Dynamical evolution of black hole-neutron star binaries in general relativity: Simulations of tidal disruption

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Joshua A. Faber,¹ Thomas W. Baumgarte,^1,2 Stuart L. Shapiro,¹ Keisuke Taniguchi,¹ and Frederic A. Rasio³
¹Department of Physics, University of Illinois at Urbana-Champaign, Urbana, Illinois 61801, USA
²Department of Physics and Astronomy, Bowdoin College, Brunswick, Maine 04011, USA
³Department of Physics and Astronomy, Northwestern University, Evanston, Illinois, 60208, USA

Received 13 July 2005; published 18 January 2006

Wecalculate the first dynamical evolutions of merging black hole-neutron starbinaries that construct the combined black hole-neutron star spacetime ina general relativistic framework. We treat the metric in theconformal flatness approximation, and assume that the black hole massis sufficiently large compared to that of the neutron starso that the black hole remains fixed in space. Usinga spheroidal spectral methods solver, we solve the resulting fieldequations for a neutron star orbiting a Schwarzschild black hole.The matter is evolved using a relativistic, Lagrangian, smoothed particlehydrodynamics (SPH) treatment. We take as our initial data recentquasiequilibrium models for synchronized neutron star polytropes generated as solutionsof the conformal thin-sandwich (CTS) decomposition of the Einstein fieldequations. We are able to construct from these models relaxedSPH configurations whose profiles show good agreement with CTS solutions.Our adiabatic evolution calculations for neutron stars with low-compactness showthat mass transfer, when it begins while the neutron starorbit is still outside the innermost stable circular orbit, ismore unstable than is typically predicted by analytical formalisms. Thisdynamical mass loss is found to be the driving forcein determining the subsequent evolution of the binary orbit andthe neutron star, which typically disrupts completely within a feworbital periods. The majority of the mass transferred onto theblack hole is accreted promptly; a significant fraction (~30%) ofthe mass is shed outward as well, some of whichwill become gravitationally unbound and ejected completely from the system.The remaining portion forms an accretion disk around the blackhole, and could provide the energy source for short-duration gamma-raybursts.

URL:	http://link.aps.org/doi/10.1103/PhysRevD.73.024012
DOI:	10.1103/PhysRevD.73.024012
PACS:	04.30.Db; 04.25.Dm; 47.11.Kb; 95.85.Sz 04.30.Db Gravitational wave generation and sources 04.25.Dm Numerical relativity 47.11.Kb Spectral methods 95.85.Sz Gravitational radiation, magnetic fields, and other astronomical observations YEAR: 2006
KEYWORDS:	black holes, neutron stars, binary stars, space-time configurations, Einstein field equations, stellar mass, Schwarzschild metric, accretion disks, gamma-ray bursts

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