  We contrast the evolution of gravitational binary mergers for the two cases
of a black hole and a normal neutron star, and a black hole and a self-bound
strange quark matter star. In both cases inspiral continues until the Roche
limit is reached, at which point it is expected that stable mass transfer to
the balck hole ensues. Whereas a neutron star would then outspiral, the strange
quark matter star barely moves out at all. Eventually, the strange quark star
loses all its mass to the black hole, as compared to the neutron star whose
outspiral continues until stable mass transfer terminates and inspiral resumes.
These scenarios result in distinctly different gravitational wave signatures.
