Variability in the Young, Open Cluster NGC2301

What percent of stars are variable? How does variability depend on the age and mass of a star? Through the study of the young (approx. 164Myr), metal rich [Fe/H]=+0.06, open cluster NGC2301 we have provided some answers to these questions. Observations were collected over 12 consecutive nights using the University of Hawaii 88" telescope on Mauna Kea. Using an orthogonal transfer CCD camera, the technique of PSF shaping was employed and used to produce ``square stars". Over 4000 cluster stars were examined. B and R band magnitudes, with limits to B=21.5 and R=19.5, were used to produce a color-magnitude diagram for NGC2301. The CMD shows a well defined main sequence covering stars from late B to mid-M spectral classes. We find that 56% of the stars observed were variable with roughly 7% of the observed stars were found to be periodic. Variability ranges from a few mmag to > 4 magnitudes with periods from tens of minutes to many days. We present a statistical study of these data in terms of color and variability type.