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

Abstract

ABSTRACT This study is the direct continuation of a previous work performed by Hillman et al., 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.