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=1995avest..29...99m&link_type=abstract

Astronomicheskii Vestnik, Tom 29, No. 2, p. 99 - 122

Astronomy and Astrophysics

Astronomy

8

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

Scientific paper

Formulation of the problem and initial data in the modeling of the protoplanetary disk around the young Sun at T-Tauri phase are considered. Brief review of new observations of T-Tauri stars with disks, which indicate the process of accretion from the disk onto the star as well as estimates of the disk and star parameters are presented. Theoretical results about the accretion disk viscosity are used. Restrictions imposed by T-Tauri star observations on initial parameters for the protoplanetary disk modeling such as accretion mass flux M˙ in the disk, luminosity and radius of the young Sun are discussed. Approximate equations for the radial distribution of the most important disk parameters and function of mass flux M˙ and disk opacity were obtained. Methods of the calculations of the disk vertical structure for the radial distances from 0.1 to 10 a.u. are presented. This technique allows to determine the boundaries of condensation zones of the most important compounds of the protoplanetary nebula - magnesium silicates, iron, and water in the outer part of the disk.

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