  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 $\gamma$-ray emission. The resulting elemental yields reproduce fairly
well the spectroscopic abundance determinations of several well studied
classical novae.
