The wind models explored in this work produce mostly normal P Cygni line profiles. These are not observed in any of the observed Pa Beta or Br Gamma line profiles. The one star for which Pa Beta displays a blueshifted absorption (CW Tau) was modeled using a wind with characteristics similar to those of the Johns & Basri (1995b) wind for SU Aur. While a reasonably good match was obtained for Pa Beta, the predicted shape for the Br Gamma line (normal P Cygni shape) is not verified. In fact, the latter displays an IPC profile.
The accretion models explored produce IPC line profiles at Pa Beta and
Br Gamma. The observed line widths and peak intensities can be explained by
a range of mass accretion rates (
M
M
yr-1) and by a range of radii from which free fall
occurs (
), however the redshifted absorption in the
model profiles is, in general, too deep when compared to the
observations. The observed range of emission peak strength to IPC depth
is not therefore reproduced, indicating that true spherically symmetric
accretion is not ocurring in these stars.
Neither the spherically symmetric accretion nor wind models explored here were able to produce Type I line profiles with peak intensities similar to those observed. Thorough radiative transfer calculations in a more realistic accretion geometry are needed to address these problems.