Abstract
Department of Astronomy and AstrophysicsUniversity of ChicagoChicago, IL, USAE-mail:pavelden@uvic.ca, fherwig@uvic.ca, mpignatari@gmail.com,truran@nova.uchicago.eduClassical novae are the results of surface thermonuclear explosions of H-rich material accretedby 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 betweenthe accreted envelope and underlying WD. We have combined the stellar evolution code MESAand post-processing nucleosynthesis tools of NuGrid into aframework that allows to produceup-to-date models of nova outbursts and compute detailed nucleosynthesis in novae occurring onCO and ONe WDs. The convective boundary mixing (CBM) in our 1D numerical simulations isimplemented using a diffusion coefficient that is exponenti ally decreasing with a distance belowthe bottom of the convective envelope. This MESA CBM prescription is based on the findings in3D hydrodynamic simulations that the velocity field, and alo ng with it the mixing expressed interms of a diffusion coefficient, decays exponentially in th e stable layer adjacent to a convectiveboundary. The framework can also use the commonly adopted 1D nova model in which the CBMis 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 ONenova outbursts that have been obtained with the Nova Framework.XII International Symposium on Nuclei in the Cosmos 2012Cairns, Australia5th - 10th August 2012
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