We present 14 nights of medium resolution ( 1-2Å ) spectroscopy of the eclipsing cataclysmic variable UU Aquarii obtained during a high accretion state in 1995 August–October .
UU Aqr appears to be an SW Sextantis star , as noted by \markcite BSH96Baptista , Steiner , & Horne ( 1996 ) , and we discuss its spectroscopic behavior in the context of the SW Sex phenomenon .
Emission line equivalent width curves , Doppler tomography , and line profile simulation provide evidence for the presence of a bright spot at the impact site of the accretion stream with the edge of the disk , and a non-axisymmetric , vertically- and azimuthally-extended absorbing structure in the disk .
The absorption has maximum depth in the emission lines around orbital phase 0.8 , but is present from \phi \approx 0.4 to \phi \approx 0.95 .
An origin is explored for this absorbing structure ( as well as the other spectroscopic behavior of UU Aqr ) in terms of the explosive impact of the accretion stream with the disk .