Photoevaporation of circumstellar disks around young stars.

摘要: We examine the ability of photoevaporative disk winds to explain low-velocity components observed in forbidden line spectra low-mass T Tauri stars. Using analytic model Shu and coworkers Hollenbach as a basis, we characteristics outflows with hydrodynamic simulations. General results from simulations agree well predictions, although some small differences are present. Most importantly, flow material surface develops at smaller radii than approximations, velocity is only one-third sound speed. A detailed presentation observational consequences given, including predicted widths, blueshifts, integrated luminosities observable sulfur nitrogen emission lines. demonstrate that these predictions agreement current data on ionized species This contrast magnetic wind models, which systematically underpredict luminosities. However, present cannot easily account for neutral oxygen lines