Abstract
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 of accretion rates from ˙M=10 -7 to 10 -4 M ○. yr -1 and are in qualitative agreement with observations of T Tauri and FU Orionis stars. The boundary layers in the solutions have two radial zones. The viscous dissipation occurs in a relatively narrow dynamical boundary layer, but most of the energy is actually radiated over a wider thermal boundary layer which extends to larger radii
Sign-in/Register to access full text options 
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a callDisclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.
