  The extremely young cluster IC 348 has been monitored in the Cousins I band
with a 0.6 m telescope at Wesleyan's Van Vleck Observatory. Photometry of 150
stars was obtained on 76 images taken on 27 separate nights during the period
December, 1998, through March, 1999. As expected, spectral characteristics
largely determine the nature of a star's variability in this cluster. None of
the stars with H-alpha in absorption were found to be variables. On the other
hand, all 16 stars identified as CTTS by their H-alpha emission equivalent
widths and the majority of the 49 WTTS in the part of the cluster we monitored
showed evidence of variability. Nineteen stars were found to be periodic, with
periods ranging from 2.24 to 16.2 days and masses ranging from 0.35 to 1.1
M-sun. Seventeen of these are WTTS and the other 2 are of unknown spectral
class. The period distribution is remarkably similar to what is found in the
Orion Nebula Cluster for stars in the same mass range. Namely, it is bimodal
with peaks at 2-3 days and 7-8 days, although there are not enough periods
known to define these features significantly by the IC 348 data alone. The
three fastest rotators are also the three most massive stars in the periodic
sample.
