Hydrodynamics of black hole-neutron star coalescence

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dc.creatorLee, William H.
dc.creatorKluzniak, Wlodzimierz
dc.date1999-03-31
dc.date.accessioned2026-07-07T02:31:05Z
dc.date.available2026-07-07T02:31:05Z
dc.descriptionWe present a numerical study of the hydrodynamics in the final stages of inspiral in a black hole-neutron star binary, when the separation becomes comparable to the stellar radius. We use a Newtonian three-dimensional Smooth Particle Hydrodynamics (SPH) code, and model the neutron star with a soft (adiabatic index Gamma=5/3) polytropic equation of state and the black hole as a Newtonian point mass which accretes matter via an absorbing boundary at the Schwarzschild radius. Our initial conditions correspond to tidally locked binaries in equilibirium. The dynamical evolution is followed for approximately 23 ms, and in every case for Gamma=5/3 we find that the neutron star is tidally disrupted on a dynamical timescale, forming a dense torus around the black hole that contains a few tenths of a solar mass. A nearly baryon-free axis is present in the system throughout the coalescence, a fireball expanding along that axis would avoid excessive baryon contamination and could give rise to a modestly beamed gamma-ray burst.
dc.descriptionTo appear in the proceedings of the XIX Texas Symposium on Relativistic Astrophysics and Cosmology (Paris, December 1998)
dc.identifierhttps://arxiv.org/abs/astro-ph/9903488
dc.identifierhttp://arxiv.org/abs/astro-ph/9903488
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/14040
dc.subjectAstrophysics
dc.titleHydrodynamics of black hole-neutron star coalescence
dc.typetext

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