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The formation of bimodal dust species (that is, both of silicate andamorphous carbon dust grains are observed in a nova eruption) in nova ejecta isstill debated. Using the Modules for Experiments in Stellar Astrophysics codeand considering the effects of WD's mass, mass-accretion rate and the chemicalprofiles of WD which are described by new parameter --- mixing depth on thechemical abundances of nova ejecta, we investigate the possibility that bimodaldust species are produced in a nova eruption. We find that $C/O$ (the ratio ofcarbon number density to oxygen number density) of nova ejecta is affected bythe mixing depth. For the model with a small mixing depth, the $C/O$ of novaejecta can evolute from lager than 1.0 to smaller than 1.0 in a whole eruption,which provides the chemical condition for the formation of bimodal dustspecies.

The Formation of Bimodal Dust Species in Nova Ejecta I: Chemical Conditions