  Models have long predicted that the frequency-averaged masses of white dwarfs
in Galactic classical novae are twice as large as those of field white dwarfs.
Only a handful of dynamically well-determined nova white dwarf masses have been
published, leaving the theoretical predictions poorly tested. The recurrence
time distributions and mass accretion rate distributions of novae are even more
poorly known. To address these deficiencies, we have combined our extensive
simulations of nova eruptions with the Strope et al (2010) and Schaefer et al
(2010) databases of outburst characteristics of Galactic classical and
recurrent novae to determine the masses of 92 white dwarfs in novae. We find
that the mean mass (frequency averaged mean mass) of 82 Galactic classical
novae is 1.06 (1.13) Msun, while the mean mass of 10 recurrent novae is 1.31
Msun. These masses, and the observed nova outburst amplitude and decline time
distributions allow us to determine the long-term mass accretion rate
distribution of classical novae. Remarkably, that value is just 1.3 x 10^{-10}
Msun/yr, which is an order of magnitude smaller than that of cataclysmic
binaries in the decades before and after classical nova eruptions. This
predicts that old novae become low mass transfer rate systems, and hence dwarf
novae, for most of the time between nova eruptions. We determine the mass
accretion rates of each of the 10 known Galactic RN, finding them to be in the
range 10^{-7} - 10^{-8} $ Msun/yr. We are able to predict the recurrence time
distribution of novae and compare it with the predictions of population
synthesis models.
