The computational method described above was originally implemented in a FORTRAN code by C. Johns-Krull to calculate H Alpha and H Beta line profiles for the T Tauri star SU Aur, which results are presented and discussed in Johns & Basri (1995b). That code was kindly provided by C. Johns-Krull for the work presented here. In order to calculate Pa Beta and Br Gamma profiles the code was changed so that the optical depths and source functions of these lines could also be computed.