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   PR # 22045
    IUE, HST and HUT observations of the white dwarf in the prototype    
    dwarf nova system U Gem have shown a hot (60,000K) component which   
    cools in the 4 month quiescent interval following outburst, resulting
    in declining UV fluxes. Disk instability models to explain dwarf     
    novae outbursts predict the accretion rate should rise during        
    quiescence. We will use the unique range, sensitivity and spectral   
    capabilities of ASCA to directly measure the boundary layer          
    luminosity during 2 spaced quiescent observations of U Gem.  The     
    spectrum will provide valuable insight to the characteristics of the 
    quiescent boundary layer, while changes will test the disk           
    instability model, as well as provide valuable constraints on the    
   effect of ongoing accretion on
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