The three-dimensional structure of extreme-ultraviolet accretion regions in AM Herculis stars: Modeling of extreme-ultraviolet photometric and spectroscopic observations

We have developed a model of the high-energy accretion region for magnetic cataclysmic variables and applied it to Extreme Ultraviolet Explorer observ ations of 10 AM Herculis type systems. The major features of the EUV light curves are well described by the model. The light curves exhibit a large va riety of features such as eclipses of the accretion region by the secondary star and the accretion stream and broad dips caused by material very close to the accretion region. While all the observed features of the light curv es are highly dependent on viewing geometry, none of the light curves are c onsistent with a flat, circular accretion spot whose light curve would vary solely from projection effects. The accretion region immediately above the white dwarf (WD) surface is a source of EUV radiation caused by either a v ertical extent to the accretion spot or Compton scattering off of electrons in the accretion column or, very likely, both. Our model yields spot sizes averaging 0.06R(WD), or f similar to 1 x 10(-3) the WD surface area, and a verage spot heights of 0.023R(WD). Spectra extracted during broad-dip phase s are softer than spectra extracted during the out-of-dip phases. This spec tral ratio measurement leads to the conclusion that Compton scattering, som e absorption by a warm absorber, geometric effects, an asymmetric temperatu re structure in the accretion region, and an asymmetric density structure o f the accretion column are all important components needed to fully explain the data. Spectra extracted at phases where the accretion spot is hidden b ehind the limb of the WD, but with the accretion column immediately above t he spot still visible, show no evidence of emission features characteristic of a hot plasma.