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Distribution of intense, moderate and weak geomagnetic storms over the solar cycle

  • Malik A. Waheed
  • Parvaiz A. KhanEmail author
  • A. K. Gwal
Original Paper
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Abstract

The geomagnetic storms observed during different phases of a solar cycle have distinct primary solar sources. Therefore, we have statistically examined, in the present study, how the geomagnetic storms of different intensities are distributed over a solar cycle. We have considered previous four cycles, viz. cycle 21, 22, 23 and 24. We selected all the storms which were observed during these cycles and classified them into three categories as: intense (Dst ≤ − 100 nT), moderate (− 100 ≤ Dst ≤ − 50) and weak (− 50 ≤ Dst ≤ − 30). We found that geomagnetic storms are distributed in such a way that maximum number of intense storms occur around peak phase of a solar cycle, while maximum number of weak storms occur during the starting and ending phases of a cycle. About 73.20% of intense storms, 58.07% and 47.93% of moderate and weak storms occurred around the peak of a cycle. Therefore, it was concluded that peak phase is dominated by intense and very intense storms due to increase in frequency of occurrence of coronal mass ejections during such periods. At the same time, the ending phase of solar cycle is dominated by the occurrence of weak storms due to the frequent occurrences of fast solar wind streams during such periods. Moreover, the total number of storms occurring during the descending phase is greater than those observed during the ascending phase. The storms with peak Dst ≤ − 200 nT were classified as very intense and designated as outstanding Sun–Earth connections. It was found that 90% of such events occur around the peak phase of solar cycle. Therefore, it was concluded that the high-risk events occur during the peak phase of a solar cycle. Therefore, extreme care must be taken while launching new space missions and operating the existing ones, during this period.

Keywords

Solar cycle Geomagnetic storms Outstanding Sun–Earth connections 

PACS Nos.

90 94 

Notes

Acknowledgements

The author Malik A. Waheed is thankful to the University Grant Commission, New Delhi, for the financial support under Basic Scientific Research (BSR) Fellowship scheme. We are also thankful to National Geophysical Data Center (NGDC) and OMNI Web for making the data available free at its Web site.

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Copyright information

© Indian Association for the Cultivation of Science 2019

Authors and Affiliations

  • Malik A. Waheed
    • 1
  • Parvaiz A. Khan
    • 1
    Email author
  • A. K. Gwal
    • 2
  1. 1.Department of PhysicsIslamic University of Science and TechnologyAwantiporaIndia
  2. 2.AISECT UniversityBhopalIndia

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