Structure of the protoplanetary accretion disk around the Sun at T Tauri phase. I. Initial data, equations, and methods of modeling.

Details Structure of the protoplanetary accretion disk around the Sun at T Tauri phase. I. Initial data, equations, and methods of modeling. Structure of the protoplanetary accretion disk around the Sun at T Tauri phase. I. Initial data, equations, and methods of modeling.

Apr 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995sosyr..29...85m&link_type=abstract

Solar System Research, Vol. 29, No. 2, p. 85 - 104

Computer Science

Accretion Disks: Protoplanetary Disks, Accretion Disks: T Tauri Stars, Accretion Disks: Structure

Scientific paper

The formulation of the problem and initial data in the modeling of the protoplanetary disk around the young Sun at the T Tauri phase are considered. A brief review of new observations of T Tauri stars with disks which indicate the process of accretion from the disk onto the star. Estimates of the disk and young star parameters are presented and theoretical results concerning the accretion disk viscosity are used. Restrictions that information on T Tauri stars with disks imposes on initial parameters for the protoplanetary disk modeling, namely, accretion mass flux M˙ from the disk onto the Sun, luminosity, and radius of the young Sun, are discussed. Values of these parameters are chosen, taking into account the constraints, in order to determine the disk characteristics at the sequential stages of its evolution. Equations for the temperature of the radiating disk surface, as well as equations relating this temperature to the interior disk temperature are derived. Both the internal energy source (dissipation of turbulence) and external source (absorption of the solar radiation) were taken into account. Approximate equations for the radial distribution of the most important disk parameters as functions of mass flux M˙ and disk opacity are obtained. Methods of calculation of vertical structure of the disk for radial distances from 0.1 to 10 a.u. are presented. This technique allows one to determine the boundaries of condensation zones of the most important components of the protoplanetary material: magnesian silicates, iron, and water. The role of temperature and opacity negative feedback in the formation of two-phase gas-solid regions for the silicates and iron in the inner part of the disk and for water in its outer region is shown.

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