Recurrent novae and long-term evolution of mass-accreting white dwarfs -- toward the accurate mass retention efficiency

TL;DR

This paper reviews the factors affecting the long-term mass growth of accreting white dwarfs, emphasizing the importance of accurate modeling of mass-loss mechanisms, especially optically thick winds, for understanding Type Ia supernova progenitors.

Contribution

It identifies key reasons for discrepancies in white dwarf mass growth rates and highlights the necessity of proper numerical techniques and assumptions, particularly regarding mass-loss processes.

Findings

Incorrect assumptions lead to divergent WD growth rate estimates.

Proper inclusion of optically thick winds is crucial for accurate mass retention calculations.

Long-term evolution models depend heavily on initial conditions and binary configurations.

Abstract

The mass growth rate of mass-accreting white dwarfs (WDs) is a key factor in binary evolution scenarios toward Type Ia supernovae. Many authors have reported very different WD mass increasing rates. In this review, we clarify the reasons for such divergence, some of which come from a lack of numerical techniques, usage of old opacities, different assumptions for binary configurations, inadequate initial conditions, and unrealistic mass-loss mechanisms. We emphasize that these assumptions should be carefully chosen in calculating the long-term evolution of accreting WDs. Importantly, the mass-loss mechanism is the key process determining the mass retention efficiency: the best approach involves correctly incorporating the optically thick wind because it is supported by the multiwavelength light curves of novae.