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The magnetic-field structure in a stationary accretion disk

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Abstract

The magnetic-field structure in regions of stationary, planar accretion disks around active galactic nuclei where general-relativistic effects can be neglected (from 10 to 200 gravitational radii) is considered. It is assumed that the magnetic field in the outer edges of the disk, which forms in the magnetosphere of the central black hole during the creation of the relativisitic jets, corresponds to the field of a magnetic dipole perpendicular to the plane of the disk. In this case, the azimuthal field component B φ in the disk arises due to the presence of the radial field B ρ and the azimuthal velocity component U φ . The value of the magnetic field at the inner radius of the disk is taken to correspond to the solution of the induction equation in a diffusion approximation. Numerical solutions of the induction equation are given for a number of cases.

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Authors and Affiliations

  1. Central (Pulkovo) Astronomical Observatory, Russian Academy of Sciences, Pulkovskoye shosse 65, St. Petersburg, 196140, Russia

    M. Yu. Piotrovich, N. A. Silant’ev, Yu. N. Gnedin, T. M. Natsvlishvili & S. D. Buliga

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  1. M. Yu. Piotrovich
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  2. N. A. Silant’ev
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  3. Yu. N. Gnedin
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  4. T. M. Natsvlishvili
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  5. S. D. Buliga
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Correspondence to M. Yu. Piotrovich.

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Original Russian Text © M.Yu. Piotrovich, N.A. Silant’ev, Yu.N. Gnedin, T.M. Natsvlishvili, S.D. Buliga, 2016, published in Astronomicheskii Zhurnal, 2016, Vol. 93, No. 5, pp. 463–473.

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Piotrovich, M.Y., Silant’ev, N.A., Gnedin, Y.N. et al. The magnetic-field structure in a stationary accretion disk. Astron. Rep. 60, 486–497 (2016). https://doi.org/10.1134/S1063772916040090

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  • DOI: https://doi.org/10.1134/S1063772916040090

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