Evolution of Disk Accretion

Abstract

We review the present knowledge of disk accretion in young low mass stars, and in particular, the mass accretion rate and its evolution with time. The methods used to obtain mass accretion rates from ultraviolet excesses and emission lines are described, and the current best estimates of mass accretion rate for Classical T Tauri stars and for objects still surrounded by infalling envelopes are given. We argue that the low mass accretion rates of the latter objects require episodes of high mass accretion rate to build the bulk of the star. Similarity solutions for viscous disk evolution suggest that the inner disk mass accretion rates can be self-consistently understood in terms of the disk mass and size if the viscosity parameter alpha is approximately 1e-2. Close companion stars may accelerate the disk accretion process, resulting in accretion onto the central star in less or equal than 1Myr; this may help explain the number of very young stars which are not currently surrounded by accretion disks (the weak emission T Tauri stars).