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Problems of magnetic dynamo

 a, b
a Lomonosov Moscow State University, Department of Physics, Leninskie Gory 1 build. 2, Moscow, 119991, Russian Federation
b Pushkov Institute of Terrestrial Magnetism, Ionosphere and Radio Wave Propagation, Russian Academy of Sciences, Kaluzhskoe shosse 4, Troitsk, Москва, 108840, Russian Federation

In what is famously known as the solar activity cycle, every 11 years a wave of quasistationary magnetic field propagates in the solar convective zone from the middle latitudes equatorwards, driven by the dynamo jointly produced by the differential rotation and mirrorasymmetric convection. Similar processes occur in other celestial bodies and can to some extent be reproduced in the lab environment. This paper reviews the current status of and future trends in the study of the dynamo problem.

Fulltext is available at IOP
Keywords: magnetic fields, dynamo, solar activity
PACS: 07.55.Db, 41.20.−q, 91.25.−r, 96.12.Hg, 96.60.Hv (all)
DOI: 10.3367/UFNe.0185.201506h.0643
Citation: Sokoloff D D "Problems of magnetic dynamo" Phys. Usp. 58 601–605 (2015)
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Received: 20th, March 2015, 25th, February 2015

Оригинал: Соколов Д Д «Проблемы магнитного динамо» УФН 185 643–648 (2015); DOI: 10.3367/UFNr.0185.201506h.0643

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