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   PR # 21501
    We propose to use 20 ksec of observing time aimed at RS CVn-type     
    binary CF Tuc in order to perform a temperature analysis of the      
    coronal plasma with the ASCA SIS.  We show that the Fe XXV-XXVI      
    complex at 6.7 keV will be detectable during the quiescent state of  
    the star.  However, we have found a very energetic long-duration  (9 
    days) flare in an extended ROSAT observation of CF Tuc.  Should ASCA 
    catch a similar event it will be possible to perform a detailed in-  
    vestigation of the Fe line complex. Ideally, we would like to have   
    the ASCA observation performed during a 300 ksec EUVE pointing al-   
    ready allocated to us in order to compare the temperature diagnostics
    obtained by both instruments. Simultaneousness is,however, not a     
   strict requirement of this pro
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