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Flow Structure in Magnetic CVs

Published online by Cambridge University Press:  23 April 2012

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

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We present a review of the modern concept of physical processes which go on in magnetic CVs with the mass transfer between the components. Using results of 3D MHD simulations, we investigated variations of the main characteristics of accretion disks depending on the value of the magnetic induction on the surface of the accreting star. In the frame of a self-consistent description of the MHD flow structure in close binaries, we formulate conditions of the disk formation and find a criterion that separates two types of flows corresponding to intermediate polars (intermediate magnetic field) and polars (strong field).

The influence of asynchronous rotation of the accretor on the flow structure in magnetic close binaries is also discussed. Simulations show that the accretion instability arising in binaries with rapid rotation of accretor (“propeller” regime) can explain the mechanism of quasi-periodic dwarf nova outbursts observed in DQ Her systems.

Keywords

binaries: closeMHDaccretion disks
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 7 , Symposium S282: From Interacting Binaries to Exoplanets: Essential Modeling Tools , July 2011 , pp. 509 - 516
Copyright
Copyright © International Astronomical Union 2012

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