Computer Science
Scientific paper
Sep 1998
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998phdt........12g&link_type=abstract
Thesis (PHD). UNIVERSITY OF WASHINGTON , Source DAI-B 59/03, p. 1155, Sep 1998, 152 pages.
Computer Science
Magnetohydrodynamics
Scientific paper
A new model for the formation of jets from magnetized young stars is presented in this dissertation. In the new model, magnetic loops which connect the star to the surrounding accretion disk become twisted due to differential rotation. The twisting of field increases the overall field strength due to the induction of an azimuthal component Bφ. As the magnetic pressure (B2) increases, the magnetic field expands. Plasma attached to the high latitude portions of the expanding loops is driven towards the rotation axis, producing a hot, well collimated high velocity component of the outflow. Plasma attached to the expanding loops at lower latitudes is driven outwards along the surface of the disk, resulting in a poorly collimated, cool, low velocity component of the outflow. Magnetic reconnection frees the plasma from the system and allows the process to repeat. Accretion by the star is modulated by magnetic reconnection if the diffusivity in the disk is low enough to inhibit field slippage in the radial direction. It is demonstrated in this dissertation that under low diffusivity conditions, accretion and jet production are both unsteady. This work also defines three classes of accretion flows in strongly magnetic systems, with the effective magnetic diffusivity in the disk determining the difference. This model qualitatively reproduces the observed jet morphology, velocity spectra, and X-Ray flare activity. As such, it can make important predictions concerning the relationship between accretion rate, mass outflow, and variability in X-Ray flux, UV veiling, and IR excess associated with T-Tauri stars. An understanding of the mechanism behind stellar jets may be in hand.
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