Spectral energy distributions of young stellar objects. I. A turbospheric model for DR Tauri.
Abstract
A turbospheric model is developed for the spectral energy distribution of the active T Tauri star DR Tau which incorporates a reddened optically thin hydrogen plasma at 65,000 K. Measurements of the spectral energy distribution covering the range 3200 A to 1.1 micron are shown to agree in detail with the model results. It is proposed that the temperature of 65,000 K is a result of equipartition between the particle kinetic energy density of the plasma and the kinetic energy density of strong turbulence which forms a chromospherelike layer, called a turbosphere. It is suggested that the turbulence is driven by the accretion of cometary clumps at a rate of 5 x 10 to the 7th solar masses/year. Results of the model calculations give the following overall parameters for DR Tau: M = 1 solar mass, R = 3 solar radii, and L = 6 solar luminosities. The turbosphere is characterized by: T = 65,000 K, N_{e} = 5 x 10 to the 12th/sq cm, and an atmospheric thickness layer = 4 x 10 to the 9th cm.
 Publication:

The Astrophysical Journal
 Pub Date:
 April 1983
 DOI:
 10.1086/160859
 Bibcode:
 1983ApJ...267..199U
 Keywords:

 Magnetohydrodynamic Turbulence;
 Spectral Energy Distribution;
 Stellar Atmospheres;
 Stellar Models;
 Stellar Spectrophotometry;
 T Tauri Stars;
 Chromosphere;
 Hydrogen Plasma;
 Kinetic Equations;
 Stellar Luminosity;
 Stellar Mass;
 Stellar Mass Accretion;
 Stellar Temperature;
 Astrophysics