Coronal Hole and Solar Global Magnetic Field Evolution in 1976-2012

Bilenko, I.A.; Tavastsherna, K.S.

Авторы: Bilenko I.A., Tavastsherna K.S.
Журнал: Solar Physics
Том: 291
Номер: 8
Год издания: 2016
Издательство: Springer Netherlands
Местоположение издательства: Dordrecht, Netherlands
Первая страница: 2329
Последняя страница: 2352
DOI: 10.1007/s11207-016-0966-2
Аннотация: We study the spatial-temporal evolution of a coronal hole and compare it with that of the solar global magnetic field in Cycles 21 – 23 (1976 – 2012). We also analyze the latitude-longitude distribution dynamics of coronal holes and the regularities in the global magnetic field associated with the solar polar field reversal. Polar and non-polar coronal hole populations are considered. The investigation reveals some temporal and spatial regularities in coronal hole distributions that match the global magnetic-field cycle evolution well. The results show that the non-polar coronal hole longitudinal distribution follows all configuration changes in the global magnetic-field structure. Reorganizations of the global magnetic field and coronal hole distributions occur simultaneously during a time interval of a few solar rotations. The cycle evolution of the non-polar coronal holes reflects the transition of the solar global magnetic field from the zonal structure to sectorial and vice versa. Two different types of waves of non-polar coronal holes are revealed from their latitudinal distribution. The first are short poleward waves. They trace the poleward motion of the unipolar photospheric magnetic fields from approximately 35◦ to the associated pole in each hemisphere and the redevelopment of a new-polarity polar CH. Although they start the poleward movement before the change of the polar magnetic field in the associated hemisphere, they reach the pole after the polar reversal. The other type of non-polar CH wave forms two sinusoidal branches associated with the positive- and negative-polarity magnetic fields. The complete period of the wave is equal to ≈ 268 CRs (22 years). These wave CHs arrive at high latitudes during declining phases when the new-polarity polar CHs are already completely formed.
Добавил в систему: Биленко Ирина Антоновна

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Coronal Hole and Solar Global Magnetic Field Evolution in 1976-2012статья Исследовательская статья

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