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We report on studies of Classical Nova (CN) explosions where we follow theevolution of thermonuclear runaways (TNRs) on oxygen-neon (ONe) white dwarfs(WDs). Using NOVA, a one-dimensional hydrodynamic computer code, we accreteSolar 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 inWDs which find that sufficient mixing with WD core material occurs after theTNR is well underway, and levels of enrichment of the CNONeMg elements arereached that agree with observations of CN ejecta abundances. Because theamount of accreted material is inversely proportional to the oxygen abundance,by first accreting Solar matter, the amount of accreted material is larger thanin those simulations with an initially enriched composition. We vary the massof the WD (from 0.6 Msun to 1.35 Msun) and the composition of the mixedmaterials. Our results show large enrichments of 7Be in the ejected gasesimplying that ONe CNe and CO CNe (Starrfield et al. 2020) may be responsiblefor a significant fraction (about 100 Msun) of the galactic 7Li ( about 1000Msun). The production of 22Na and 26Al in CN explosions and the gamma-rayemission predicted by our simulations is discussed. The WDs in all oursimulations eject less material than they accrete and we predict that the WD isgrowing in mass as a consequence of the CN outburst. ONe CNe, therefore, may bean important channel for accretion induced collapse (AIC) events.

Hydrodynamic Simulations of Oxygen-Neon Classical Novae as Galactic $^7$Li Producers and Potential Accretion Induced Collapse Progenitors