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We examine the properties of white dwarfs (WDs) accreting hydrogen-richmatter in and near the stable burning regime of accretion rates as modeled bytime-dependent calculations done with Modules for Experiments in StellarAstrophysics (MESA). We report the stability boundary for WDs of masses between0.51 solar masses and 1.34 solar masses as found via time-dependentcalculations. We also examine recurrent novae that are accreting at rates closeto, but below, the stable burning limit and report their recurrence times andignition masses. Our dense grid in accretion rates finds the expected minimumpossible recurrence times as a function of the WD mass. This enables inferencesto be made about the minimum WD mass possible to reach a specific recurrencetime. We compare our computational models of post-outburst novae to the stablyburning WDs and explicitly calculate the duration and effective temperature(Teff) of the post-novae WD in the supersoft phase. We agree with the measuredturnoff time - Teff relation in M31 by Henze and collaborators, infer WD massesin the 1.0-1.3 solar masses range, and predict ejection masses consistent withthose observed. We close by commenting on the importance of the hot heliumlayer generated by stable or unstable hydrogen burning for the short- andlong-term evolution of accreting white dwarfs.

Hydrogen Burning on Accreting White Dwarfs: Stability, Recurrent Novae, and the Post-Novae Supersoft Source