  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.
