Physics
Scientific paper
May 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agusmsh22a..01l&link_type=abstract
American Geophysical Union, Fall Meeting 2007, abstract #SH22A-01
Physics
7524 Magnetic Fields, 7835 Magnetic Reconnection (2723, 7526), 7836 Mhd Waves And Instabilities (2149, 2752, 6050), 2724 Magnetopause And Boundary Layers, 2740 Magnetospheric Configuration And Dynamics
Scientific paper
We discuss recent 2D and 3D MHD numerical simulations of disk accretion to rotating stars with aligned or misaligned dipole magnetic fields. We focus on the main features observed in these simulations: the structure of the magnetospheric plasma flows for different misalignment angles, the structure of the inner regions of the disk, the evolution of the magnetic field, the properties of the hot spots at the surface of the star, and the spin history of the star. We discuss the nature of "funnel flows," where plasma of the inner region of the disk accelerates towards the star along the star's magnetic field. We go on to describe the "propeller stage" of accretion where a rapidly rotating star expels most of the incoming disk matter. The matter is centrifugally driven into conical outflows or winds with super fast magnetosonic speeds above and below the equatorial plane. Closer to the star's rotation axis we find collimated, oppositely-directed, magnetically dominated flows of energy and angular momentum along the open magnetic field lines of the star. In this stage, the magnetically dominated flows or "Poynting jets" cause the star to spins-down rapidly. This work was supported by NASA and NSF.
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