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We report on studies of Classical Nova (CN) explosions where we follow theevolution of thermonuclear runaways (TNRs) on Carbon Oxygen (CO) white dwarfs(WDs). We vary both the mass of the WD (from 0.6 M$_\odot$ to 1.35 M$_\odot$)and the composition of the accreted material. Our simulations are guided by theresults of multi-dimensional studies of TNRs in WDs that find sufficient mixingwith WD core material occurs after the TNR is well underway, reaching levels ofenrichment that agree with observations of CN ejecta abundances. We use NOVA(our 1-dimensional hydrodynamic code) to accrete solar matter until the TNR isongoing and then switch to a mixed composition (either 25% WD material and 75%solar or 50% WD material and 50% solar). Because the amount of accretedmaterial is inversely proportional to the initial $^{12}$C abundance, by firstaccreting solar matter the amount of material taking part in the outburst islarger than in those simulations where we assume a mixed composition from thebeginning. Our results show large enrichments of $^7$Be in the ejected gasesimplying that CO CNe may be responsible for a significant fraction ($\sim$ 100M$_\odot$) of the $^7$Li in the galaxy ($\sim$1000 M$_\odot$). In addition,although the ejected gases are enriched in WD material, the WDs in thesesimulations eject less material than they accrete. We predict that the WD isgrowing in mass as a consequence of the accretion-outburst-accretion cycle andCO CNe may be an important channel of Supernova Ia progenitors.

Carbon-Oxygen Classical Novae are Galactic $^7$Li Producers as well as Potential Supernova Ia Progenitors