In-depth analysis of evolving binary systems that produce nova eruptions

Abstract

\n This study is the direct continuation of a previous work performed by Hillman et\xa0al., where they used their feedback dominated numerical simulations to model the evolution of four initial models with white dwarf (WD) masses of 0.7 and $1.0\\, \\mathrm{M}_\\odot$ and red dwarf (RD) masses of 0.45 and $0.7\\, \\mathrm{M}_\\odot$ from first Roche lobe contact of the donor RD, over a few times 109 yr, until the RD was eroded down to below $0.1\\, \\mathrm{M}_\\odot$. This study presents an in-depth analysis of their four models complimented by three models with a higher WD mass of $1.25\\, \\mathrm{M}_\\odot$, one of which comprises an oxygen-neon (ONe) core. Common features were found for all seven models on a secular time-scale as well as on a cyclic time-scale. On the other hand, certain features were found that are strongly dependent either on the WD or the RD mass but are indifferent to the other of the two. Additionally, a model with a WD composed of an ONe core was compared with its corresponding carbon oxygen (CO) core WD model and found to have a significant impact on the heavy element abundances in the ejecta composition.