  We report on studies of Classical Nova (CN) explosions where we follow the
evolution of thermonuclear runaways (TNRs) on oxygen-neon (ONe) white dwarfs
(WDs). Using NOVA, a one-dimensional hydrodynamic computer code, we accrete
Solar matter until the TNR is ongoing and then switch to a mixed composition.
This approach is guided by the results of multi-dimensional studies of TNRs in
WDs which find that sufficient mixing with WD core material occurs after the
TNR is well underway, and levels of enrichment of the CNONeMg elements are
reached that agree with observations of CN ejecta abundances. Because the
amount of accreted material is inversely proportional to the oxygen abundance,
by first accreting Solar matter, the amount of accreted material is larger than
in those simulations with an initially enriched composition. We vary the mass
of the WD (from 0.6 Msun to 1.35 Msun) and the composition of the mixed
materials. Our results show large enrichments of 7Be in the ejected gases
implying that ONe CNe and CO CNe (Starrfield et al. 2020) may be responsible
for a significant fraction (about 100 Msun) of the galactic 7Li ( about 1000
Msun). The production of 22Na and 26Al in CN explosions and the gamma-ray
emission predicted by our simulations is discussed. The WDs in all our
simulations eject less material than they accrete and we predict that the WD is
growing in mass as a consequence of the CN outburst. ONe CNe, therefore, may be
an important channel for accretion induced collapse (AIC) events.
