CO nova ejecta composition from model calculations

We consider the detailed composition of the ejecta for a large sample of evolutionary sequences of nova outbursts through several cycles, assuming different (systematic) combinations of parameters accreting white dwarf (WD)'s mass, its core temperature and the mass transfer rate. We also investigate the effect of the WD composition different C/O ratios and Ne trace abundance - on nova characteristics. The stellar evolution code used includes an extended nuclear reactions network, OPAL opacities, and diffusion of all elements. Our main conclusions are that CO progenitors reproduce most of the observed abundances and abundance ratios, and that correlations between them, if any, are in very good agreement with observations. The WD composition is generally not reflected in the abundances of the ejecta. The (higher than solar) Ne abundances typical of many CO novae can be explained by a Ne concentration of a few percent in the WD composition, which is predicted by WD evolutionary calculations.