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    PR # 31507                                                                   
     GINGA observations of the RS CVn binary II Peg have revealed in the q       
     uiescent X-ray spectrum the presence of a power-law tail up to 18 keV       
     , while simultaneous radio (VLA) observations have supported the real       
     ity of the tail. The high-energy tail cannot be interpreted as non-th       
     ermal emission because of the energy requirements and as an alternati       
     ve it was explained in terms of a differential emission measure distr       
     ibution of thermal plasma. This implies considerable amounts of plasm       
     a at temperatures >50 MK. Independent confirmation of very hot corona       
     l gas is of paramount importance, given the implications for coronal        
     modelling. We propose to observe II Peg to search for a hot coronal c       
     omponent.                                                                   
                                                                                 
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