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   62015
   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 (1980-1995), the combined IPC, PSPC, and SIS
   observations of this star suggest that the X-ray emission appears to be
   monotonically increasing, displaying 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. Based on spectral analyses we argue that this rate
   change, probably due to the distortion of surface magnetic field
   activity, may be a precursor to another mass ejection. We propose two
   ASCA SIS observations to continue monitoring this very unusual single O
   star behavior.
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