  Recent spectropolarimetric observations suggest that young low-mass stars
such as classical T Tauri stars (CTTSs) possess relatively strong (~kG)
magnetic field. This supports a scenario in which the final accretion onto the
stellar surface proceeds through a magnetosphere, and the winds are formed in
magnetohydrodynamics (MHD) processes. We examine recent numerical simulations
of magnetospheric accretions via an inclined dipole and a complex magnetic
fields. The difference between a stable accretion regime, in which accretion
occurs in ordered funnel streams, and an unstable regime, in which gas
penetrates through the magnetosphere in several unstable streams due to the
magnetic Rayleigh-Taylor instability, will be discussed. We describe how MHD
simulation results can be used in separate radiative transfer (RT) models to
predict observable quantiles such as line profiles and light curves. The
plausibility of the accretion flows and outflows predicted by MHD simulations
(via RT models) can be tested against observations. We also address the issue
of outflows/winds that arise from the innermost part of CTTSs. First, we
discuss the line formations in a simple disk wind and a stellar wind models. We
then discuss the formation of the conically shaped magnetically driven outflow
that arises from the disk-magnetosphere boundary when the magnetosphere is
compressed into an X-type configuration.
