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Distribution and recovery phase of geomagnetic storms during solar cycles 23 and 24

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dc.contributor.author Mishra, Wageesh
dc.contributor.author Sahani, Preity Sukla
dc.contributor.author Khuntia, Soumyaranjan
dc.contributor.author Chakrabarty, Dibyendu
dc.date.accessioned 2024-06-21T04:08:17Z
dc.date.available 2024-06-21T04:08:17Z
dc.date.issued 2024-05
dc.identifier.citation Monthly Notices of the Royal Astronomical Society, Vol. 530, No. 3, pp. 3171–3182 en_US
dc.identifier.issn 0035-8711
dc.identifier.uri http://hdl.handle.net/2248/8483
dc.description Open Access. en_US
dc.description This is an Open Access article distributed under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0/), which permits unrestricted reuse, distribution, and reproduction in any medium, provided the original work is properly cited.
dc.description.abstract Coronal mass ejections (CMEs) and Stream Interaction Regions (SIRs) are the main drivers of intense geomagnetic storms. We study the distribution of geomagnetic storms associated with different drivers during solar cycles 23 and 24 (1996–2019). Although the annual occurrence rate of geomagnetic storms in both cycles tracks the sunspot cycle, the second peak in storm activity lags the second sunspot peak. SIRs contribute significantly to the second peak in storm numbers in both cycles, particularly for moderate to stronger-than-moderate storms. We note semiannual peaks in storm numbers much closer to equinoxes for moderate storms, and slightly shifted from equinoxes for intense and stronger-than-intense storms. We note a significant fraction of multiple-peak storms in both cycles due to isolated ICMEs/SIRs, while single-peak storms from multiple interacting drivers, suggesting a complex relationship between storm steps and their drivers. Our study focuses on investigating the recovery phases of geomagnetic storms and examining their dependencies on variousstorm parameters. Multiple-peak storms in both cycles have recovery phase duration strongly influenced by slow and fast decay phases with no correlation with the main phase build-up rate and Dst peak. However, the recovery phase in single-peak storms for both cycles depends to some extent on the main phase build-up rate and Dst peak, in addition to slow and fast decay phases. Future research should explore recovery phases of single and multiple-peak storms incorporating in situ solar wind observations for a deeper understanding of storm evolution and decay processes. en_US
dc.language.iso en en_US
dc.publisher Oxford University Press on behalf of Royal Astronomical Society en_US
dc.relation.uri https://doi.org/10.1093/mnras/stae1045
dc.rights © 2024 The Author(s).
dc.subject Sun: coronal mass ejections (CMEs) en_US
dc.subject Sun: heliosphere en_US
dc.subject Sun: solar-terrestrial relations en_US
dc.title Distribution and recovery phase of geomagnetic storms during solar cycles 23 and 24 en_US
dc.type Article en_US


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