Nova Framework: A New Tool For Modeling of Nova Outbursts and Nucleosynthesis

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.