*Initial Configuration*

Stars A and C obey a n = 1 polytropic equation of state, P=Kρ^{Γ}_{0}, at
t = 0. They are evolved according to the adiabatic evolution law,
P=(Γ-1)ρ_{0}&epsilon, where P is the pressure, K the polytropic constant, &epsilon
is the internal specific energy, and ρ_{0} the rest-mass density. We chose Γ = 2
to mimick stiff nuclear matter. Both stars are irrotational (nonspinning) and are in a
quasiequilibrium circular orbit.

We consider two differing BHNS mass ratios: case A1-farbc, with mass ratio
M_{BH}:M_{NS} = 3:1 and case C, with a mass ratio M_{BH}:M_{NS} =
1:1. The initial compaction of the neutron star for both cases is M_{NS}/R_{NS} = 0.145.

last updated 8 July 08 by AH