  We consider spherically symmetric accretion onto a small, possibly
primordial, black hole residing at the center of a neutron star governed by a
cold nuclear equation of state (EOS). We generalize the relativistic Bondi
solution for such EOSs, approximated by piecewise polytropes, and thereby
obtain analytical expressions for the steady-state matter profiles and
accretion rates. We compare these rates with those found by time-dependent,
general relativistic hydrodynamical simulations upon relaxation and find
excellent agreement. We consider several different candidate EOSs, neutron star
masses and central densities and find that the accretion rates vary only
little, resulting in an accretion rate that depends primarily on the black hole
mass, and only weakly on the properties of the neutron star.
