Application of historic datasets to understanding open solar flux and the 20th-century grand solar maximum. 2. Solar observations
Application of historic datasets to understanding open solar flux and the 20th-century grand solar maximum. 2. Solar observations
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DOI：
10.3389/fspas.2022.976444
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发表时间：
2022-09
期刊：
影响因子：
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通讯作者：
M. Lockwood;M. Owens;S. Yardley;I. Virtanen;A. Yeates;A. Muñoz-Jaramillo
中科院分区：
文献类型：
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作者：
M. Lockwood;M. Owens;S. Yardley;I. Virtanen;A. Yeates;A. Muñoz-Jaramillo
我们研究了从20世纪上升到现代太阳极大期（MGSM）峰值的太阳活动的历史观测，并与此后发生的下降观测进行了比较。在现有的太阳观测的上升和下降的主要区别是准确的磁图从太阳磁图：我们在这里使用合成磁图来解释上升，并采用历史观测的极冠细丝，以测试它们，并验证它们的使用。我们表明，在太阳黑子极小期的日食图像揭示了从论文1（洛克伍德等人，2022年）。我们还利用来自历史上的极性光斑的白色光图像的极冕洞流量，但必须考虑的事实，这些光斑图像不告诉我们的极性领域的影响。考虑到这一点，极冕洞通量与基于太阳黑子数的开放通量连续性模型得出的值之间的一致性非常好。这种比较表明，一个可能的解决方案，“开放的通量问题”是开放的流光带内的通量，从光球场的日冕场的基于潜力的建模是没有捕捉。我们采取一个详细的看看在MGSM，周期19的峰值太阳周期，并显示极冕洞通量的变化和推断的向极通量浪涌是可预测的通量出现在两个半球的不对称性隐含transequatorial通量转移和/或“反黑尔”（或更一般的“流氓”活动区通量）出现在太阳黑子周期的后期。
We study historic observations of solar activity from the 20th-century rise towards the peak of the Modern Grand Solar Maximum (MGSM) and compare with observations of the decline that has occurred since. The major difference in available solar observations of the rise and of the fall are accurate magnetograms from solar magnetographs: we here use synthetic magnetograms to interpret the rise and employ historic observations of Polar Crown Filaments to test them and verify their use. We show that eclipse images at sunspot minimum reveal the long-term variation of open flux deduced from geomagnetic observations in Paper 1 (Lockwood et al., 2022). We also make use of polar coronal hole fluxes derived from historic white light images of polar faculae, but have to consider the implications of the fact that these facular images do not tell us the polarity of the field. Given this caveat, the agreement between the polar coronal hole fluxes and the values derived from open flux continuity modelling based on sunspot numbers is extremely good. This comparison indicates that one possible solution to the “open flux problem” is open flux within the streamer belt that potential-based modelling of coronal fields from photospheric fields is not capturing. We take a detailed look at the solar cycle at the peak of the MGSM, cycle 19, and show the variation of the polar coronal hole fluxes and the inferred poleward flux surges are predictable from the asymmetries in flux emergence in the two hemispheres with implied transequatorial flux transfer and/or “anti-Hale” (or more general “rogue” active region flux) emergence late in the sunspot cycle.