  Classical novae are the results of surface thermonuclear explosions of H-rich
material accreted by white dwarfs (WDs) from their low-mass main-sequence or
red-giant binary companions. Chemical composition analysis of their ejecta
shows that nova outbursts occur on both carbon-oxygen (CO) and oxygen-neon
(ONe) WDs, and that there is cross-boundary mixing between the accreted
envelope and underlying WD. We have combined the stellar evolution code MESA
and post-processing nucleosynthesis tools of NuGrid into a framework that
allows to produce up-to-date models of nova outbursts and compute detailed
nucleosynthesis in novae occurring on CO and ONe WDs. The convective boundary
mixing (CBM) in our 1D numerical simulations is implemented using a diffusion
coefficient that is exponentially decreasing with a distance below the bottom
of the convective envelope. This MESA CBM prescription is based on the findings
in 3D hydrodynamic simulations that the velocity field, and along with it the
mixing expressed in terms of a diffusion coefficient, decays exponentially in
the stable layer adjacent to a convective boundary. The framework can also use
the commonly adopted 1D nova model in which the CBM is mimicked by assuming
that the accreted envelope has been pre-enriched with WD's material. In this
preliminary report, we present the most interesting new results related to CO
and ONe nova outbursts that have been obtained with the Nova Framework.
