Magnetic evolution of complex solar active regions
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arXiv
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| Format: | Preprint |
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2025
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| _version_ | 1866908382000054272 |
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| author | Nikbakhsh, Shabnam Tanskanen, Eija I. Hackman, Thomas |
| author_facet | Nikbakhsh, Shabnam Tanskanen, Eija I. Hackman, Thomas |
| contents | Aims. This study investigates the magnetic evolution of solar active regions (ARs), with a particular focus on understanding how the magnetic morphology of simple and complex ARs changes throughout their lifetime. Methods. To analyse the magnetic evolution of ARs, we developed a Magnetic Evolution Method (MEM) that segments each region's lifetime into three phases: growth, main, and recovery. The method was applied to ARs observed between January 1996 and December 2020. Results. We found that complex active regions (CARs) have a mean lifetime of approximately 24 days, which is 8 days longer than that of simple active regions (SARs). Most CARs (94%) first appear with a simple magnetic structure and remain in this configuration for about 3 days (growth phase), before transitioning into complex structures for around 5 days (main phase), after which they typically revert to a simple state (recovery phase). The average lifetimes of SARs and CARs show no significant difference between solar cycles 23 and 24, suggesting that active region lifetimes are independent of the solar cycle. Conclusions. By tracking the full magnetic evolution of ARs, our study reveals that CARs typically become magnetically complex around three days after emergence and remain in that state for a limited but critical period. This temporal structure, uncovered using a novel method that follows ARs throughout their full development, provides important context for identifying the magnetic conditions associated with increased eruptive potential. The results offer a foundation for improving the forecasting of solar flares and magnetic clouds, and suggest that the magnetic evolution of ARs is largely independent of the solar cycle. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2505_21759 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Magnetic evolution of complex solar active regions Nikbakhsh, Shabnam Tanskanen, Eija I. Hackman, Thomas Solar and Stellar Astrophysics Aims. This study investigates the magnetic evolution of solar active regions (ARs), with a particular focus on understanding how the magnetic morphology of simple and complex ARs changes throughout their lifetime. Methods. To analyse the magnetic evolution of ARs, we developed a Magnetic Evolution Method (MEM) that segments each region's lifetime into three phases: growth, main, and recovery. The method was applied to ARs observed between January 1996 and December 2020. Results. We found that complex active regions (CARs) have a mean lifetime of approximately 24 days, which is 8 days longer than that of simple active regions (SARs). Most CARs (94%) first appear with a simple magnetic structure and remain in this configuration for about 3 days (growth phase), before transitioning into complex structures for around 5 days (main phase), after which they typically revert to a simple state (recovery phase). The average lifetimes of SARs and CARs show no significant difference between solar cycles 23 and 24, suggesting that active region lifetimes are independent of the solar cycle. Conclusions. By tracking the full magnetic evolution of ARs, our study reveals that CARs typically become magnetically complex around three days after emergence and remain in that state for a limited but critical period. This temporal structure, uncovered using a novel method that follows ARs throughout their full development, provides important context for identifying the magnetic conditions associated with increased eruptive potential. The results offer a foundation for improving the forecasting of solar flares and magnetic clouds, and suggest that the magnetic evolution of ARs is largely independent of the solar cycle. |
| title | Magnetic evolution of complex solar active regions |
| topic | Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2505.21759 |