Accretion channeling in classical T Tauri stars

It is now accepted that accretion in classical T Tauri stars is controlled by the stellar magnetosphere, as opposed to the traditional disk boundary layer model. The magnetosphere truncates the disk at several stellar radii allowing material to couple to the field and fall toward the star. Observations indicate the presence of hot spots on the stellar surface where accretion flows impact the photosphere. By considering magnetic fields with a realistic degree of complexity we demonstrate that the geometry of the field strongly affects the location and distribution of hot spots - the signatures of accretion.