The Relativistic Roche Problem. I. Equilibrium Theory for a Body in Equatorial, Circular Orbit around a Kerr Black Hole

Fishbone, L.G.

doi:10.1086/152395

Cited by 69 publications

(77 citation statements)

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“…[16]) to compressible configurations. These ellipsoidal calculations have also been generalized to include relativistic effects [17,18,19]. Equilibrium models of Newtonian BHNS binaries also have been constructed by solving the exact fluid equations numerically and again treating the black hole as a point mass [20].…”

Section: Introductionmentioning

confidence: 99%

Black hole-neutron star binaries in general relativity: Quasiequilibrium formulation

2004

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We present a new numerical method for the construction of quasiequilibrium models of black holeneutron 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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Section: Introductionmentioning

confidence: 99%

Black hole-neutron star binaries in general relativity: Quasiequilibrium formulation

2004

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“…According to a study based on the tidal approximation (which is referred to as a study for configuration of a Newtonian star in circular orbits around a BH in its relativistic tidal field; e.g., [3,4,5,6,7]), the fate is classified into two cases, depending on the mass ratio q ≡ M NS /M BH , where M BH and M NS denote the masses of BH and NS, respectively. For q < ∼ q c , the NS of radius R will be swallowed into the BH horizon without tidal disruption before the orbit reaches the innermost stable circular orbit (ISCO) [5,6], while for q > ∼ q c , NS may be tidally disrupted before plunging into BH.…”

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Merger of black hole-neutron star binaries: Nonspinning black hole case

2006

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We perform a simulation for merger of a black hole (BH)-neutron star (NS) binary in full general relativity preparing a quasicircular state as initial condition. The BH is modeled by a moving puncture with no spin and the NS by the Γ-law equation of state with Γ = 2. Corotating velocity field is assumed for the NS. The mass of the BH and the rest-mass of the NS are chosen to be ≈ 3.2M⊙ and ≈ 1.4M⊙ with relatively large radius of the NS ≈ 14 km. The NS is tidally disrupted near the innermost stable orbit but ∼ 80% of the material is swallowed into the BH with small disk mass ∼ 0.3M⊙ even for such small BH mass ∼ 3M⊙. The result indicates that the system of a BH and a massive disk of ∼ M⊙ is not formed from nonspinning BH-NS binaries, although a disk of mass ∼ 0.1M⊙ is a possible outcome.

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“…Fully relativistic simulations of BHNS binaries have received far less attention. Most BHNS calculations to date, including quasiequilibrium (QE) calculations [10,11,12,13,14,15,16,17,18] and dynamical treatments [19,20,21,22,23,24,25], employ Newtonian gravitation in either some or all aspects of their formulation. We have recently launched a new effort to study BHNS binaries in a fully relativistic framework (see also [26,27]), first by constructing QE models [28,29] and then by employing them as initial data in dynamical simulations [7,30].…”

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Quasiequilibrium sequences of black-hole–neutron-star binaries in general relativity

et al. 2006

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We construct quasiequilibrium sequences of black hole-neutron star binaries for arbitrary mass ratios by solving the constraint equations of general relativity in the conformal thin-sandwich decomposition. We model the neutron star as a stationary polytrope satisfying the relativistic equations of hydrodynamics, and account for the black hole by imposing equilibrium boundary conditions on the surface of an excised sphere (the apparent horizon). In this paper we focus on irrotational configurations, meaning that both the neutron star and the black hole are approximately nonspinning in an inertial frame. We present results for a binary with polytropic index n = 1, mass ratio M Coalescing black hole-neutron star (hereafter BHNS) binaries are among the most promising sources of gravitational waves for laser interferometers [1,2,3,4]. BHNS mergers may reveal a wealth of astrophysical information (see e.g. [5]), and, along with mergers of binary neutron stars, are also considered primary candidates for central engines of short-duration gamma-ray bursts (SGRBs) [6,7,8]. Recent observations of several SGRBs localized by the Swift and HETE-2 satellites in regions with low star formation strongly suggest that a compact binary merger scenario for SGRBs is favored over models involving the collapse of massive stars (see, e.g., [9] and references cited therein).Significant effort has gone into the study of binary neutron stars and binary black holes, which are also promising sources of gravitational radiation. Fully relativistic simulations of BHNS binaries have received far less attention. Most BHNS calculations to date, including quasiequilibrium (QE) calculations [10,11,12,13,14,15,16,17,18] and dynamical treatments [19,20,21,22,23,24,25], employ Newtonian gravitation in either some or all aspects of their formulation. We have recently launched a new effort to study BHNS binaries in a fully relativistic framework (see also [26,27]), first by constructing QE models [28,29] and then by employing them as initial data in dynamical simulations [7,30]. So far we have focused on binaries for which the black hole mass is much greater than the neutron star mass. For binaries with such extreme mass ratios the rotation axis can be taken to pass through the center of the black hole, and the tidal effects of the neutron star on the black * Also at: Department of Physics, University of Illinois at UrbanaChampaign, Urbana, Illinois 61801, USA † Also at: Department of Astronomy and NCSA, University of Illinois at Urbana-Champaign, Urbana, Illinois 61801, USA hole may be ignored. These approximations simplify the problem considerably (see [28]). However, they break down for binaries containing comparable mass companions. Such systems are more suitable as SGRB candidates, because the tidal disruption of the neutron star by the black hole will occur near or outside the innermost stable circular orbit. This disruption may be necessary to create a gaseous accretion disk around the black hole capable of generating a SGRB [7]. Gravitational wav...

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The Relativistic Roche Problem. I. Equilibrium Theory for a Body in Equatorial, Circular Orbit around a Kerr Black Hole

Cited by 69 publications

References 0 publications

Black hole-neutron star binaries in general relativity: Quasiequilibrium formulation

Black hole-neutron star binaries in general relativity: Quasiequilibrium formulation

Merger of black hole-neutron star binaries: Nonspinning black hole case

Quasiequilibrium sequences of black-hole–neutron-star binaries in general relativity

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