Abstract
After briefly reviewing the evidence for disk-driven winds in young stellar objects, the author concentrates on one attractive mechanism that offers a natural explanation for the inferred link between accretion disks and energetic outflows in young stars. He discusses the origin of the magnetic field in the disk and its coupling to the mostly neutral matter in different density regimes. He then describes the general dynamical and kinematic characteristics of such outflows as well as their expected thermal structure, and points out some of the observational implications of these properties.
