  Novae are cataclysmic variables driven by accretion of H-rich material onto a
white-dwarf (WD) star from its low-mass main-sequence binary companion. New
time-domain observational capabilities, such as the Palomar Transient Factory
and Pan-STARRS, have revealed a diversity of their behaviour that should be
theoretically addressed. Nova outbursts depend sensitively on nuclear physics
data, and more readily available nova simulations are needed in order to
effectively prioritize experimental effort in nuclear astrophysics. In this
paper we use the MESA stellar evolution code to construct multicycle nova
evolution sequences with CO WD cores. We explore a range of WD masses and
accretion rates as well as the effect of different cooling times before the
onset of accretion. In addition, we study the dependence on the elemental
abundance distribution of accreted material and convective boundary mixing at
the core-envelope interface. Models with such convective boundary mixing
display an enrichment of the accreted envelope with C and O from the underlying
white dwarf that is commensurate with observations. We compare our results with
the previous work and investigate a new scenario for novae with the
3He-triggered convection.
