- The models have use the calculations of Meggitt and Wickramasinghe
1985. These assume characteristic electron temperatures,,
electron number density, and propagation path, s, and are
characterised by the optical depth parameter Meggitt and
Wickramasinghe (1982).
- The models assume a value for the system inclination and for the
offset of the magnetic dipole field from the spin axis of the white
dwarf.
- The viewing angle to the magnetic field line of each emission point is
calculated as a function of spin phase of the white dwarf together with
the local field strength and optical depth.
- Emission from extended regions are then modelled by calculating the
Stokes parameters for each point and summing to obtain the polarized
light curves. The complete radiative transfer is not carried out.
- Projection effects are taken into consideration because most of the
emission is not optically thin.
- We have used lambda=10^6,10 keV models with a field
of 60 MG at the magnetic poles in the test cases.
Stephen Potter
Thu Jul 31 14:44:15 BST 1997