  We present a study of the B and Be star populations of the Double Cluster h
and chi Persei. Blue optical spectroscopy is used to first measure projected
rotational velocity, V sin i, effective surface temperature, T_eff, and surface
gravity, log g, for B-type sample stars, while available Stromgren photometry
is used to calculate T_eff and log g for the Be stars showing emission. In our
sample of 104 objects for which we measured these stellar parameters, 28 are
known or proposed Be stars. Of these Be stars, 22 show evidence of emission at
the times of our observations, and furthermore, we find evidence in our data
and the literature for at least 8 transient Be stars in the clusters. We find
that the Be stars are not rotating near their critical velocity, contrary to
the results of studies of similar open clusters. We compare the results of our
analysis with other previous studies, and find that the cluster members are
more evolved than found by Huang & Gies but still retain much of their initial
rotational angular momentum.
