Observations of jets from accretion disks have constrained the launching radius to be confined to a zone close to the centre of the disk. The time evolution of a viscous, resistive accretion disk with a radially varying magnetisation distribution is studied. The magnetic field is advected into the centre of the disk over two accretion timescales. The magnetic field distribution evolves towards a power law. The field lines bend sharply near the disk surface. A super-fast magnetosonic wind is launched from the innermost region of the disk due to numerical effects.
CITATION STYLE
Murphy, G. C., Zanni, C., & Ferreira, J. (2009). Magnetic field advection in weakly magnetised viscous resistive accretion disks: Numerical simulations. In Astrophysics and Space Science Proceedings (Vol. 0, pp. 117–122). Springer Science and Business Media B.V. https://doi.org/10.1007/978-3-642-00576-3_14
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