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Features of the Evolution of Active and Quiet Structures in Two Levels of the Sun’s Atmosphere

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Abstract

This paper analyzes the latitudinal and temporal variations of magnetic fields in the photosphere and variations of solar structures, such as active regions, coronal holes, and flocculi, in the Sun’s upper chromosphere. The investigation is based on two types of solar observations obtained in the Kitt Peak observatory (United States) during almost three solar cycles, from January 1, 1977 to September 30, 2003. These are the synoptic maps of the strength of the longitudinal magnetic field of the Sun and observations of the solar chromosphere in the He I 1083 nm line. The aim of this work was to reveal features and interconnection of variations in magnetic fields of the photosphere and solar structures in the upper chromosphere in this period. Detailed comparison of weak magnetic fields (0–20 G) with coronal holes and stronger magnetic fields (50–200 G) with active regions reveals some features in the evolution of active and quiet structures in two levels of the Sun’s atmosphere―in the photosphere and in the chromosphere.

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ACKNOWLEDGMENTS

This work used NSO/Kitt Peak (United States) data obtained from January 1, 1977 to September 30, 2003 in cooperation of NSF/NOAO, NASA/GSFC, and NOAA/SEL. We are grateful to all organizations for the possibility to use the observational material and, especially, to Dr. J. Harvey who was kind enough to give us access to the data.

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  1. Crimean Astrophysical Observatory, Russian Academy of Sciences, Nauchny, Crimea, 98409, Russia

    O. A. Andreeva

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Correspondence to O. A. Andreeva.

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Translated by A. Nikol’skii

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Andreeva, O.A. Features of the Evolution of Active and Quiet Structures in Two Levels of the Sun’s Atmosphere. Geomagn. Aeron. 62, 873–881 (2022). https://doi.org/10.1134/S0016793222070052

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