Observations of T Tauri stars using Hubble Space Telescope GHRS.: I.: Far-ultraviolet emission lines

We have analyzed Goddard High Resolution Spectrograph data of eight classical T Tauri stars (CTTSs) and one weak-lined T Tauri star (WTTS). The GHRS data consist of spectral ranges 40 Angstrom wide centered on 1345, 1400, 1497, 1550, and 1900 Angstrom. These UV spectra show strong Si IV and C IV emission and large quantities of sharp (similar to40 km s(-1)) H-2 lines. All the H-2 lines belong to the Lyman band, and all the observed lines are single peaked and optically thin. The averages of all the H-2 lines centroids for each star are negative, which may indicate that they come from an outflow. We interpret the emission in H-2 as being the result of fluorescence, mostly by H-Lyalpha, and identify seven excitation routes within 4 Angstrom of that line. We obtain column densities (10(12)-10(15) cm(-2)) and optical depths (similar to1 or less) for each exciting transition. We conclude that the populations are far from being in thermal equilibrium. We do not observe any lines excited from the far blue wing of which implies that the molecular features are excited by an absorbed profile. Si IV and C IV (corrected for emission) have widths of similar to200 km s(-1) and an array of centroids (blueshifted lines, centered, redshifted). These characteristics are difficult to understand in the context of current models of the accretion shock. For DR Tau we observe transient strong blueshifted emission, perhaps the result of reconnection events in the magnetosphere. We also see evidence of multiple emission regions for the hot lines. While C IV is optically thin in most stars in our sample, Si IV is not. However, C IV is a good predictor of Si IV and H2 emission. We conclude that most of the flux in the hot lines may be caused by accretion processes, but the line profiles can have multiple and variable components.