Profiles of strong permitted lines in classical T Tauri stars

We present a spectral analysis of 30 T Tauri stars observed with the Hamilt on echelle spectrograph over more than a decade. One goal is to test magnet ospheric accretion model predictions. Observational evidence previously pub lished supporting the model, such as emission-line asymmetry and a high fre quency of redshifted absorption components, are considered. We also discuss the relation between different line-forming regions and search for good ac cretion rate indicators. In this work we confirm several important points o f the models, such as the correlation between accretion and outflow, broad emission components that are mostly central or slightly blueshifted, and on ly the occasional presence of redshifted absorption. We also show, however, that the broad emission components supposedly formed in the magnetospheric accretion flow only partially support the models. Unlike the predictions, they are sometimes redshifted and are mostly found to be symmetric. The pub lished theoretical profiles do not have a strong resemblance to our observe d ones. We emphasize the need for accretion models to include a strong turb ulent component before their profiles will match the observations. The effe cts of rotation, as well as the outflow components? will also be needed to complete the picture.