Johann Christoph M?ller’s Sunspot Observations in 1719???1720: Snapshots of the Immediate Aftermath of the Maunder Minimum
Johann Christoph M?ller’s Sunspot Observations in 1719???1720: Snapshots of the Immediate Aftermath of the Maunder Minimum
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约翰·克里斯托夫·穆勒 (Johann Christoph Möller) 1719???1720 年的太阳黑子观测：蒙德极小期之后的快照
DOI：
10.1007/s11207-021-01880-8
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发表时间：
2021
期刊：
影响因子：
2.8
通讯作者：
Imada Shinsuke
中科院分区：
文献类型：
--
作者：
Hayakawa Hisashi;Iju Tomoya;Kuroyanagi Chiaki;Carrasco V?ctor M. S.;Besser Bruno P.;Uneme Shoma;Imada Shinsuke
蒙德极小期(1645年 - 1715年)在过去四个世纪中记录的太阳周期振幅和太阳黑子位置分布方面是独一无二的；然而，直到1749年，人们对它的恢复和向规则太阳周期的过渡知之甚少，而且现有的重建在这里是不同的。这篇文章介绍了太阳周期−3的快照，包括约翰·克里斯托弗·米勒(以下简称 - )在1719年JCM 1720年对太阳黑子的观测。我们在圣彼得堡的俄罗斯国家图书馆手抄部鉴定了他的太阳黑子图画，并汇编了他的传记和观察专长。随后，我们分析了他的太阳黑子图，得出了观测到的太阳黑子的群数和位置。结果和与当代观测的对比分析表明，JCM报告了多达五个太阳黑子群，与塞巴斯蒂安·阿利舍尔的记录很好地吻合，但与约翰·罗斯特在现有数据库中的记录形成了鲜明对比。这些比较表明，与现有数据库中的理解不同，1719年 - 1720年记录的ROST极大的值可能代表了单个太阳黑子数，而不是太阳黑子群数。因此，JCM的群号构成了代表1719年 - 1720年太阳活动的可靠参考，并在蒙德极小值之后显示出相对中等的太阳周期幅度。此外，JCM的太阳黑子图提供了关于太阳黑子位置的非常详细的信息。我们的分析可以定位两个太阳半球中报告的太阳黑子群，而不是蒙德极小期的太阳黑子群，后者支持建议的太阳周期−4和−3之间的转换。
The Maunder Minimum (1645 – 1715) was unique in terms of solar-cycle amplitudes and sunspot-position distributions registered in the last four centuries; however, little is known for its recovery and transition to the regular solar cycles until 1749 and the existing reconstructions vary from one to another here. This article presents a snapshot of Solar Cycle −3 including sunspot observations by Johann Christoph Müller (hereafter, JCM) in 1719 – 1720. We identified his sunspot drawings in the manuscript department of the National Library of Russia in St. Petersburg and compiled his biographical profile and observational expertise. Subsequently, we analysed his sunspot drawings and derived the group number and positions of the observed sunspots. The results and comparative analyses with contemporary observations revealed that JCM reported up to five sunspot groups, corresponding well with Sebastian Alischer’s records but contrasting with Johann Rost’s records in the existing databases. These comparisons indicated that Rost’s extremely large values recorded in 1719 – 1720 probably represented individual sunspot numbers instead of sunspot group numbers, unlike the understanding in the existing databases. Accordingly, JCM’s group number forms a robust reference for representing the solar activity in 1719 – 1720 and exhibits relatively moderate solar cycle amplitude in the immediate aftermath of the Maunder Minimum. Moreover, JCM’s sunspot drawings provide significantly detailed information on sunspot positions. Our analyses could locate the reported sunspot groups in both solar hemispheres, unlike those in the Maunder Minimum, which support the suggested transition between Solar Cycles −4 and −3.