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.