  We present a scenario for the formation and evolution of disk galaxies within
the framework of an inflationary CDM universe, and we compare the results with
observations ranking from the present-day up to z~1. Galactic disks are
built-up inside-out by gas infall with accretion rates driven by the
cosmological mass aggregation history (MAH). We generate the MAHs for a
Gaussian density fluctuation field, and we calculate the gravitational collapse
and virialization of the dark halos. Assuming detailed angular momentum
conservation, disks in centrifugal equilibrium are built-up within them. The
disk galactic evolution is followed through a physically self-consistent
approach. The main disk galaxy properties and their correlations are determined
by the mass, the MAH, and the spin parameter. The models give exponential disk
surface brightness (SB) profiles with realistic parameters (including LSB
galaxies), nearly flat rotation curves, and negative gradients in the B-V
radial profile. The main trends across the Hubble sequence are reproduced. A
maximum in the star formation rate for most of the models is attained at z~
1.5-2.5 (this rate is approximately 2.5-4.0 times larger than the present one).
The scale radii and the bulge-to-total ratios decrease with z, while the
central SB increase. The B-band TF relation remains almost the same at
different redshifts. Our scenario reveals that the cosmological initial
conditions are able to determine the main properties of disk galaxies and
predict evolutionary features for the present-day dominant galaxy population
that are in agreement with very recent deep field observational studies.
