  The dynamical evolution of super star clusters (SSCs) moving in the
background of a dark matter halo has been investigated as a possible event
responsible for the formation of bulges in late-type spirals. The underlying
physical processes include sinking of SSCs due to the dynamical friction and
stripping of SSCs on their way to the center. Our model calculations show that
only sinking of circumnuclear SSCs contributes to the formation of galactic
bulges at the early stage. Based on the assumption of a universal density
profile for the dark matter halo, and an isothermal model for the SSCs, our
simulations have yielded bulges that are similar in many aspects to the
observational ones. In particular, the derived surface density profiles can be
well fitted by anexponential structure with nuclear cusps, which is consistent
with HST observations.
