  The star formation history of the northern and southern M31 disk is measured
using samples of BV photometry for 4' X 4' regions taken from the KPNO/CTIO
Local Group Survey (Massey et al. 2001). The distances, mean reddening values,
and age distributions of the stars in these regions were measured using the
routines of Dolphin (1997, 2002). Independent measurements of overlapping
fields show that the results are stable for most samples. A slight distance
gradient is seen across the major axis of the southern disk, and a mean
distance of 24.47+/-0.03 is found by combining the results. Higher mean
reddening values follow the spiral structure. The stellar age distributions are
consistent with episodic star formation confined mainly to the gas-rich arm
regions. If these episodes were caused by propagating density waves, the waves
did not cause significant star formation episodes in the gas-poor interarm
regions. Combination of all of the results provides the total star formation
rate for 1.4 square degrees of the M31 disk for six epochs. These results
suggest that star formation in the disk declined by ~50% from ~250 to ~50 Myr
ago. The lowest star formation rate occurred ~25 Myr ago followed by a ~20%
increase to the present. The mean star formation rate for this large portion of
M31 over the past 60 Myr is 0.63+/-0.07 solar masses per year, suggesting a
total mean rate for the disk of ~1 solar masses per year.
