Nucleosynthesis in Classical Novae: ONe vs. CO White Dwarfs

Abstract

Detailed nucleosynthesis in the ejecta of classical novae has been determined for a grid of hydrodynamic nova models. The reported 14 evolutionary sequences, followed from the onset of accretion up to the explosion and ejection stages, span a range of CO and ONe white dwarf masses (0.8-1.35 $M_o$) and mixing levels between the accreted envelope and the underlying white dwarf core (25-75%). The synthesis of each isotope, from ${}^1$H to ${}^{40}$Ca, is discussed along with its sensitivity to model parameters. Special emphasis is given to isotopes such as ${}^{13}$C, ${}^{15}$N, and ${}^{17}$O, which may account for a significant fraction of their Galactic content. Production of the radioactive isotopes ${}^7$Be, ${}^{22}$Na, and ${}^{26}$Al is also analyzed, since they may provide a direct test of the thermonuclear runaway model through their $γ$-ray emission. The resulting elemental yields reproduce fairly well the spectroscopic abundance determinations of several well studied classical novae.