Astronomy and Astrophysics – Astronomy
Scientific paper
Jan 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21710404r&link_type=abstract
American Astronomical Society, AAS Meeting #217, #104.04; Bulletin of the American Astronomical Society, Vol. 43, 2011
Astronomy and Astrophysics
Astronomy
Scientific paper
I will discuss results of 2D and 3D MHD simulations of disk accretion onto young rotating magnetized stars. The disk magnetosphere interaction leads to formation of funnel streams and hot spots on the stellar surface. The energy distribution in the spots is such that the highest energy photons are expected to radiate from the central parts of spots. The oscillation of the shock wave is expected but it can be smeared by the inhomogeneity in the shock front. If the disk carries the magnetic field, then the disk magnetosphere interaction leads to reconnection events and possibly to the X-ray flares. MRI simulations show different flaring behavior in cases of the parallel and anti-parallel fields. Non-stationary accretion can lead to the conical shaped winds similar to X-winds from the disk-magnetosphere boundary, where 10-30 percent of matter is accelerated by the magnetic force up to and beyond the escape speed. A smaller part of matter is accelerated up to much higher velocities in the axial region along stellar field lines. Research is supported by NASA and NSF grants.
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