  We perform N-Body/SPH simulations of disk galaxy formation inside equilibrium
spherical and triaxial cuspy dark matter halos. We systematically study the
disk properties and morphology as we increase the numbers of dark matter and
gas particles from 10^4 to 10^6 and change the force resolution. The force
resolution influences the morphological evolution of the disk quite
dramatically. Unless the baryon fraction is significantly lower than the
universal value, with high force resolution a gaseous bar always forms within a
billion years after allowing cooling to begin. The bar interacts with the disk,
transferring angular momentum and increasing its scale length. In none of the
simulations does the final mass distribution of the baryons obey a single
exponential profile. Indeed within a few hundred parsecs to a kiloparsec from
the center the density rises much more steeply than in the rest of the disk,
and this is true irrespective of the presence of the bar.
