Published August 18, 1997
| Published + Submitted
Journal Article
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Binary Neutron Stars in General Relativity: Quasiequilibrium Models
Chicago
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Abstract
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.
Additional Information
© 1997 American Physical Society. (Received 8 April 1997) It is a pleasure to thank Manish Parashar for his help with the implementation of DAGH, and Andrew Abrahams, James Lombardi, and Fred Rasio for several helpful discussions. This work was supported by NSF Grant AST 96-18524 and NASA Grant NAG 5-3420 at Illinois, NSF Grant PHY 94-08378 at Cornell, and by the NSF Binary Black Hole Grand Challenge Grant Nos. NSF PHY 93-18152/ASC 93-18152 (ARPA supplemented).Attached Files
Published - PhysRevLett.79.1182.pdf
Submitted - 9704024.pdf
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9704024.pdf
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Additional details
- Alternative title
- Binary Neutron Stars in General Relativity: Quasi-Equilibrium Models
- Eprint ID
- 87493
- Resolver ID
- CaltechAUTHORS:20180629-152837218
- NSF
- AST 96-18524
- NASA
- NAG 5-3420
- NSF
- PHY 94-08378
- NSF
- PHY 93-18152
- NSF
- ASC 93-18152
- Advanced Research Projects Agency (ARPA)
- Created
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2018-06-29Created from EPrint's datestamp field
- Updated
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2021-11-15Created from EPrint's last_modified field