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Classical novae are the results of surface thermonuclear explosions ofhydrogen accreted by white dwarfs (WDs) from their low-mass main-sequence orred-giant binary companions. Chemical composition analysis of their ejectashows that nova outbursts occur on both carbon-oxygen (CO) and more massiveoxygen-neon (ONe) WDs, and that there is cross-boundary mixing between theaccreted envelope and underlying WD. We demonstrate that the state-of-the-artstellar evolution code MESA and post-processing nucleosynthesis tools of NuGridcan successfully be used for modeling of CO and ONe nova outbursts andnucleosynthesis. The convective boundary mixing (CBM) in our 1D numericalsimulations is implemented using a diffusion coefficient that is exponentiallydecreasing with a distance below the bottom of the convective envelope. We showthat this prescription produces maximum temperature evolution profiles andnucleosynthesis yields in good agreement with those obtained using the commonlyadopted 1D nova model in which the CBM is mimicked by assuming that theaccreted envelope has been pre-mixed with WD's material. In a previous paper,we have found that 3He can be produced in situ in solar-composition envelopesaccreted with slow rates (dM/dt < 1e-10 M_sun/yr) by cold (T_WD < 1d7 K) COWDs, and that convection is triggered by 3He burning before the nova outburstin this case. Here, we confirm this result for ONe novae. Additionally, we findthat the interplay between the 3He production and destruction in thesolar-composition envelope accreted with an intermediate rate, e.g. dM/dt =1e-10 M_sun/yr, by the 1.15 M_sun ONe WD with a relatively high initial centraltemperature, e.g. T_WD = 15e6 K, leads to the formation of a thick radiativebuffer zone that separates the bottom of the convective envelope from the WDsurface.

MESA and NuGrid Simulations of Classical Nova Outbursts and Nucleosynthesis