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   PR # 42003
   The X-ray coronae of Hertzsprung-gap giants are among the hottest
   known (log T > 7.3); reminiscent of flaring gas in solar active
   regions, or on RS CVn binaries and dMe stars. Yet, the F0-G1 giants
   as a class are not noted for transient UV or X-ray outbursts. The
   paradox (flare-temperature plasma, but lack of overt flaring
   behavior) bears on the nature of coronal heating at the crucial
   evolutionary juncture where shallow convective envelopes first
   emerge; the key transition between hot-star and cool-star X-ray
   activity. ASCA can add unique insight by directly detecting the
   highest excitation coronal gas; possible short-term variability of
   the multi-keV X-rays; and anomalies in the coronal abundances. 31
   Comae (G0 III), well-studied at other wavelengths, is the most
   promising target.
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