• Lithium Production
• Novae
• Nucleosynthesis
• Stochastic Processes
• Turbulent Mixing

Classical Nova explosions occur on white dwarf stars in a close binary system that accrete gas from the "normal" companion over long periods of time (10^5 yr). The accreting material is compressed and heated due to the white dwarf's high surface gravity, triggering a thermonuclear runaway in a degenerate environment and leading to mass ejection. Several 3D models have shown that a few minutes before the outburst, the white dwarf envelope enters in a not fully-developed turbulent regime, which introduces a range of length scales for energy transport and element mixing. In this thesis, the dynamical data from fully-3D simulations are coupled to 1D modeling of the explosion, and the effects of turbulent mixing on light element nucleosynthesis are studied with a novel stochastic approach based on the Gillespie algorithm. This treatment of turbulent mixing avoids introducing unphysical parametric modifications that have so far been used to model this stage of the outburst. This approach can be directly implemented into 1D nova models in order to better treat the nucleosynthesis and the final lithium yield.