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.

这封信充分利用了 2006 年至 2020 年间在白光、Fe xi 789.2 nm ( T _fexi = 1.2 0.1 MK) 和 Fe xiv 530.3 nm ( T _fexiv = 1.8 0.1 MK) 发射中获得的一组独特的日全食观测结果来自 Advanced Composition Explorer/SWEPAM-SWICS 的原位 Fe 电荷状态和质子速度测量，以识别不同太阳风流的源区域。日食观测揭示了普遍存在的开放结构总是与Fe ^{10+ 的}Fe xi发射相关，因此电子温度恒定，T _c = T _fexi ，在不断扩大的日冕中。发现原位 Fe 电荷态聚集在 Fe ¹⁰⁺周围，独立于 300-700 km s ^-1流速度，称为连续太阳风。因此，Fe ¹⁰⁺产生了持续的太阳风与其在太阳上的T _fexi源之间的基准链接。虽然与流光相关的Fe ¹³⁺的 Fe xiv发射的空间分布在整个太阳周期中发生变化，但原位的零星电荷状态> Fe ¹¹⁺不表现出循环依赖性，无论速度如何。据推测，后面的这些流是从温度≥ T _{fexiv 的}热日冕等离子体中释放出来的 由与它们磁连接的日珥的动态行为驱动，在流光的隆起内和活动区域内。在不断扩大的日冕中以相同的T _fexi为特征的缓慢、中速和快速太阳风的连续流的发现对塑造太阳风的物理过程提出了新的限制。