Astronomy and Astrophysics – Astronomy
Scientific paper
Mar 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...423..736r&link_type=abstract
Astrophysical Journal v.423, p.736
Astronomy and Astrophysics
Astronomy
36
Accretion, Accretion Disks, Hydrodynamics, Radiative Transfer, Stars: Formation
Scientific paper
Two-dimensional axisymmetric solutions of the equations of hydrodynamics, including radiation transport and local energy generation due to viscosity, are presented for the case of non-self-gravitating protoplanetary disks around young solar-type stars. The parameters that are varied include the accretion rate in the disk, the magnitude of the viscosity parameter α, the boundary conditions, and the initial conditions. In general, for α > 0.05 and for distances >0.5 AU, the flow pattern is found to consist of a radial outflow near the equatorial plane and a radial inflow near the disk surface. Unlike one-dimensional vertical structure models in this regime, the flow is stable to convection, implying a physically inconsistent model in which the convective turbulence required to generate the viscosity is actually not present. Reduction of α to order 10-3 is necessary to regain consistency. However, in the warmer regions interior to 0.5 AU, where the opacity rises steeply as a consequence of hydrogen ionization, a physically consistent turbulent flow is found even for α = 0.05. Model results are compared with one-dimensional vertical structure calculations.
Bell Katherine Robbins
Bodenheimer Peter
Rozyczka Michal
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