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Corotating Interaction Regions during Solar Cycle 24: A Study on Characteristics and Geoeffectiveness

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Abstract

Corotating interaction regions (CIRs) form in the interaction region between the solar-wind high-speed streams and slow streams, leading to compressed plasma and magnetic fields. Using solar-wind measurements upstream of Earth, we identified 290 CIRs encountered by Earth during January 2008 through December 2019 (Solar Cycle 24). The occurrence rate is the maximum during the solar-cycle descending phase (\(\approx 33\) year−1), followed by occurrences during solar minimum (\(\approx 24\) year−1), the ascending phase (\(\approx 22\) year−1), and solar maximum (\(\approx 11\) year−1). At 1 AU, CIRs are found to be large-scale interplanetary structures with an average (median) duration of \(\approx 26\) hours (\(\approx 24\) hours) and radial extent of \(\approx 0.31\) AU (\(\approx 0.27\) AU). CIRs are characterized by average (median) plasma density of \(\approx 29\) cm−3 (\(\approx 26\) cm−3), ram pressure of \(\approx 11\) nPa (\(\approx 9\) nPa), temperature of \(\approx 5\times 10^{5}\) K (\(\approx 4\times 10^{5}\) K), and magnetic-field magnitude of \(\approx 15\) nT (\(\approx 14\) nT). The CIR characteristic features exhibit no clear solar-cycle phase dependence. About 30% of the CIRs are found to be geoeffective, causing geomagnetic storms with the peak SYM-H \(\leq -50\) nT; 25% caused moderate storms (−50 nT ≥ SYM-H \(>-100\) nT), and 5% caused intense storms (SYM-H \(\leq -100\) nT). The geoeffectiveness is found to decrease with the decreasing solar flux. CIRs during equinoxes are found to be more geoeffective compared to those during solstices. On average, SYM-H is strongly associated with the CIR plasma characteristic parameters (anti-correlation coefficient \(r=-0.65\) to −0.89), while the association is weaker for the AE-index (\(r=0.41\) to 0.67).

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Data Availability

The solar-wind plasma and interplanetary magnetic-field data are collected from OMNIWeb (omniweb.gsfc.nasa.gov/). The solar coronal AIA images are taken from NASA’s Solar Dynamics Observatory (sdo.gsfc.nasa.gov/). The geomagnetic SYM-H and AE indices are obtained from the World Data Center for Geomagnetism, Kyoto, Japan (wdc.kugi.kyoto-u.ac.jp/). The \(F_{10.7}\) solar flux are obtained from the LASP Interactive Solar Irradiance Data Center (lasp.colorado.edu/lisird/).

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Acknowledgments

The work of R. Hajra is funded by the Science and Engineering Research Board (SERB, grant no. SB/S2/RJN-080/2018), a statutory body of the Department of Science and Technology (DST), Government of India through the Ramanujan Fellowship. We would like to thank the reviewer for extremely valuable suggestions that substantially improved the manuscript.

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  1. Indian Institute of Technology Indore, Simrol, Indore, 453552, India

    Rajkumar Hajra & Jibin V. Sunny

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Appendix

Table 3 presents a catalog of all CIRs identified from January 2008 through December 2019. The approximate start and end times are given as the day of the year. The table is available in the Electronic Supplementary Material.

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Hajra, R., Sunny, J.V. Corotating Interaction Regions during Solar Cycle 24: A Study on Characteristics and Geoeffectiveness. Sol Phys 297, 30 (2022). https://doi.org/10.1007/s11207-022-01962-1

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