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Structure and physics of solar faculae

IV: Chromospheric granular structure

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Abstract

The methods used and the results obtained in the measurement of the distances between the centers of chromospheric granules are described. A coincidence of these structures at two different altitudes was observed. Observations made in the K2v, or in the K3 and CN lines permit the comparison of two different altitudes: the upper and the lower chromosphere. These results include flocculi on the edge of the supergranules as well as plages. Two main results are obtained: (l)the most likely distance between two neighboring granules is, at the minimum of the solar cycle, of about 2″. 60 for K3 and 2″.45 for CN, and (2) this distance is decreasing with growing solar activity.

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Author notes

  1. C. Fang

    Present address: Dept. of Astronomy, University of Nanjing, Nanjing, China

Authors and Affiliations

  1. Observatoire de Paris-Meudon, L.A. 326, 92195, Meudon Principal Cedex, France

    C. Fang & Z. Mouradian

  2. University of Ioannina, Ioannina, Greece

    G. Banos

  3. L.A.T. - I.A.P., 98 bis Bld. Arago, 75014, Paris, France

    S. Dumont & J. C. Pecker

Authors
  1. C. Fang
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  2. Z. Mouradian
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  3. G. Banos
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  4. S. Dumont
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  5. J. C. Pecker
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Fang, C., Mouradian, Z., Banos, G. et al. Structure and physics of solar faculae. Sol Phys 91, 61–70 (1984). https://doi.org/10.1007/BF00213612

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  • DOI: https://doi.org/10.1007/BF00213612

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