  The inner 0.1 AU around accreting T Tauri stars hold clues to many physical
processes that characterize the early evolution of solar-type stars. The
accretion-ejection connection takes place at least in part in this compact
magnetized region around the central star, with the inner disk edge interacting
with the star's magnetosphere thus leading simultaneously to magnetically
channeled accretion flows and to high velocity winds and outflows. The magnetic
star-disk interaction is thought to have strong implications for the angular
momentum evolution of the central system, the inner structure of the disk, and
possibly for halting the migration of young planets close to the stellar
surface. We review here the current status of magnetic field measurements in T
Tauri stars, the recent modeling efforts of the magnetospheric accretion
process, including both radiative transfer and multi-D numerical simulations,
and summarize current evidence supporting the concept of magnetically-channeled
accretion in young stars. We also discuss the limits of the models and
highlight observational results which suggest that the star-disk interaction is
a highly dynamical and time variable process in young stars.
