Electromagnetic Fields in Jets

Abstract

The magnetic fields and energy flows in an astronomical jet described by our earlier model are calculated in detail. Though the field distribution varies with the external pressure function p(z), it depends only weakly on the other boundary conditions. Individual fieldlines were plotted; the lines become nearly vertical at the bottom and are twisted at the top. An animation of a fieldline's motion was made, which shows the line being wound up by the accretion disc's differential rotation and rising as a result of this. The distribution of Poynting flux within the jet indicates that much of the energy flows up the jet from the inside of the accretion disc but a substantial fraction flows back down to the outside.

8 pages, 5 figures. Accepted for publication in MNRAS

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• Relativistic Jets and Long-Duration Gamma-ray Bursts from the Birth of Magnetars
• Three-Dimensional MHD Simulation of Caltech Plasma Jet Experiment: First Results
• Fields from a relativistic magnetic explosion
• A New Interpretation for the Hot Corona in Active Galactic Nuclei