  Modelling of the polarized cyclotron emission from magnetic cataclysmic
variables (MCVs) has been a powerful technique for determining the structure of
the accretion zones on the white dwarf. Until now, this has been achieved by
constructing emission regions (for example arcs and spots) put in by hand, in
order to recover the polarized emission. These models were all inferred
indirectly from arguments based on polarization and X-ray light curves. Potter,
Hakala & Cropper (1998) presented a technique (Stokes imaging) which
objectively and analytically models the polarized emission to recover the
structure of the cyclotron emission region(s) in MCVs. We demonstrate this
technique with the aid of a test case, then we apply the technique to
polarimetric observations of the AM Her system V347 Pav. As the system
parameters of V347 Pav (for example its inclination) have not been well
determined, we describe an extension to the Stokes imaging technique which also
searches the system parameter space (GOSSIP).
