Black hole-neutron star binaries in general relativity: Quasiequilibrium formulation
We present a new numerical method for the construction of quasiequilibrium models of black hole-neutron star binaries. We solve the constraint equations of general relativity, decomposed in the conformal thin-sandwich formalism, together with the Euler equation for the neutron star matter. We take t...
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Veröffentlicht in: | Physical review. D, Particles and fields Particles and fields, 2004-09, Vol.70 (6), Article 064040 |
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Format: | Artikel |
Sprache: | eng |
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Zusammenfassung: | We present a new numerical method for the construction of quasiequilibrium models of black hole-neutron star binaries. We solve the constraint equations of general relativity, decomposed in the conformal thin-sandwich formalism, together with the Euler equation for the neutron star matter. We take the system to be stationary in a corotating frame and thereby assume the presence of a helical Killing vector. We solve these coupled equations in the background metric of a Kerr-Schild black hole, which accounts for the neutron star's black hole companion. In this paper we adopt a polytropic equation of state for the neutron star matter and assume large black hole-to-neutron star mass ratios. These simplifications allow us to focus on the construction of quasiequilibrium neutron star models in the presence of strong-field, black hole companions. We summarize the results of several code tests, compare with Newtonian models, and locate the onset of tidal disruption in a fully relativistic framework. |
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ISSN: | 1550-7998 0556-2821 1550-2368 1089-4918 |
DOI: | 10.1103/PhysRevD.70.064040 |