Nucleosynthesis in classical novae: Recent results from TNR theory

Thermonuclear runaways on accreting white dwarfs are modelled by means of an implicit 1D hydrodynamical code, able to follow both the accretion and the explosion stages. Properties at the end of the accretion stage and main features of the explosions have been obtained for different initial conditions. A special emphasis has been put on the influence of the mass and the initial composition of the envelope. Properties of carbon-oxygen (CO) and oxygen-neon (ONe) novae have been compared: accreted and ejected masses, mean velocities of the ejecta, peak temperatures, and so on. But the main results we will present concern the nucleosynthesis, with a detailed analysis of the yields of CO versus ONe novae. The influence of the exact composition of the core (assumed to be mixed with the envelope) will be analyzed. We will also discuss in some detail the synthesis of some important elements for gamma-ray astronomy, such as Be-7, Na-22 and Al-26, and give some insights of the implications of our results for the chemical evolution of the Galaxy.