Authors: R.V.E. Lovelace, M.M. Romanova, and W.I. Newman

A model and simulation code have been developed for time-dependent axisymmetric disk accretion onto a compact object including for the first time the influence of an ordered magnetic field. The accretion rate and radiative luminosity of the disk are naturally coupled to the rate of outflow of energy and angular momentum in magnetically driven z winds. The magnetic field of the wind is treated in a phenomenological way suggested by self-consistent wind solutions. The radial accretion speed u(r,t) of the disk matter is shown to be the sum of the usual viscous contribution and a magnetic contribution r2/3 Bp2 / s where Bp (r,t) is the poloidal field threading the disk and s (r,t) is the disk's surface mass density. An enhancement or variation in Bp   at a large radial  distance leads to the formation of a soliton-like structure in the disk density, temperature, and B-field which propagates implosively inward. The implosion gives a burst in the power output in winds or jets and a simultaneous burst in the disk radiation. The model is pertinent to the formation of discrete fast moving components in jets observed by very - long - baseline interferometry. These components appear to originate at times of optical outbursts of the active galactic nucleus. 



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Last updated on 29.01.07