  The tomographic method "Physical Parameter Eclipse Mapping" is a tool to
reconstruct spatial distributions of physical parameters (like temperatures and
surface densities) in accretion discs of cataclysmic variables. After
summarizing the method, we apply it to multi-colour eclipse light curves of
various dwarf novae and nova-likes like VZ Scl, IP Peg in outburst, UU Aqr,
V2051 Oph and HT Cas in order to derive the temperatures (and surface
densities) in the disc, the white dwarf temperature, the disc size, the
effective temperatures and the viscosities. The results allows us to establish
or refine a physical model for the accretion disc. Our maps of HT Cas and V2051
Oph, for example, indicate that the (quiescent) disc must be structured into a
cool, optically thick inner disc sandwiched by hot, optically thin
chromospheres. In addition, the disc of HT Cas must be patchy with a covering
factor of about 40% caused by magnetic activity in the disc.
