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   PR # 22063
    Many of the observed properties of low mass X-ray binaries are       
    determined by the corona formed by X-ray heating of the accretion    
    disk.  A test of current models for such coronae comes from studies  
    of the broadening of the iron K line and of the strength and spectrum
    of the emission lines from nitrogen, oxygen and iron in the 0.5 - 2  
    KeV energy band.  Using ASCA we can measure the shape and energy of  
    the iron K line, and test models for broadening by line blending,    
    rotation, relativistic effects, and Compton scattering.  We can also 
    measure the low energy line emission and compare with models for line
    emission in order to test for departures from solar abundances.      
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