  We examine the star-forming history (SFH) of the M31 disk during the past few
hundred Myr. The luminosity functions (LFs) of main sequence stars at distances
R_GC > 21 kpc (i.e. > 4 disk scale lengths) are matched by models that assume a
constant star formation rate (SFR). However, at smaller R_GC the LFs suggest
that during the past ~10 Myr the SFR was 2 - 3 times higher than during the
preceding ~100 Myr. The rings of cool gas that harbor a significant fraction of
the current star-forming activity are traced by stars with ages ~100 Myr,
indicating that (1) these structures have ages of at least 100 Myr, and (2)
stars in these structures do not follow the same relation between age and
random velocity as their counterparts throughout the disks of other spiral
galaxies, probably due to the inherently narrow orbital angular momentum
distribution of the giant molecular clouds in these structures. The
distribution of evolved red stars is not azimuthally symmetric, in the sense
that their projected density along the north east segment of the major axis is
roughly twice that on the opposite side of the galaxy. The north east arm of
the major axis thus appears to be a fossil star-forming area that dates to
intermediate epochs. Such a structure may be the consequence of interactions
with a companion galaxy.
