  We present the results from a multi-wavelength study of the mixed H+He
composition DAO white dwarf RE J0720-318. A detailed analysis of UV and EUV
spectroscopic data with state-of-the-art non-LTE photospheric models
demonstrates that the observed opacity to EUV radiation probably results from a
more complex structure than a simple H+He, chemically layered atmosphere.
Instead, EUV photometry and phase resolved EUV spectroscopy indicate a likely
spatial non-uniformity in the surface distribution of helium, which is
consistent with a model in which material is accreted from the wind of the dM
secondary. The rotational modulation of the spatially inhomogeneous EUV opacity
allows us to estimate the rotation period of the white dwarf (0.463 +/- 0.004
days). We have also reviewed two plausible origins proposed by Burleigh et al.
(1997) and Dupuis et al. (1997) to account for the unusual N(HI)/N(HeI)~1 along
this line of sight. We conclude that it is probably due to the presence of a
cloud of ionized gas along this line of sight, rather than a circumbinary disk.
The cloud, residing between 123-170pc distant in the direction of the CMa ISM
tunnel, may be >40pc in length.
