(a) Time evolution of disk accretion rates among three stars of different masses, based on Eq. (6) of Manara et al. (2012). The disk accretion rate drops faster with decreasing mass of the central object. (b) Disk mass vs. (sub)stellar mass at different times, based on Ṁ_g measurements of Manara et al. (2012). The solid lines from thick to thin represent the ages of systems, from 0 to 0.5, 1, and 3 Myr. The green dashed lines correspond to the linear and quadratic relation between the disk mass and the stellar mass. When the disk is ≲1 Myr old, M_d ∝ M_⋆, while when the age is greater than ~ 1−3 Myr.