Modeling of the Turbulent Transport Coefficients in a Gas-Dust Accretion Disk

Details Modeling of the Turbulent Transport Coefficients in a Gas-Dust Accretion Disk Modeling of the Turbulent Transport Coefficients in a Gas-Dust Accretion Disk

Nov 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000sosyr..34..469k&link_type=abstract

Solar System Research, v. 34, Issue 6, p. 469-480 (2000).

Physics

Scientific paper

An heuristic way of modeling the turbulent exchange coefficients for Keplerian accretion disks surrounding solar-type stars is considered. The formulas for these coefficients, taking into account the inverse effects of dust transfer and potential temperature on the maintenance of shear turbulence, generalize to protoplanetary gas-dust clouds the expression for the turbulent viscosity coefficient in so-called α-disks which was obtained in a classic work by Shakura and Syunyaev (1973). The defining relationships are derived for turbulent diffusion and heat flows, which describe, for the two-phase mixture rotating differentially at an angular velocity Ω(r, z), the dust and heat transfer in the direction perpendicular to the central plane of the disk. The regime of limiting saturation by small dust particles of the layer of ``cosmic fluid'' located slightly above (or below) the dust subdisk is analyzed.

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