Initial Configuration

Stars A and C obey a n = 1 polytropic equation of state, P=Kρ^Γ₀, at t = 0. They are evolved according to the adiabatic evolution law, P=(Γ-1)ρ₀&epsilon, where P is the pressure, K the polytropic constant, &epsilon is the internal specific energy, and ρ₀ 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