Abstract

In our earlier work [2–4], we proposed using the coronal magnetic field as an implicit tracer when studying the properties of differential rotation of the solar corona. At present, this is virtually the only way to study the rotation of the Sun at large heliocentric distances up to the source surface. In the present work, calculations of the coronal magnetic field have been extended over a longer time interval, till December 31, 2015. It is shown that the solar corona rotates differentially at all heliocentric distances up to the source surface. The differential rotation gradient decreases with distance. As we approach the source surface, the corona rotation becomes more rigid, but even at large heliocentric distances it remains slightly differential. We believe that the differential rotation of the solar corona reflects the rotation of deep subphotospheric layers. In this case, the behavior of the coronal rotation characteristics can be used as indicator of differential rotation of the subphotospheric layers. We have compared the changes in the coronal rotation characteristics with distance with helioseismic data and obtained a satisfactory agreement. Cycle variations in the differential rotation of subphotospheric layers have been investigated for the first time.

中文翻译：

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太阳日冕作为亚光圈层旋转差的指示

摘要

在我们较早的工作中[2-4]，我们建议在研究日冕的差分旋转特性时使用日冕磁场作为隐式示踪剂。目前，这实际上是研究太阳在距源表面大太阳心距距离处旋转的唯一方法。在目前的工作中，日冕磁场的计算已扩展到一个较长的时间间隔，直到2015年12月31日。结果表明，日冕在所有日心距上都以不同的方式旋转，直至源表面。差分旋转梯度随距离减小。当我们接近源表面时，电晕旋转变得更加坚硬，但是即使在大的日心距下，电晕旋转仍会略有差异。我们相信，日冕的旋转差反映了深亚光层的旋转。在这种情况下，日冕旋转特性的行为可以用作亚光球层差旋转的指示。我们已经比较了日冕数据随距离的变化和日震数据，并获得了满意的结果。首次研究了亚光圈层差速旋转中的周期变化。