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Time–Latitudinal Development of the White-Light Coronal Structures over a Solar Cycle

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Abstract

Large-scale coronal structures (helmet streamers) observed in the white-light corona during total solar eclipses and/or with ground-based coronagraphs are mostly located only above quiescent types of prominences. These helmet streamers are maintained due to the magnetic fields of the Sun. Time–latitudinal distribution of prominences during a solar cycle, however, shows both the poleward and equatorward migrations, similar to the 530.3 nm emission corona (the green corona) intensities. Distribution of observed coronal helmet streamers during total solar eclipses, enlarged with the helmet streamers as were obtained by the ground-based coronagraph observations, are compared with the heliographic distribution of prominences and the green corona intensities for the first time. It is shown that the distribution of above-mentioned helmet streamers, reflects – roughly – the time–latitudinal distribution of prominences and emission corona branches, and migrates together with them over a solar cycle.

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Authors and Affiliations

  1. Observatory Úpice, U Lipek 160, 542 32 Úpice, Czech Republic

    Marcel BělÍk & Eva MarkovÁ

  2. Astronomical Institute, Slovak Academy of Sciences, 059 60 Tatranská Lomnica, Slovakia

    Vojtech Rušin & Milan Minarovjech

Authors
  1. Marcel BělÍk
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  2. Eva MarkovÁ
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  3. Vojtech Rušin
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  4. Milan Minarovjech
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Correspondence to Vojtech Rušin.

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BělÍk, M., MarkovÁ, E., Rušin, V. et al. Time–Latitudinal Development of the White-Light Coronal Structures over a Solar Cycle. Sol Phys 224, 269–275 (2004). https://doi.org/10.1007/s11207-005-5720-0

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  • DOI: https://doi.org/10.1007/s11207-005-5720-0

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