  We present new red optical spectra of V592 Cas aimed at exploring the
properties of the outflow of this system in a spectral region where the
underlying white dwarf and the accretion disk do not contribute significantly
to the observed absorption components of the H-alpha and HeI line profiles. We
use the H-alpha emission line to study the wind, which appears as pronounced
blueshifted P-Cygni absorption troughs whose low velocity end contaminates the
blue side of the emission line profile. The wind appears to be episodic in
nature, with multiple events reaching velocities of 5000km/sec in H-alpha.
Similar (but weaker) wind signatures appear in the HeI5876AA line but are
absent in HeI6678AA. Our data suggest that during wind episodes the wind is
phase dependent and is visible for half the orbit of the system. Considering
that V592 Cas is viewed almost face-on, the symmetry axis of the outflow can
not be orthogonal to the disk and/or the outflow must have some other inherent
asymmetry in outflow geometry. A possible origin of the wind is in a disk
hotspot, either at the initial impact point of the accretion stream on the disk
edge or as a result of disk overflow (similar to SW Sextantis stars).
Simultaneous optical photometry during one night of our spectroscopic
observations indicate that there is no clear relationship between the optical
brightness variations and the strength of the outflow in this system.
