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    PR # 32022                                                                   
     Contrary to the evidence suggested by Einstein and EXOSAT data, very        
     low-mass stars at the bottom of the main-sequence do have coronae.          
     These stars have completely convective structures and are slowly            
     rotating. The origin and energetics of their coronae are not                
     presently understood.  ROSAT recently measured the broadband X-ray          
     flux for only 8 of these stars, most of which are too faint and             
     either are close binaries or have nearby companions. CN Leo (dM6e,          
     $<$0.10 solar mass) provides the best opportunity to measure the            
     quiescent coronal spectrum with ASCA. Although a flare star, it is          
     relatively inactive, enabling its quiescent state to be measured. The       
     differential emission measure will be determined, and variability           
    searched for in the quiescent                                                
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