Modeling the Hα line emission around classical T Tauri stars using magnetospheric accretion and disk wind models

The authors study the profiles of classical T Tauri star (CTTS) Hα lines in a model that includes both magnetospheric accretion and a disk wind. They show that the Hα line strongly depends on the densities and temperatures inside the magnetosphere and the disk wind region. The bulk of the flux comes from the magnetospheric component for the usual CTTS parameters, but the disk wind contribution becomes more important as the mass accretion rate, the temperatures, and densities of the wind increase. They also show that most of the disk wind contribution to the Hα line is emitted at the innermost region of the disk wind.