  We use kinematic measurements of a large sample of galaxies from the Team
Keck Redshift Survey in the GOODS-N field to measure evolution in the optical
and near-IR Tully-Fisher relations to z = 1.2. We construct Tully-Fisher
relations with integrated line-of-sight velocity widths of ~ 1000 galaxies in B
and ~ 670 in J-band; these relations have large scatter, and we derive a
maximum-likelihood least squares method for fitting in the presence of scatter.
The B-band Tully-Fisher relations, from z=0.4 to z=1.2, show evolution of ~
1.0-1.5 mag internal to our sample without requiring calibration to a local TF
relation. There is evolution in both Tully-Fisher intercept and slope,
suggesting differential luminosity evolution. In J-band, there is evolution in
slope but little evolution in overall luminosity. The slope measurements imply
that bright, massive blue galaxies fade {\it more strongly} than fainter blue
galaxies from z ~ 1.2 to now. This conclusion runs counter to some previous
measurements and to our naive expectations, but we present a simple set of star
formation histories to show that it arises naturally if massive galaxies have
shorter timescales of star formation, forming most of their stars before z ~ 1,
while less massive galaxies form stars at more slowly declining rates. This
model predicts that the higher global star formation rate at z ~ 1 is mostly
due to higher SFR in massive galaxies. The amount of fading in B-band
constrains star formation timescale more strongly than redshift of formation.
Tully-Fisher and color-magnitude relations can provide global constraints on
the luminosity evolution and star formation history of blue galaxies.
