Physics – Plasma Physics
Scientific paper
Nov 1998
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998aps..dpp.b1m03v&link_type=abstract
American Physical Society, Division of Plasma Physics Meeting, November 16-20, 1998 New Orleans, LA, abstract #B1M.03
Physics
Plasma Physics
Scientific paper
A review is made of magnetohydrodynamic (MHD) theory, simulations, and observations of the origin of outflows from accretion disks. Stationary magnetohydrodynamic outflows from a rotating accretion disk have recently been found and studied by time-dependent axisymmetric simulations.(G.V. Ustyugova, A.V. Koldoba, M.M. Romanova, V.M. Chechetkin, and R.V.E. Lovelace, Magneto-Centrifugally Driven Winds: Comparison of MHD Simulations with Theory), Astrophysical Journal, 1998, submitted. The accretion disk is treated as a perfectly conducting, constant density boundary [ρ(r)] with Keplerian rotation. The outflow velocity from this surface is not specified but rather is determined self-consistently from the MHD equations. The temperature of the matter outflowing from the disk is small in the region where the magnetic field is inclined away from the symmetry axis (c_s^2 << v_K^2), but relatively high (c_s^2 buildrel < \over ~ v_K^2) at small radii in the disk where the magnetic field is not inclined away from the axis (where cs is the sound speed and vK is the rotation velocity of the disk). We have found a large class of stationary MHD winds which go super-fast-magnetosonic and exceed the escape speed. The outflows are approximately radial with only small collimation within the simulation region. Close to the disk the outflow is driven by the centrifugal force while at all larger distances the flows are driven by the magnetic force J × B/c. We show that care in the treatment of the outer boundary conditions is required to avoid artificial collimation of the outflows.
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