The Composition of Nova Ejecta from Multicycle Evolution Models

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Abstract

Following a previous systematic study involving calculations of evolutionary sequences of nova outbursts through several cycles, for combinations of parameters—the accreting white dwarf (WD's) mass, its core temperature, and the mass transfer rate—spanning the entire parameter space, assuming CO WDs (with C and O in equal mass fractions), we now consider the detailed composition of the ejecta for the subset of models which simulated classical nova outburst. We also investigate the effect of the additional input parameter—the WD composition—on nova characteristics by calculating evolutionary sequences with pure-carbon and pure-oxygen WD progenitors. The stellar evolution code used includes an extended nuclear reactions network, OPAL opacities, and diffusion of all elements.

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