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Magnetic field generation in an accretion disk of close binary star

Published online by Cambridge University Press:  18 July 2013

Dmitry V. Bisikalo  and
Andrey G. Zhilkin
Dmitry V. Bisikalo
Affiliation:
Institute of Astronomy of the RAS, 48 Pyatnitskaya str., Moscow, Russia, email: bisikalo@inasan.ru
Andrey G. Zhilkin
Affiliation:
Institute of Astronomy of the RAS, 48 Pyatnitskaya str., Moscow, Russia, email: bisikalo@inasan.ru
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Abstract

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Using results of 3D MHD numerical simulations we investigate the generation of the magnetic field in an accretion disk of a close binary star. Analysis of the numerical simulations shows that the magnetic field, which is mainly toroidal, is intensively generated in the accretion disk. In the disk, we can distinguish three regions: inner region of the intensive toroidal field generation due to the differential rotation; region of the current sheets; and outer region of the magnetic field dissipation. In the outer regions of the accretion disk of a magnetic close binary system two types of the dynamo may exist. One of them is the laminar dynamo that occurs as a result of the nonaxisymmetric motions. The other type is the turbulent αω-dynamo. Numerical simulations show that during the disk lifetime the dynamo effect in the outer region of the disk can be significant.

Keywords

Accretion disksbinaries: closeMHDdynamo
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S294: Solar and Astrophysical Dynamos and Magnetic Activity , August 2012 , pp. 187 - 192
Copyright
Copyright © International Astronomical Union 2013 

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