  Self-consistent bars that form in galaxies embedded within cuspy halos are
unable to flatten the cusp. Short bars form in models with quasi-flat rotation
curves. They lose angular momentum to the halo through dynamical friction, but
the continuous concentration of mass within the disk as the bar grows actually
compresses the halo further, overwhelming any density reduction due to the
modest angular momentum transfer to the halo. Thus the Weinberg-Katz proposed
solution to the non-existence of the predicted cuspy halos from CDM simulations
would seem to be unworkable. I also find that the concerns over the performance
of N-body codes raised by these authors do not apply to the methods used here.
