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Classical novae are thermonuclear explosions that take place in the envelopesof accreting white dwarfs in binary systems. The material piles up underdegenerate conditions, driving a thermonuclear runaway. The energy released bythe suite of nuclear processes operating at the envelope heats the material upto peak temperatures about 100 - 400 MK. During these events, about 10-3 - 10-7Msun, enriched in CNO and, sometimes, other intermediate-mass elements (e.g.,Ne, Na, Mg, Al) are ejected into the interstellar medium. To account for thegross observational properties of classical novae (in particular, the largeconcentrations of metals spectroscopically inferred in the ejecta), modelsrequire mixing between the (solar-like) material transferred from the secondaryand the outermost layers (CO- or ONe-rich) of the underlying white dwarf.Recent multidimensional simulations have demonstrated that Kelvin-Helmholtzinstabilities can naturally produce self-enrichment of the accreted envelopewith material from the underlying white dwarf at levels that agree withobservations. However, the feasibility of this mechanism has been explored inthe framework of CO white dwarfs, while mixing with different substrates stillneeds to be properly addressed. Three-dimensional simulations of mixing at thecore-envelope interface during nova outbursts have been performed with themultidimensional code FLASH, for two types of substrates: CO- and ONe-rich. Weshow that the presence of an ONe-rich substrate, as in "neon novae", yieldslarger metallicity enhancements in the ejecta, compared to CO,rich substrates(i.e., non-neon novae). A number of requirements and constraints for such 3-Dsimulations (e.g., minimum resolution, size of the computational domain) arealso outlined.

Three-dimensional simulations of turbulent convective mixing in ONe and CO classical nova explosions