A large, deep, and nearly complete B < 24.5 redshift sample is used to
measure the change with redshift in the distribution function of the
stellar mass production rate in individual galaxies. The evolution of
the star formation rate distribution with redshift is interpreted in t
erms of the history of spiral galaxy formation, with the disk componen
t modeled as a single evolving entity, and the characteristic timescal
es, luminosities, and epochs varying according to galaxy type. The mor
e massive forming galaxies seen at z = 1-3 are identified as earlier t
ype spirals, whose star formation rates are initially high and then de
cline rapidly at z < 1, while for later type spirals and smaller mass
irregulars the mass formation rates at z < 1 are lower, and the format
ion process persists to redshifts much closer to the present epoch. We
find that these models can be consistent with the data and fit well i
nto a broad picture of other recent results if q(0) = 0.02 and many of
the disks begin their growth at z much less than 3, but that they pre
dict too many bright star formers at high z in flat universes.