The observational effort in obtaining high resolution hydrogen line spectra in T Tauri stars has been accompanied by modeling the line profiles in an attempt to explain the wealth of information they provide. Published models have been concentrating in the study of Balmer line profiles, especially H Alpha, and the results obtained have been discussed in previous chapters. Near infrared lines have seldom been modeled, mainly due to the lack of high signal-to-noise high spectral resolution observations. That is put to an end with the Pa Beta and Br Gamma data presented here. In order to take full advantage of these data, Pa Beta and Br Gamma line profile modeling requiring full radiative transfer is necessary.
Producing a radiative transfer code leading to the calculation of line profiles can, on its own, be the subject of a full Ph.D. dissertation, which is not the aim here. However, in order to compare the data with model results, very simple wind and accretion models were set up making use of procedures that do not involve the development from scratch of such a code.