  We present spectroscopy and orbital periods Porb for 30 apparently
non-magnetic cataclysmic binaries with periods below about 3 hours, nearly all
of which are dwarf novae, mostly of the SU Ursae Majoris subclass. We then turn
to the evidence supporting the prediction that short-period dwarf novae evolve
toward longer periods after passing through a minimum period -- the "period
bounce" phenomenon. Plotting data from the literature reveals that for
superhump period excess $\epsilon = (P_{\rm sh} - P_{\rm orb} )/P_{\rm orb}$
below about 0.015, the period appears to increase with decreasing epsilon,
agreeing at least qualitatively with the predicted behavior. Next, motivated by
the long (decadal) outburst intervals of the WZ Sagittae subclass of
short-period dwarf novae, we ask whether there could be a sizable population of
"lurkers" -- systems that resemble dwarf novae at minimum light, but do not
outburst over accessible timescales (or at all), and therefore do not draw
attention to themselves. By examining the outburst history of the Sloan Digital
Sky Survey sample of CVs, which were selected by color and not by outburst, we
find that a large majority of the color-selected dwarf-nova-like objects have
been observed to outburst, and conclude that "lurkers", if they exist, are a
relatively minor part of the CV population.
