Identifying the Coronal Source Regions of Solar Wind Streams from Total Solar Eclipse Observations and in situ Measurements Extending over a Solar Cycle
Identifying the Coronal Source Regions of Solar Wind Streams from Total Solar Eclipse Observations and in situ Measurements Extending over a Solar Cycle
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DOI：
10.3847/2041-8213/abe775
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发表时间：
2021-03
期刊：
影响因子：
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通讯作者：
S. Habbal;M. Druckmüller;N. Alzate;A. Ding;Judd Johnson;P. Štarha;J. Hoderová;B. Boe;S. Constant
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文献类型：
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作者：
S. Habbal;M. Druckmüller;N. Alzate;A. Ding;Judd Johnson;P. Štarha;J. Hoderová;B. Boe;S. Constant
这封信利用了2006年至2020年期间在白色光Fe xi 789.2 nm下获得的一组独特的日全食观测结果（T fexi = 1.2 ± 0.1 MK），和Fe xiv 530.3 nm（T fexiv = 1.8 ± 0.1 MK）发射，并由Advanced Composition Explorer/SWEPAM进行原位Fe电荷状态和质子速度测量-SWICS用于确定不同太阳风气流的源区。日食观测揭示了无处不在的开放结构总是与Fe 10+的Fe xi发射，因此一个恒定的电子温度，Tc = T fexi，在不断扩大的日冕。原位的Fe电荷状态被发现聚集在Fe 10+周围，与300-700 km s−1的流速度无关，被称为连续太阳风。因此，Fe 10+产生了连续的太阳风和它在太阳的T fexi源之间的基准联系。虽然空间分布的Fe xiv发射从Fe 13+与流光的变化在整个太阳周期，零星出现的电荷状态> Fe 11+原位表现出没有周期依赖性，无论速度。这些后者流被证明是从热日冕等离子体中释放出来的，温度≥T fexiv，在流的凸起和活动区域内，由与它们磁性相连的磁共振的动力学行为驱动。在不断膨胀的日冕中发现了以相同的T fexi为特征的连续的慢、中、快太阳风流，这对形成太阳风的物理过程提出了新的限制。
This letter capitalizes on a unique set of total solar eclipse observations acquired between 2006 and 2020 in white light, Fe xi 789.2 nm (T fexi = 1.2 ± 0.1 MK), and Fe xiv 530.3 nm (T fexiv = 1.8 ± 0.1 MK) emission complemented by in situ Fe charge state and proton speed measurements from Advanced Composition Explorer/SWEPAM-SWICS to identify the source regions of different solar wind streams. The eclipse observations reveal the ubiquity of open structures invariably associated with Fe xi emission from Fe10+ and hence a constant electron temperature, T c = T fexi, in the expanding corona. The in situ Fe charge states are found to cluster around Fe10+, independently of the 300–700 km s−1 stream speeds, referred to as the continual solar wind. Thus, Fe10+ yields the fiducial link between the continual solar wind and its T fexi sources at the Sun. While the spatial distribution of Fe xiv emission from Fe13+ associated with streamers changes throughout the solar cycle, the sporadic appearance of charge states >Fe11+ in situ exhibits no cycle dependence regardless of speed. These latter streams are conjectured to be released from hot coronal plasmas at temperatures ≥T fexiv within the bulge of streamers and from active regions, driven by the dynamic behavior of prominences magnetically linked to them. The discovery of continual streams of slow, intermediate, and fast solar wind characterized by the same T fexi in the expanding corona places new constraints on the physical processes shaping the solar wind.