Sequences of spectra of the nova-like cataclysmic variable ( CV ) BZ Cam were acquired on 9 nights in 2005-2006 in order to study the time development of episodes of wind activity known to occur frequently in this star .
We confirm the results of Ringwald & Naylor ( 1998 ) that the P-Cygni absorption components of the lines mostly evolve from higher expansion velocity to lower velocity as an episode progresses .
We also commonly find blueshifted emission components in the H \alpha line profile , whose velocities and durations strongly suggest that they are also due to the the wind .
Curiously , Ringwald & Naylor reported common occurences of redshifted H \alpha emission components in their BZ Cam spectra .
We have attributed these emission components in H \alpha to occasions when gas concentrations in the bipolar wind ( both frontside and backside ) become manifested as emission lines as they move beyond the disk ’ s outer edge .
We also suggest , based on changes in the P-Cygni profiles during an episode , that the progression from larger to smaller expansion velocities is due the higher velocity portions of a wind concentration moving beyond the edge of the continuum light of the disk first , leaving a net redward shift of the remaining absorption profile .

We derive a new orbital ephemeris for BZ Cam , using the radial velocity of the core of the HeI 5876Å line , finding P = 0.15353 ( 4 ) .
Using this period the wind episodes in BZ Cam are found to be concentrated near inferior conjuction of the emission line source .
This result helps confirm that the winds in nova-like CVs are often phase dependent , in spite of the puzzling implication that such winds lack axisymmetry .

We argue that the radiation-driven wind in BZ Cam receives an initial boost by acting on gas that has been lifted above the disk by the interaction of the accretion stream with the disk , thereby imposing flickering time scales onto the wind events , as well as leading to an orbital modulation of the wind due to the non-axisymmetric nature of the stream/disk interaction .
Simultaneous photometry and spectroscopy were acquired on 3 nights in order to test the possible connection between flickering continuum light and the strength of the frontside wind .
We found strong agreement on one night , some agreement on another , and no agreement on the third .
We suggest that some flickering events lead to only backside winds which will not have associated P Cygni profiles .