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The three-dimensional structure of the solar corona

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Abstract

The surface where the radial component of the solar magnetic field changes sign is computed for a minimum corona. It is shown that (1) the projection of the folds of this surface onto the plane of the sky is consistent with the helmet structures observed during the eclipse of June 30, 1954; (2) there are type 1 and type 2 helmets, according to the well-known classification of coronal structures; (3) some elements of this sign-change surface of the radial field can be classified as so-called envelopes. The results obtained suggest that more complex coronal structures can be described in a similar way. An MHD model of polar plumes is considered.

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Authors and Affiliations

  1. Institute of Astrophysics, Paris, France

    S. L. Koutchmy

  2. Institute of Terrestrial Magnetism, the Ionosphere, and Radio Wave Propagation, Russian Academy of Sciences, Troitsk, Moscow oblast, 142190, Russia

    V. L. Merzlyakov & M. M. Molodenskii

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  1. S. L. Koutchmy
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  2. V. L. Merzlyakov
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  3. M. M. Molodenskii
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__________

Translated from Astronomicheski\(\overset{\lower0.5em\hbox{$\smash{\scriptscriptstyle\smile}$}}{l} \) Zhurnal, Vol. 78, No. 10, 2001, pp. 953–960.

Original Russian Text Copyright © 2001 by Koutchmy, Merzlyakov, Molodenski\(\overset{\lower0.5em\hbox{$\smash{\scriptscriptstyle\smile}$}}{l} \).

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Koutchmy, S.L., Merzlyakov, V.L. & Molodenskii, M.M. The three-dimensional structure of the solar corona. Astron. Rep. 45, 834–840 (2001). https://doi.org/10.1134/1.1408984

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