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Conference Paper

Variation of coronal mass ejection Properties over solar cycles

Authors

Gopalswamy,  Nat
IUGG 2023, General Assemblies, 1 General, International Union of Geodesy and Geophysics (IUGG), External Organizations;

Michalek,  Grzegorz
IUGG 2023, General Assemblies, 1 General, International Union of Geodesy and Geophysics (IUGG), External Organizations;

Yashiro,  Seiji
IUGG 2023, General Assemblies, 1 General, International Union of Geodesy and Geophysics (IUGG), External Organizations;

Makela,  Pertti
IUGG 2023, General Assemblies, 1 General, International Union of Geodesy and Geophysics (IUGG), External Organizations;

Xie,  Hong
IUGG 2023, General Assemblies, 1 General, International Union of Geodesy and Geophysics (IUGG), External Organizations;

Akiyama,  Sachiko
IUGG 2023, General Assemblies, 1 General, International Union of Geodesy and Geophysics (IUGG), External Organizations;

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Citation

Gopalswamy, N., Michalek, G., Yashiro, S., Makela, P., Xie, H., Akiyama, S. (2023): Variation of coronal mass ejection Properties over solar cycles, XXVIII General Assembly of the International Union of Geodesy and Geophysics (IUGG) (Berlin 2023).
https://doi.org/10.57757/IUGG23-3905


Cite as: https://gfzpublic.gfz-potsdam.de/pubman/item/item_5020642
Abstract
While most of the properties of Coronal Mass Ejections (CMEs) have been established soon after their discovery in the early 1970s, a wealth of information have been accumulated especially because of the data from the SOHO and STEREO missions. This paper is focused on the solar cycle variation of CMEs at the Sun and in the interplanetary medium. We provide an update on the variation of CME properties over solar cycles 23-25. While the solar activity cycle is primarily expressed in terms of the Sunspot number (SSN), CMEs provide a different perspective on the owing to their origin in sunspot regions as well as other non-spot magnetic regions such as quiescent filament regions. Only very energetic CMEs originate almost exclusively from solar active regions, where large quantities of magnetic free energy can be stored and released. The multiple types of CME solar sources result in a variation of the correlation between CME occurrence rate and SSN as a function of the solar cycle phase (rise, maximum, and declining phases). Weak solar activity observed in solar cycle 24 has been found to result in a weak heliospheric state, which backreacts on CME properties. In addition to CME rate, we also discuss the properties of associated phenomena such as prominences, solar energetic particle events, interplanetary CMEs, and type II radio bursts. We also compare the CME rate vs. SSN relation among the three recent solar cycles: 23, 24, and 25.