Vrielmann, SStiening, ROffutt, W2024-04-262024-04-262002-01-01https://doi.org/10.1046/j.1365-8711.2002.05544.xhttps://hdl.handle.net/20.500.14394/2782<p>This is the prepublished version harvested from ArXiv. The published version is located at <a href="http://onlinelibrary.wiley.com/doi/10.1046/j.1365-8711.2002.05544.x/abstract;jsessionid=C67651D41E3A9E66B25B848366B8D4CE.d02t01">http://onlinelibrary.wiley.com/doi/10.1046/j.1365-8711.2002.05544.x/abstract;jsessionid=C67651D41E3A9E66B25B848366B8D4CE.d02t01</a></p>We analyse simultaneous UBVR quiescent light curves of the cataclysmic variable V2051 Oph using the Physical Parameter Eclipse Mapping (PPEM) method in order to map the gas temperature and surface density of the disc for the first time. The disc appears optically thick in the central regions, and gradually becomes optically thin towards the disc edge or shows a more and more dominating temperature inversion in the disc chromosphere. The gas temperatures in the disc range from about 13 500 K near the white dwarf to about 6000 K at the disc edge. The intermediate part of the disc has temperatures of 9000 to 6500 K.* accretionaccretion discs; * binaries: eclipsing; * stars: individual: V2051 Oph; * novaecataclysmic variablesAstrophysics and Astronomyarticle