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   PR # 12191
    Previous IPC and PSPC observations have shown that the coronae of
    many active stars are composed of multiple temperature components.The
    relatively poor sensitivity of those detectors to relevant temperatur
    e differences may make reliable estimates suspect,however. ASCA's uni
    que resolving power and sensitivity will allow us to determine whethe
    r the old multi-temperature models are appropriate or whether they mu
    st be replaced with a new generation of models in which EM(T) is deri
    ved explicitly from the lines. Our target list comprises very bright
    active stars, among them AU Mic, which has outstanding properties amo
    ng the nearest stars, and for which we possess unique complementary
    data sets (e.g.,from HST) crucial for a comprehensive modeling of its
   corona.
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