The Relativitic Evolution of Black Hole-Neutron Star Binaries

Details The Relativitic Evolution of Black Hole-Neutron Star Binaries The Relativitic Evolution of Black Hole-Neutron Star Binaries

Dec 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004aas...205.7604f&link_type=abstract

American Astronomical Society Meeting 205, #76.04; Bulletin of the American Astronomical Society, Vol. 36, p.1473

Astronomy and Astrophysics

Astrophysics

Scientific paper

We report results from our new relativistic evolution calculations of black hole-neutron star (BH-NS) binaries. The evolution equations of general relativity are treated in the conformally flat (CF) approximation. Assuming that the BH mass is significantly larger than that of the NS allows us to simplify the field equations for the NS, which we solve self-consistently in a fixed BH background spacetime. This approach guarantees that self-gravity is fully included. The NS fluid, assumed here to follow a gamma-law equation of state (EOS), is evolved using a Lagrangian SPH method. The field equations are solved by spectral methods in spheroidal coordinates. The code has been tested by comparing our results to previously computed quasi-equilibrium sequences, showing good agreement.
Our results are a crucial first step in evaluating the stability of mass transfer in extremely close BH-NS binaries. They will allow us to describe quantitatively the dynamical tidal disruption of the NS, and to determine the dependence on the initial binary parameters, including the mass ratio and assumed NS EOS. We will also discuss the implications for detecting gravitational waves from the merger of these systems, about which, in contrast to NS-NS binaries, little is currently known for systems with components of comparable mass.
JAF is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-0401533.

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