  We measure the duty cycles for an existing sample of well observed, nearby
dwarf novae using data from AAVSO, and present a quantitative empirical
relation between the duty cycle of dwarf novae outbursts and the X-ray
luminosity of the system in quiescence. We have found that $\log
DC=0.63(\pm0.21)\times(\log L_{X}({\rm erg\,s^{-1}})-31.3)-0.95(\pm0.1)$, where
DC stands for duty cycle. We note that there is intrinsic scatter in this
relation greater than what is expected from purely statistical errors. Using
the dwarf nova X-ray luminosity functions from \citet{Pretorius12} and
\citet{Byckling10}, we compare this relation to the number of dwarf novae in
the Galactic Bulge Survey which were identified through optical outbursts
during an 8-day long monitoring campaign. We find a specific frequency of X-ray
bright ($L_{X}>10^{31}\,{\rm erg\,s^{-1}}$) Cataclysmic Variables undergoing
Dwarf Novae outbursts in the direction of the Galactic Bulge of
$6.6\pm4.7\times10^{-5}\,M_{\odot}^{-1}$. Such a specific frequency would give
a Solar neighborhood space density of long period CVs of
$\rho=5.6\pm3.9\times10^{-6}\,$pc$^{-3}$. We advocate the use of specific
frequency in future work, given that projects like LSST will detect DNe well
outside the distance range over which $\rho\approx{\textrm const}$.
