  Positions of High-Mass X-ray Binaries are often known precisely enough to
unambiguously identify the optical component, and a number of those stars are
monitored by the OGLE and MACHO collaborations. The light curves of two such
candidates are examined for evidence of Be star behavior and for periodicity.
One of the stars exhibits two periods of 6.833 and 15.586 hours, much shorter
and more stable than periods of Be/X-Ray Binaries that are attributed to the Be
star's disk, but consistent with short-term Be variability attributed to
pulsations. The multiperiodicity is quantified with Fourier techniques and
examined for phase stability; a combination of radial and non-radial pulsations
is discussed.
