THE STRUCTURE OF SHOCK-WAVES IN THE CASE OF ACCRETION ONTO LOW-MASS YOUNG STARS

A physical analysis and mathematical formulation of the structure of a n accretion shock wave in the case of young stars are given. Some resu lts are presented, and the dependence of the structure of the shock on various parameters is investigated. In the general case, the relative intensities and profiles of lines in the spectra of T Tauri stars sho uld depend on the velocity and density of the infalling gas, as well a s on the accretion geometry. The calculation results may serve as a ba se for elucidating the nature of the activity of young stars.