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   PR # 22007
    We propose to study the coronae of two of the most variable dMe stars
    (UV Cet, EQ Peg). Both targets are significantly variable on         
    timescales of 10 minutes and longer and frequently show strong X-ray 
    flares.  These stars have been suggested to show evidence for coronal
    heating by flare-like events. ASCA's spectral resolution will allow  
    us to get a detailed emission measure distribution as a function of  
    temperature both for quiescent and flaring states and to identify    
    high-T plasma (above 10 MK) with great accuracy. By fitting the      
    spectra, T-sensitive line blends will show whether dynamic processes 
    heat the coronae to a continuum of temperatures, or whether canonical
    2-T models apply. Knowledge of temperature distribution and          
   variability is crucial for the
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