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    PR # 32006                                                                   
     The solar coronal abundance anomaly known as the ``FIP Effect''    re       
     mains somewhat of a mystery.  ASCA observations of the active stars c       
     hi 1 Ori (GO V), xi Boo A (G8 V) and Wolf 630 (dM3e), and of the    l       
     ower activity binary alpha Cen A,B will yield their coronal         a       
     bundances of N, O, Ne, S (high FIP) and Mg, Si, Fe (low FIP).       W       
     hether or not a FIP-like effect, or other abundance anomaly, is     p       
     revalent in these stars is of central importance for the field of   s       
     tellar coronae, for models seeking to explain the solar FIP effect, a       
     nd for a possible origin of the galactic cosmic rays.                       
                                                                                 
                                                                                 
                                                                                 
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