Abstract
The evolution of protoplanetary disks around young stars is briefly reviewed. The most important physical mechanisms that drive the mass accretion are gravitational, magnetic, and thermal convective instabilities. These mechanisms are dominant in different regions of the disk and at different evolutionary epochs.
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Ruden, S.P. Theory of protoplanetary disks. Astrophys Space Sci 223, 57–68 (1995). https://doi.org/10.1007/BF00989154
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DOI: https://doi.org/10.1007/BF00989154