  The past growth of the central black hole (BH) might have enhanced the
density of cold dark matter halo particles at the Galactic center. We compute
this effect in realistic growth models of the present (2-3)*10**6 solar mass BH
from a low-mass seed BH, with special attention to dynamical modeling in a
realistic galaxy environment with merger and orbital decay of a seed BH formed
generally outside the exact center of the halo. An intriguing ``very-dense
spike'' of dark matter has been claimed in models of Gondolo and Silk with
density high enough to contradict with experimental upper bounds of neutralino
annihilation radiation. This ``spike'' disappears completely or is greatly
weakened when we include important dynamical processes neglected in their
idealized/restrictive picture with cold particles surrounding an at-the-center
zero-seed adiabaticly-growing BH. For the seed BH to spiral in and settle to
the center within a Hubble time by dynamical friction, the seed mass must be at
least a significant fraction of the present BH. Any subsequent at-the-center
growth of the BH and steepening of the central Keplerian potential well can
squeeze the halo density distribution only mildly, whether the squeezing
happens adiabatically or instantaneously.
