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Impact of the magnetic field on the structure of accretion disks in semi-detached binaries

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Abstract

We discuss characteristic features of the magnetic gas-dynamical structure of the flows in a semi-detached binary system obtained from three-dimensional simulations, assuming that the intrinsic magnetic field of the accreting star is dipolar. The turbulent diffusion of the magnetic field is taken into account. The SS Cyg system is considered as an example. Including the magnetic field can alter the basic parameters of the accretion disk, such as the accretion rate and the characteristic density. The magnetic field in the disk is primarily toroidal.

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Authors and Affiliations

  1. Institute of Astronomy, Russian Academy of Sciences, ul. Pyatnitskaya 48, Moscow, 109017, Russia

    A. G. Zhilkin & D. V. Bisikalo

  2. Chelyabinsk State University, ul. Bratiev Kashirinykh 129, Chelyabinsk, 454021, Russia

    A. G. Zhilkin

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  1. A. G. Zhilkin
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  2. D. V. Bisikalo
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Original Russian Text © A.G. Zhilkin, D.V. Bisikalo, 2009, published in Astronomicheskiĭ Zhurnal, 2009, Vol. 86, No. 5, pp. 475–484.

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Zhilkin, A.G., Bisikalo, D.V. Impact of the magnetic field on the structure of accretion disks in semi-detached binaries. Astron. Rep. 53, 436–445 (2009). https://doi.org/10.1134/S1063772909050072

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  • DOI: https://doi.org/10.1134/S1063772909050072

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