Hydrodynamic Simulations of Mergers of Neutron Stars and Newtonian Black Holes

Details Hydrodynamic Simulations of Mergers of Neutron Stars and Newtonian Black Holes Hydrodynamic Simulations of Mergers of Neutron Stars and Newtonian Black Holes

May 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996aas...188.8404l&link_type=abstract

American Astronomical Society, 188th AAS Meeting, #84.04; Bulletin of the American Astronomical Society, Vol. 28, p.960

Astronomy and Astrophysics

Astronomy

Scientific paper

We have performed Newtonian smooth particle hydrodynamic simulations for the merger of a 1.4 Msun neutron star with a black hole in a compact binary system. The neutron star is modeled as a stiff polytrope and the black hole is treated as a point mass. Initial results for a mass ratio q=MNS/MBH=1 (Lee & Kluzniak, 1995), have shown that a hydrodynamical instability leads to violent disruption of the system on a dynamical timescale. We present preliminary results for different mass ratios (q <= 1), which exhibit qualitatively different behavior. The gravitational radiation waveforms produced during the event are computed in the quadrupole approximation. Implications for the likelihood of such events being the source of gamma ray bursts are discussed. Lee, W.H., Kluzniak, W., \em{Acta Astron., {45}, 1995, 705. }

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