Binary Neutron Stars in Quasi-Equilibrium Circular Orbit: A Fully Relativistic Treatment

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dc.creatorBaumgarte, Thomas W.
dc.creatorShapiro, Stuart L.
dc.creatorCook, Gregory B.
dc.creatorScheel, Mark A.
dc.creatorTeukolsky, Saul A.
dc.date1997-01-14
dc.date.accessioned2026-07-07T03:31:26Z
dc.date.available2026-07-07T03:31:26Z
dc.descriptionWe present a numerical scheme that solves the initial value problem in full general relativity for a binary neutron star in quasi-equilibrium. While Newtonian gravity allows for a strict equilibrium, a relativistic binary system emits gravitational radiation, causing the system to lose energy and slowly spiral inwards. However, since inspiral occurs on a time scale much longer than the orbital period, we can adopt a quasi-equilibrium approximation. In this approximation, we integrate a subset of the Einstein equations coupled to the equations of relativistic hydrodynamics to solve the initial value problem for binaries of arbitrary separation, down to the innermost stable orbit.
dc.description3 pages LaTeX using sprocl.sty, 2 figures, to appear in: Proceedings of the 18th Texas Symposium on Relativistic Astrophysics (eds Olinto, Frieman and Schramm, World Scientific)
dc.identifierhttps://arxiv.org/abs/gr-qc/9701033
dc.identifierhttp://arxiv.org/abs/gr-qc/9701033
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/35861
dc.subjectGeneral Relativity and Quantum Cosmology
dc.subjectAstrophysics
dc.titleBinary Neutron Stars in Quasi-Equilibrium Circular Orbit: A Fully Relativistic Treatment
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