04.25.Dm, 97.60.Jd
 
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