This research centers on accretion and outflow in rotating stars with magnetic fields. Examples of such objects include young T Tauri stars, white dwarfs in cataclysmic variables, and neutron stars in various binary systems. Here, a theoretical and computational effort will be undertaken in which advanced modeling codes, including a 3D program using a cubed sphere numerical grid, will be used to investigate accretion and outflow processes among such stars. Specific goals are to: (1) Better understand how disk material interacts with stellar magnetospheres, and which instabilities are responsible for launching the disk matter to the magnetic field lines of the star. (2) To explore how the multipolar structure of a stellar magnetosphere influences the accretion process. And (3) to determine what is the dominant mechanism of launching outflows from magnetized stars. The techniques and numerical methods developed here will also have general value and are applicable in other areas of science like planetary science, geophysics, earth magnetospheric science, heliospheric science, and in engineering. Young scientists (including undergraduates and graduate students) will be trained in magnetohydrodynamics. A research associate will also be supported who, in addition to working closely with the Principle Investigators, will aid in the education of students. Results from this work will be incorporated into the groups outreach programs, including and exhibit at the local Science Center and in an outreach program being developed for school children and teachers.
