******************************************************
   PR # 22011
    We propose ASCA observations of a sample of 3 X-ray-bright G-type    
    pre-main sequence stars. These 2 solar mass stars are about 2 million
    years old, and near the base of their Hayashi tracks.  The large     
    X-ray luminosities are presumably indicative of the presence of a    
    magnetic dynamo.  However, there is evidence that the emission       
    measure distributions differ from those of older active late-type    
    stars. We propose to measure the coronal emission measure            
    distribution directly, and use it together with existing UV spectra  
    to study the coronal heating in these stars and search for           
    differences in the atmospheres. Such differences may be attributable 
    to the different interior structure, and presumably different dynamo 
   operation, in these fully conv
 ******************************************************