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   PR # 21505
    We propose to observe six nearby single dMe stars with the SIS.      
    Previous X-ray spectra for this class of stars were usually fitted   
    with two-temperature Raymond models, suggesting the presence of ther-
    mally-structured coronae. The SIS observations will clarify many     
    details of the emission, for instance if it is really dominated by   
    plasma in discrete temperature intervals,or if it can be described by
    a more realistic model of solar-type coronal structures(loops). While
    a hydrostatic loop model spectrum fits the available low-resolution  
    data equally well, our simulations show that SIS spectra can resolve 
    the model ambiguity. We plan to analyze the SIS data using both a    
    loop-model fitting approach, and a model-independent procedure to    
   reconstruct the source emissio
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