  The question whether the dark matter halo density in the centers of galaxies
could be changed through interactions with a rotating bar in the baryonic disk
is of considerable current interest. While N-body simulations have been used to
address this question, it has also been claimed that results from such
simulations cannot be trusted. Based on a perturbative treatment of resonant
exchanges between orbits and a rotating perturbation, Weinberg & Katz contend
that N-body simulations of this process will not reveal the continuum result
unless many more than the usual numbers of particles are employed. Here I
report a study designed to examine their contention, finding results that show
no dependence on the number of particles over the range usually employed up to
that advocated by these authors. I show that my results are independent of all
numerical parameters, and that field methods perform equally with grid methods
in this respect. I also identify the reasons that the required particle number
suggested by Weinberg & Katz is excessive.
