  Pre-main-sequence stars are observed to be surrounded by both accretion flows
and some kind of wind or jet-like outflow. Recent work by Matt and Pudritz has
suggested that if classical T Tauri stars exhibit stellar winds with mass loss
rates about 0.1 times their accretion rates, the wind can carry away enough
angular momentum to keep the stars from being spun up unrealistically by
accretion. This paper presents a preliminary set of theoretical models of
accretion-driven winds from the polar regions of T Tauri stars. These models
are based on recently published self-consistent simulations of the Sun's
coronal heating and wind acceleration. In addition to the convection-driven MHD
turbulence (which dominates in the solar case), we add another source of wave
energy at the photosphere that is driven by the impact of plasma in neighboring
flux tubes undergoing magnetospheric accretion. This added energy, determined
quantitatively from the far-field theory of MHD wave generation, is sufficient
to produce T Tauri-like mass loss rates of at least 0.01 times the accretion
rate. While still about an order of magnitude below the level required for
efficient angular momentum removal, these are the first self-consistent models
of T Tauri winds that agree reasonably well with a range of observational mass
loss constraints. The youngest modeled stellar winds are supported by Alfven
wave pressure, they have low temperatures ("extended chromospheres"), and they
are likely to be unstable to the formation of counterpropagating shocks and
clumps far from the star.
