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Cataclysmic Variables (CVs) and Symbiotic Binaries are close (or not soclose) binary star systems which contain both a white dwarf (WD) primary and alarger cooler secondary star that typically fills its Roche Lobe. The coolerstar is losing mass through the inner Lagrangian point of the binary and afraction of this material is accreted by the WD. Here we report on ourhydrodynamic studies of the thermonuclear runaway (TNR) in the accretedmaterial that ends in a Classical Nova explosion. We have followed theevolution of the TNRs on both carbon-oxygen (CO) and oxygen-neon (ONe) WDs. Wereport on 3 studies in this paper. First, simulations in which we accrete onlysolar matter using NOVA (our 1-D, fully implicit, hydro code). Second, we useMESA for similar studies in which we accrete only Solar matter and compare theresults. Third, we accrete solar matter until the TNR is ongoing and thenswitch the composition in the accreted layers to a mixed composition: either25% WD and 75% solar or 50% WD and 50% Solar matter. We find that the amount ofaccreted material is inversely proportional to the initial 12C abundance (asexpected). Thus, accreting solar matter results in a larger amount of accretedmaterial to fuel the outburst; much larger than in earlier studies where amixed composition was assumed from the beginning of the simulation. Our mostimportant result is that all these simulations eject significantly less massthan accreted and, therefore, the WD is growing in mass toward theChandrasekhar Limit.

Hydrodynamic Simulations of Classical Novae; CO and ONe White Dwarfs are Supernova Ia Progenitors