Abstract
We review recent axisymmetric and three-dimensional (3D) magnetohydrodynamic (MHD) numerical simulations of magnetospheric accretion, plasma-field interaction and outflows from the disk-magnetosphere boundary.
Highlights
Important magnetic fields are present in many classes of accreting stars
The light-curves from these stars show complex patterns of periodic, quasi-periodic, or irregular variability which can be connected with different processes at the disk-magnetosphere boundary, such as complex paths of matter flow around the magnetosphere, rotations of the hot spots, waves excited in the inner disk, inflation and reconnection of external magnetic field lines of the magnetosphere, and other processes (e.g., [1])
Outflows are observed from a number of Classical T Tauri stars (CTTSs) (e.g., [2]) and a few accreting neutron stars and white dwarfs (e.g., [3])
Summary
Important magnetic fields are present in many classes of accreting stars. Some of them are very young, such as Classical T Tauri stars (CTTSs), while others are very old — white dwarfs and neutron stars. Outflows are observed from a number of CTTSs (e.g., [2]) and a few accreting neutron stars and white dwarfs (e.g., [3]). Some of the outflows may originate at the disk-magnetosphere boundary (e.g., [4, 5]). The problem of the disk-magnetosphere interaction is multidimensional and requires global axisymmetric and three-dimensional (3D) numerical simulations. We describe results of recent numerical simulations of magnetospheric accretion and outflows from the disk-magnetosphere boundary
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