  (abridged) The Extreme Ultraviolet Explorer (EUVE) satellite was employed in
1999 February to acquire phase-resolved EUV photometric and spectroscopic
observations of the AM Her-type cataclysmic variable V834 Centauri. Although we
do not understand the EUV light curves in detail, they are explained
qualitatively by a simple model of accretion from a ballistic stream along the
field lines of a tilted magnetic dipole centered on the white dwarf. The 75-140
Angstrom EUVE spectra are well described by either a blackbody or a pure-H
stellar atmosphere absorbed by a neutral hydrogen column density, but
constraints on the size of the EUV emission region and its UV brightness favor
the blackbody interpretation with temperature kT ~ 17.6 eV, hydrogen column
density N_H ~ 7.4x10^{19} cm^{-2}, fractional emitting area f ~ 10^{-3}, and
luminosity L_soft ~ 7.2x10^{32} (d/100 pc)^2 erg s^{-1}. The ratio of the EUV
to X-ray luminosities is L_soft/L_hard ~ 40, signaling that some mechanism
other than irradiation (e.g., blob heating) dominates energy input into the
accretion spot.
