  We present a dynamical friction model based on Chandrasekhar's formula that
reproduces the fast inspiral and stalling experienced by satellites orbiting
galaxies with a large constant density core. We show that the fast inspiral
phase does not owe to resonance. Rather, it owes to the background velocity
distribution function for the constant density cores being dissimilar from the
usually-assumed Maxwellian distribution. Using the correct background velocity
distribution function and the semi-analytic model from Petts et al. (2015), we
are able to correctly reproduce the infall rate in both cored and cusped
potentials. However, in the case of large cores, our model is no longer able to
correctly capture core-stalling. We show that this stalling owes to the tidal
radius of the satellite approaching the size of the core. By switching off
dynamical friction when rt(r) = r (where rt is the tidal radius at the
satellite's position) we arrive at a model which reproduces the N-body results
remarkably well. Since the tidal radius can be very large for constant density
background distributions, our model recovers the result that stalling can occur
for Ms/Menc << 1, where Ms and Menc are the mass of the satellite and the
enclosed galaxy mass, respectively. Finally, we include the contribution to
dynamical friction that comes from stars moving faster than the satellite. This
next-to-leading order effect becomes the dominant driver of inspiral near the
core region, prior to stalling.
