MAGNETOSPHERIC ACCRETION MODELS FOR THE HYDROGEN EMISSION-LINES OF T-TAURI STARS

Using a statistical equilibrium radiative transfer treatment, we exami ne the behavior of hydrogen emission lines arising from the magnetosph eric infall zones of classical T Tauri stars. Having calculated self-c onsistent line profiles of the Balmer lines, Pa beta and Br gamma, we explore parameter space, examining the effects of the magnetospheric g as temperature and size on the line fluxes. We compare model and obser ved line fluxes for the Balmer lines and find a good match using a rel atively small. range of parameters. We are also able to match the obse rved Br gamma line profile of the embedded object WL 16, which support s the use of the infrared lines in studying magnetospheric infall even in the earliest stages of star formation. Finally, we discuss constra ints on the physical parameters and the possibility of using the emiss ion lines as accretion rate indicators.