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<p>Each solar cycle (SC) is divided into four phases: solar minimum, ascending phase, solar maximum, and descending phase. For SCs 21 – 24, a total of 237 solar proton events (SPEs) were recorded and categorized by peak flux as follows: weak (10 pfu ≤ peak flux &lt; 100&#xa0;pfu; 126 events, 53.2%), moderate (100 pfu ≤ peak flux &lt; 1000&#xa0;pfu; 68 events, 28.7%), and strong (peak flux ≥ 1000 pfu; 43 events, 18.1%). The phase distribution of the 237 SPEs is as follows: 3.4% during solar minimum, 23.6% during ascending phase, 38.4% during solar maximum and 34.6% during descending phase. Statistical distributions of SPEs of different intensities across four phases are as follows: weak SPEs concentrate at solar maximum (41.3%), with the rest spread over the ascending (26.1%), descending (29.4%) and minimum (3.2%) phases. Moderate SPEs instead peak during the descending phase (39.7%), followed by solar maximum (33.8%), ascending (20.6%) and minimum (5.9%). Strong SPEs reached their highest fraction in the descending phase (41.9%), then solar maximum (37.2%) and ascending (20.9%); no strong events were recorded at minimum. We find a clear, universal pattern: the phase-resolved occurrence rates of weak, moderate and strong SPEs all migrate from one cycle to the next. Despite SC 21 having the largest smoothed monthly sunspot numbers among SCs 21 – 24, it produced no strong SPEs during its solar maximum.; the most intense SPEs of SCs 22 – 23 occurred during solar maximum, whereas the strongest SPEs of SCs 21 and 24 appeared in the descending and ascending phases, respectively. Peak fluxes of the SPEs in SCs 22 – 23 markedly surpassed those in SCs 21and 24, with SC 21 registering the weakest strong SPE.</p>

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Statistical Properties and Solar Cycle Distribution of Solar Proton Events Across Three Intensity Classes

  • 期刊论文

  • 发表日期：

    2026年4月13日

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  • Qi Li,
  • Gui-Ming Le

摘要

Each solar cycle (SC) is divided into four phases: solar minimum, ascending phase, solar maximum, and descending phase. For SCs 21 – 24, a total of 237 solar proton events (SPEs) were recorded and categorized by peak flux as follows: weak (10 pfu ≤ peak flux < 100 pfu; 126 events, 53.2%), moderate (100 pfu ≤ peak flux < 1000 pfu; 68 events, 28.7%), and strong (peak flux ≥ 1000 pfu; 43 events, 18.1%). The phase distribution of the 237 SPEs is as follows: 3.4% during solar minimum, 23.6% during ascending phase, 38.4% during solar maximum and 34.6% during descending phase. Statistical distributions of SPEs of different intensities across four phases are as follows: weak SPEs concentrate at solar maximum (41.3%), with the rest spread over the ascending (26.1%), descending (29.4%) and minimum (3.2%) phases. Moderate SPEs instead peak during the descending phase (39.7%), followed by solar maximum (33.8%), ascending (20.6%) and minimum (5.9%). Strong SPEs reached their highest fraction in the descending phase (41.9%), then solar maximum (37.2%) and ascending (20.9%); no strong events were recorded at minimum. We find a clear, universal pattern: the phase-resolved occurrence rates of weak, moderate and strong SPEs all migrate from one cycle to the next. Despite SC 21 having the largest smoothed monthly sunspot numbers among SCs 21 – 24, it produced no strong SPEs during its solar maximum.; the most intense SPEs of SCs 22 – 23 occurred during solar maximum, whereas the strongest SPEs of SCs 21 and 24 appeared in the descending and ascending phases, respectively. Peak fluxes of the SPEs in SCs 22 – 23 markedly surpassed those in SCs 21and 24, with SC 21 registering the weakest strong SPE.