  We analyse the impact of the initial abundances of the underlying white dwarf
core on the nucleosynthesis accompanying classical nova outbursts, in the
framework of hydrodynamic models of the explosion. Specifically, we take into
account the chemical stratification of the white dwarf. It turns out that the
presence of a thick CO-buffer on top of the ONe-rich core, as results from
detailed calculations of previous evolution of the progenitor star, may lead to
significant amounts of both 7Li and 26Al, after an outburst that, due to the
lack of neon isotopes in the ejecta, would be misclassified as a non-neon nova
(i.e., CO nova).
