  Establishing the origin of accretion powered winds from forming stars is
critical for understanding angular momentum evolution in the star-disk
interaction region. Here, the high velocity component of accretion powered
winds is launched and accreting stars are spun down, in defiance of the
expected spin-up during magnetospheric accretion. T Tauri stars in the final
stage of disk accretion offer a unique opportunity to study the connection
between accretion and winds and their relation to stellar spindown. Although
spectroscopic indicators of high velocity T Tauri winds have been known for
decades, the line of He I 10830 offers a promising new diagnostic to probe the
magnetically controlled star-disk interaction and wind-launching region. The
high opacity and resonance scattering properties of this line offer a powerful
probe of the geometry of both the funnel flow and the inner wind that, together
with other atomic and molecular spectral lines covering a wide range of
excitation and ionization states, suggests that the magnetic interaction
between the star and disk, and the subsequent launching of the inner high
velocity wind, is sensitive to the disk accretion rate.
