Magneto-Centrifugal Launching of Jets from Accretion Disks. II: Inner Disk-Driven Winds

Details Magneto-Centrifugal Launching of Jets from Accretion Disks. II: Inner Disk-Driven Winds Magneto-Centrifugal Launching of Jets from Accretion Disks. II: Inner Disk-Driven Winds

2003-06-25

arxiv.org/abs/astro-ph/0306519v1

Astrophys.J.595:631,2003

Astronomy and Astrophysics

Astrophysics

11 pages, 6 figures. Accepted for publication in ApJ, scheduled for vol. 595, October 1, 2003

Scientific paper

10.1086/377494

We follow numerically the time evolution of axisymmetric outflows driven magneto-centrifugally from the inner portion of accretion disks, from their launching surface to large, observable distances. Special attention is paid to the collimation of part of the outflow into a dense, narrow jet around the rotation axis, after a steady state has been reached. For parameters typical of T Tauri stars, we define a fiducial ``jet'' as outlined by the contour of constant density at 10^4 cm^{-3}. We find that the jet, so defined, appears nearly cylindrical well above the disk, in agreement with previous asymptotic analyses. Closer to the equatorial plane, the density contour can either bulge outwards or pinch inwards, depending on the conditions at the launching surface, particularly the mass flux distribution. We find that even though a dense, jet-like feature is always formed around the axis, there is no guarantee that the high-density axial jet would dominate the more tenuous, wide-angle part of the wind. Specifically, on the 100 AU scale, resolvable by HST and ground-based adaptive optics for nearby T Tauri winds, the fraction of the wind mass flux enclosed by the fiducial jet can vary substantially, again depending on the launching conditions. We show two examples in which the fraction is ~20% and ~45%. These dependences may provide a way to constrain the conditions at the launching surface, which are poorly known at present.

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