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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 ($\rm T_{fexi}$= $1.2 \pm 0.1$ MK) and Fe XIV 530.3 nm ($\rm T_{fexiv}$ = $ 1.8 \pm 0.1$ MK)emission, complemented by in situ Fe charge state and proton speed measurementsfrom ACE/SWEPAM-SWICS, to identify the source regions of different solar windstreams. The eclipse observations reveal the ubiquity of open structures,invariably associated with Fe XI emission from $\rm Fe^{10+}$, hence a constantelectron temperature, $\rm T_{c}$ = $\rm T_{fexi}$, in the expanding corona.The in situ Fe charge states are found to cluster around $\rm Fe^{10+}$,independently of the 300 to 700 km $\rm s^{-1}$ stream speeds, referred to asthe continual solar wind. $\rm Fe^{10+}$ thus yields the fiducial link betweenthe continual solar wind and its $\rm T_{fexi}$ sources at the Sun. While thespatial distribution of Fe XIV emission, from $\rm Fe^{13+}$, associated withstreamers, changes throughout the solar cycle, the sporadic appearance ofcharge states $> \rm Fe^{11+}$, in situ, exhibits no cycle dependenceregardless of speed. These latter streams are conjectured to be released fromhot coronal plasmas at temperatures $\ge \rm T_{fexiv}$ within the bulge ofstreamers and from active regions, driven by the dynamic behavior ofprominences magnetically linked to them. The discovery of continual streams ofslow, intermediate and fast solar wind, characterized by the same $\rmT_{fexi}$ in the expanding corona, places new constraints on the physicalprocesses shaping the solar wind.

the astrophysical journal. letters

Identifying the Coronal Source Regions of Solar Wind Streams from Total  Solar Eclipse Observations and in situ Measurements Extending Over a Solar  Cycle