Merger of a neutron star with a Newtonian black hole

Newtonian smooth particle hydro simulations are presented of the merger of a 1.4 M. neutron star with a black hole of equal mass. The initial state of the system is modeled with a stiff polytrope orbiting a point mass. Dynamical instability sets in when the orbital separation is equal to about three stellar radii. The ensuing mass transfer occurs on the dynamical timescale. No accretion torus is formed. At the end of the computation a corona of large extent shrouds an apparently stable binary system of a 0.25 M. star orbiting a 2.3 M. black hole.