Authors: G.V. Ustyugova, A.V. Koldoba, M.M. Romanova, V.M. Chechetkin, and R.V.E. Lovelace

Magnetohydrodynamic simulations have been made of the formation of outflows from a Keplerian disk threaded by a magnetic field. The disk is treated as a boundary condition, where matter is ejected with Keplerian azimuthal speed and poloidal speed less than the slow magnetosonic velocity, and where boundary conditions on the magnetic field correspond to a highly conducting disk. Initially, the space above the disk, the corona, is filled with high specific entropy plasma in the thermal equilibrium in the gravitational potential of the central object. The initial magnetic field is poloidal and is represented by a superposition of monopoles located below the plane of the disk. The rotation of the disk twists the initial poloidal magnetic field, and this twist propagates into the corona pushing and collimating matter into jet-like outflow in a cylindrical region. Matter outflowing from the disk flows and accelerates in the Z-direction owing to both the magnetic and pressure gradient forces. The flow accelerates through the slow magnetosonic and Alfven surfaces and at larger distances through the fast magnetosonic surface. The flow velocity of the jet is approximately parallel to the Z-axis, and the collimation results from the pinching force of the toroidal magnetic field. For a non-rotating disk no collimation is observed.



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Last updated on 29.01.07