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Understanding the long-term evolution of green line coronal emission and its relation to the sunspots

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Abstract

Significant association between flux emergence and the complexity of the involved processes in the solar corona could be substantial in estimating magnetic field activities and related driving mechanisms. In this study, we analysed solar magnetic activity in the time period between 1939 and 2022, covering solar cycles 17 to the present cycle 25. Our study was principally based on green coronal intensity, which was calculated using observations collected from a global network of coronal stations. Specifically, we utilized the homogenized Fe XIV 530.3 nm coronal emission line provided by the Astronomical Institute of the Slovak Academy of Sciences, as well as of the International Sunspot number index. The analyses were carried out using the Cross-Correlation and Empirical Mode Decomposition techniques. Firstly, the study found that there are strong and positive correlations between the two indices, with high coefficients specifically during the examined solar cycles. Secondly, the empirical mode decomposition technique reveals unique properties of the intrinsic mode functions (IMFs), highlighting distinctions between the emergence of sunspots and green coronal emissions based on their various modulations. Indeed, these IMFs are most likely closely linked to the magnetic flux rope structure and indirectly connected with the emergence of sunspot events. The observed lag between MCI and the SSN could potentially be linked to the dynamics between coronal response time and the evolutions of active regions. Furthermore, there is a steady decrease observed in the green coronal index from solar cycle 17 to the current cycle 25 that could be attributed to waning behaviour of solar magnetic field strength. This decline can also be regarded as evidence of the Centennial Gleissberg solar activity cycle during the descending phase. Interestingly, the green coronal index exhibits a significant degree of phase synchronization with sunspot numbers, suggesting that the intricate relationship between green coronal intensity and sunspot numbers can be potentially driven by processes such as heating, the formation of active coronal regions, and the emergence of magnetic flux.

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Notes

  1. https://www.kozmos-online.sk/slnko/modifikovany-koronalny-index-modified-coronal-index/.

  2. http://sidc.be/silso/datafiles/.

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Acknowledgements

We would like to express our gratitude to the providers of data used; Astronomical Institute, Slovak Academy of Sciences for the Modified Coronal Index and the Sunspot Index and Long-term Solar Observations for the Sunspot data.

Funding

This study is supported by the National Natural Science Foundation of China (NSFC 12373063,11533009) and the 25-cm Coronagraph Development Project. The research work of A. Elmhamdi in this project was supported by King Saud University, Deanship of Scientific Research, College of Science Research Center. This work also received support from “Yunnan Revitalization Talent Support Program” Innovation Team Project (202405AS350012), and the Yunnan Fundamental Research Projects (grant No. 202301AV070007).

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Authors and Affiliations

  1. School of Physical Science and Technology, Southwest Jiaotong University, 999, **’an Road, Pidu District, Chengdu, 611756, Sichuan, China

    Jacob Oloketuyi, Yu Liu & Fengrong Zhu

  2. Department of Physics, Bamidele Olumilua University of Education, Science and Technology, Ikere-Ekiti City, P.O. Box 250, Ekiti State, Nigeria

    Jacob Oloketuyi

  3. Department of Physics and Astronomy, King Saud University, 11451, Riyadh, Saudi Arabia

    Abouazza Elmhamdi

  4. School of Mathematics and Computer Science, Yunnan Minzu University, Kunming, 650504, Yunnan, China

    Linhua Deng

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  1. Jacob Oloketuyi
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Oloketuyi, J., Liu, Y., Elmhamdi, A. et al. Understanding the long-term evolution of green line coronal emission and its relation to the sunspots. Astrophys Space Sci 369, 35 (2024). https://doi.org/10.1007/s10509-024-04300-y

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