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   PR # 12011
    A few active stars show very strong He I D3 absorption. In the Sun,
    similarly excited He I is directly associated with the Solar corona
    and is reasonably modeled by coronal-flux induced photoionization and
    recombination in the lower atmosphere.Active cool stars,such as RSCVn
    binaries,are well known coronal sources which are not well character-
    ized by a single temperature; they require material near 2and 20 MK.
    Why {\em more} such stars don't show D3 absorption iscurious. ASCA
    data will allow improved emission measure analyses through better ene
    rgy resolution. I propose to observe several activestars with strong
    D3. Coronae will be characterized differentially from star to star by
    fitting plasma emission models. Significant line strength variations
   can be detected in SIS spectra
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