paper

The Structure of Magnetocentrifugal Winds I. Steady Mass Loading

arXiv:astro-ph/0410704 · doi:10.1086/432040

Abstract

We present the results of a series of time-dependent numerical simulations of cold, magnetocentrifugally launched winds from accretion disks. Our simulations span four and half decades of mass loading; in the context of a disk with a launching region from $0.1\AU$ to $1.0\AU$ around a $1\solarmass$ star and a field strength of about $20\gauss$ at the inner disk edge, this amounts to mass loss rates of -- $3\times 10^{-5}\solarmassyear$ from each side of the disk. We find that the degree of collimation of the wind increases with mass loading; however even the ``lightest'' wind simulated is significantly collimated compared with the force-free magnetic configuration of the same magnetic flux distribution. The implication is that for flows from young stellar objects a radial field approximation is inappropriate. Surprisingly, the terminal velocity of the wind and the magnetic lever arm are still well-described by the analytical solutions for a radial field geometry. We also find that the isodensity contours and Alfvén surface are very nearly self-similar in mass loading. The wind becomes unsteady above some critical mass loading rate. For a small enough injection speed, we are able to obtain the first examples of a class of heavily-loaded magnetocentrifugal winds with magnetic fields completely dominated by the toroidal component all the way to the launching surface.

arXiv comment36 pages, including 19 figures, LaTeX, revised and accepted by ApJ

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