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   PR # 12115
      We propose to use ASCA spectra of O stars to address the following
    questions: 1)What is the temperature distribution of the emission?
    2) Do O stars show hard, non-thermal X-ray tails?  3) What does the
    observed line emission tell us about chemical abundances? 4) What is
    the level of variability of the X-ray emission?We will also determine
    if the observed X-ray flux is sufficient to produce the strengths of
    the "superionized" OVI lines observed in the UV. We will also examine
    the importance of circumstellar (wind) absorption, though this is
    expected to be minimal for the stars selected.



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