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.

通量出现与日冕所涉及过程的复杂性之间的显着关联对于估计磁场活动和相关驱动机制可能具有重要意义。在这项研究中，我们分析了 1939 年至 2022 年期间的太阳磁活动，涵盖太阳周期 17 至当前周期 25。我们的研究主要基于绿色日冕强度，该强度是使用从全球日冕网络收集的观测数据计算得出的。站。具体来说，我们利用了斯洛伐克科学院天文研究所提供的均质 Fe XIV 530.3 nm 日冕发射线以及国际太阳黑子数指数。使用互相关和经验模态分解技术进行分析。首先，研究发现这两个指数之间存在很强的正相关性，特别是在所检查的太阳周期期间，系数很高。其次，经验模态分解技术揭示了本征模态函数（IMF）的独特性质，突出了太阳黑子的出现和基于其不同调制的绿色日冕发射之间的区别。事实上，这些IMF很可能与磁通绳结构密切相关，并与太阳黑子事件的出现间接相关。观察到的 MCI 和 SSN 之间的滞后可能与日冕响应时间和活动区域演化之间的动态有关。此外，从太阳周期 17 到当前周期 25，观察到绿色日冕指数稳步下降，这可能归因于太阳磁场强度的减弱行为。这种下降也可以被视为百年格莱斯堡太阳活动周期下降阶段的证据。有趣的是，绿色日冕指数与太阳黑子数量表现出显着程度的相位同步，这表明绿色日冕强度和太阳黑子数量之间的复杂关系可能是由加热、活跃日冕区域的形成以及太阳黑子的出现等过程驱动的。磁通量。