Astronomy and Astrophysics – Astronomy
Scientific paper
May 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21840702l&link_type=abstract
American Astronomical Society, AAS Meeting #218, #407.02; Bulletin of the American Astronomical Society, Vol. 43, 2011
Astronomy and Astrophysics
Astronomy
Scientific paper
We use axisymmetric magnetohydrodynamics (MHD) to investigate the launching and collimation of jets emerging from the disk-magnetosphere boundary of accreting magnetized stars. Our analysis shows that the emergence of a collimated jet is a two-step process: first, the matter is accelerated along field lines extending up from the disk by the magnetic pressure force. Then, the matter is collimated by the toroidal magnetic field in the stellar corona. The jet emerges from the disk-magnetosphere boundary and is weakly matter dominated. The matter in the jet crosses the Alfven and fast magnetosonic surfaces a few stellar radii above the disk. Even far from the disk, the magnetic force continues to accelerate and collimate the jet. We observe a matter ejection-to-accretion ratio of 0.25 in steady state. A high accretion rate can generate the strong magnetic pressure which drives the matter from the disk and as such, these simulations may apply to EXor and FUOR class stars which undergo episodes of enhanced accretion. In general, the models can be applied to many types of magnetized stars--white dwarfs, neutron stars, and brown dwarfs--which exhibit periods of enhanced accretion.
Lii Patrick
Lovelace Richard
Romanova Marina M.
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