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Magnetic tensions can control the dynamics of accretion disks

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Abstract

Magnetic tensions are likely to be the dominant shear force in accretion disks, larger when integrated than turbulent viscosity by an order of magnitude or more. In galactic disks, they guarantee the mass-accretion rate required by the quasar phenomenon. In fast-revolving, clumpy disks, magnetic pressures can exceed static pressures and be amplified towards ram pressures. The inner, near-rigidly rotating parts of galactic disks are suggestive candidates. The gas velocities in such magnetically controlled disks mimic higher central masses than present.

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Authors and Affiliations

  1. Institut für Astrophysik, Bonn, Germany

    W. Kundt

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  1. W. Kundt
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Kundt, W. Magnetic tensions can control the dynamics of accretion disks. Astrophys Space Sci 172, 285–291 (1990). https://doi.org/10.1007/BF00643321

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