  Gamma Cas (B0.5IVe) is the noted prototype of a subgroup of classical Be
stars exhibiting hard thermal X-ray emission. This paper reports results from a
23-year optical campaign with an Automated Photometric Telescope (APT) on this
star. A series of unstable long cycles of length 56--91 days has nearly ceased
over the last decade. Herein, we revise the frequency of the dominant coherent
signal at 0.82238 cy/d. This signal's amplitude has nearly disappeared in the
last 15 years but has somewhat recovered its former strength. We confirm the
presence of secondary nonradial pulsation signals found by other authors at
frequencies 1.25, 2.48, and 5.03 cy/d. The APT data from intensively monitored
nights reveal rapidly variable amplitudes among these frequencies. We show that
peculiarities in the 0.82 cy/d waveform exist that can vary even over several
days. Although the 0.82 cy/d frequency is near the star's presumed rotation
frequency. However, because of its phase slippage with respect to a dip pattern
in the star's far-UV light curve it is preferable to consider the latter
pattern, not the 0.82 cy/d signal, that carries a rotation signature. We also
find hints of the UV dip pattern in periodograms of early-season APT data.
Last, we discuss a fading outburst in a recent TESS light curve of gamma Cas.
This fading is an initial abrupt 1.5% absorption. Its recovery to its initial
flux requires 9-days, a circumstance we attribute to magnetic confinement of an
ejected blob suspended over its surface.
