Classical novae are the result of thermonuclear flashes of H accreted by CO or ONe white dwarfs , leading eventually to the dynamic ejection of the surface layers .
These are observationally known to be enriched in heavy elements , such as C , O and Ne that must originate in layers below the H-flash convection zone .
Building on our previous work we now present stellar evolution simulations of ONe nova , and provide a comprehensive comparison of our models with previous work .
Some of our models include exponential convective boundary mixing model to account for the observed enrichment of the ejecta even when accreting material with a solar abundance distribution .
Our models produce maximum temperature evolution profiles and nucleosynthesis yields in good agreement with models that generate enriched ejecta by assuming that the accreted material was pre-enriched .
We confirm for ONe nova the result we reported previously , i.e .
we found that ^ { 3 } He can be produced in situ in solar-composition envelopes accreted with slow rates ( \dot { M } < 10 ^ { -10 } M _ { \odot } / \mbox { yr } ) by cold ( T _ { WD } < 10 ^ { 7 } K ) CO WDs , and that convection is triggered by ^ { 3 } He burning before the nova outburst in this case .
In addition , we now find that the interplay between the ^ { 3 } He production and destruction in the solar-composition envelope accreted with an intermediate rate , e.g . \dot { M } = 10 ^ { -10 } M _ { \odot } / \mbox { yr } , by the 1.15 M _ { \odot } ONe WD with a relatively high initial central temperature , e.g . T _ { WD } = 15 \times 10 ^ { 6 } K , leads to the formation of a thick radiative buffer zone that separates the bottom of the convective envelope from the WD surface .
We present detailed nucleosynthesis calculations based on the post-processing technique , and demonstrate in which way much simpler single-zone trajectories extracted from the multi-zone stellar evolution simulations can be used , in lieu of full multi-zone simulations , to analyse the sensitivity of nova abundance predictions on nuclear reaction rate uncertainties .
Trajectories for both CO and ONe for different central T and accretion rates are provided .
We compare our nova simulations with observations of nova and pre-solar grain believed to originate in nova .