Boundary Layers in Pre-Main-Sequence Accretion Disks

摘要: We present self-consistent solutions, using α-viscosity, for the flow and energetics of optically thick boundary layers in accretion disks around pre-main-sequence stars. The solutions span a range rates from ˙M=10 -7 to 10 -4 M ○. yr -1 are qualitative agreement with observations T Tauri FU Orionis have two radial zones. viscous dissipation occurs relatively narrow dynamical layer, but most energy is actually radiated over wider thermal layer which extends larger radii