Solar Activity And Space Weather


Annual numbers of solar events relevant to space weather (X-class solar flares and fast CMEs) and space weather events (SEP events, geomagnetic storms) superposed on V2.0 SSN (grey, arbitrary scale) during SCs 21- 24. Large SEP events with >10 MeV proton intensity ≥10 pfu, and major geomagnetic storms (Dst ≤ – 100 nT), are included. The number of GOES X-class flares is divided by 2 to fit the scale. CME data are from the Solwind coronagraph (1979-1985), Solar Maximum Mission Coronagraph/Polarimeter (1985-1989), and SOHO/LASCO (1996-2019).

After providing an overview of solar activity as measured by the sunspot number (SSN) and space weather events during solar cycles (SCs) 21-24, we focus on the weak solar activity in SC 24.

The weak solar activity reduces the number of energetic eruptions from the Sun and hence the number of space weather events. The speeds of coronal mass ejections (CMEs), interplanetary (IP) shocks, and the background solar wind all declined in SC 24. One of the main heliospheric consequences of weak solar activity is the reduced total (magnetic + gas) pressure, magnetic field strength, and Alfvén speed.

There are three groups of phenomena that decline to different degrees in SC 24 relative to the corresponding ones in SC 23: (i) those that decline more than SSN does, (ii) those that decline like SSN, and (iii) those that decline less than SSN does. The decrease in the number of severe space weather events such as high-energy solar energetic particle (SEP) events and intense geomagnetic storms is deeper than the decline in SSN. CMEs expand anomalously and hence their magnetic content is diluted resulting in weaker geomagnetic storms. The reduction in the number of intense geomagnetic storms caused by corotating interaction regions is also drastic. The diminished heliospheric magnetic field in SC 24 reduces the efficiency of particle acceleration, resulting in fewer high-energy SEP events. The numbers of IP type II radio bursts, IP socks, and high-intensity energetic storm particle events closely follow the number of fast and wide CMEs (and approximately SSN).

The number of halo CMEs in SC 24 declines less than SSN does, mainly due to the weak heliospheric state. Phenomena such as IP CMEs and magnetic clouds related to frontside halos also do not decline significantly. The mild space weather is likely to continue in SC 25, whose strength has been predicted to be not too different from that of SC 24.

Nat Gopalswamy, Pertti Mäkelä, Seiji Yashiro, Sachiko Akiyama, Hong Xie

Comments: 16 pages, 10 figures, 3 tables, to appear in Journal of Physics: Conference Series, Proc. 2nd International Symposium on Space Science 2021, LAPAN, Indonesia
Subjects: Solar and Stellar Astrophysics (astro-ph.SR)
Cite as: arXiv:2201.02724 [astro-ph.SR] (or arXiv:2201.02724v1 [astro-ph.SR] for this version)
Submission history
From: Nat Gopalswamy
[v1] Sat, 8 Jan 2022 01:37:44 UTC (1,369 KB)
https://arxiv.org/abs/2201.02724

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