  I show that the predicted densities of the inner dark matter halos in LCDM
models of structure formation appear to be higher than estimates from real
galaxies and constraints from dynamical friction on bars. This inconsistency
would not be a problem for the LCDM model if physical processes that are
omitted in the collisionless collapse simulations were able to reduce the dark
matter density in the inner halos. I review the mechanisms proposed to achieve
the needed density reduction.
