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Magnetohydrodynamic stability of broad line region clouds

Authors

  • Martin Krause,

    Corresponding author
    1. Max-Planck-Institut für Extraterrestrische Physik, Giessenbachstr., Garching, Germany
    • Universitätssternwarte München, München, Germany
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  • Marc Schartmann,

    1. Universitätssternwarte München, München, Germany
    2. Max-Planck-Institut für Extraterrestrische Physik, Giessenbachstr., Garching, Germany
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  • Andreas Burkert

    1. Universitätssternwarte München, München, Germany
    2. Max-Planck-Institut für Extraterrestrische Physik, Giessenbachstr., Garching, Germany
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    • Max-Planck fellow.


E-mail: krause@mpe.mpg.de, mkrause@usm.lmu.de

ABSTRACT

Hydrodynamic stability has been a longstanding issue for the cloud model of the broad line region in active galactic nuclei. We argue that the clouds may be gravitationally bound to the supermassive black hole. If true, stabilization by thermal pressure alone becomes even more difficult. We further argue that if magnetic fields are present in such clouds at a level that could affect the stability properties, they need to be strong enough to compete with the radiation pressure on the cloud. This would imply magnetic field values of a few gauss for a sample of active galactic nuclei we draw from the literature.

We then investigate the effect of several magnetic configurations on cloud stability in axisymmetric magnetohydrodynamic simulations. For a purely azimuthal magnetic field which provides the dominant pressure support, the cloud first gets compressed by the opposing radiative and gravitational forces. The pressure inside the cloud then increases, and it expands vertically. Kelvin–Helmholtz and column density instabilities lead to a filamentary fragmentation of the cloud. This radiative dispersion continues until the cloud is shredded down to the resolution level. For a helical magnetic field configuration, a much more stable cloud core survives with a stationary density histogram which takes the form of a power law. Our simulated clouds develop sub-Alfvénic internal motions on the level of a few hundred km s−1.

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