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   72001
   The rapidly rotating non-radial pulsator, Zeta Oph, an O9.5V(e) star,
   has a history of mass ejections and the formation of shells. Over a
   period of 15 years, this star has been observed by the IPC, PSPC, and
   SIS instruments. The combined observations suggest that the emission
   appears to be monotonically increasing (a factor of 3 increase in flux
   over this time span). During the last 5 years, the rate of change in X-
   ray emission increased a factor of 10 as compared to the rate between
   1980 and 1990. This rate change may be due to the distortion of surface
   magnetic field activity, and a precursor to another mass ejection.
   Spectral analysis of our previous ASCA observation of this star
   supports this scenario. We propose two ASCA observations to continue
   monitoring this O star.
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