  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 measurements
from ACE/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 $\rm Fe^{10+}$, hence a constant
electron 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 as
the continual solar wind. $\rm Fe^{10+}$ thus yields the fiducial link between
the continual solar wind and its $\rm T_{fexi}$ sources at the Sun. While the
spatial distribution of Fe XIV emission, from $\rm Fe^{13+}$, associated with
streamers, changes throughout the solar cycle, the sporadic appearance of
charge states $> \rm Fe^{11+}$, in situ, exhibits no cycle dependence
regardless of speed. These latter streams are conjectured to be released from
hot coronal plasmas at temperatures $\ge \rm T_{fexiv}$ 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 $\rm
T_{fexi}$ in the expanding corona, places new constraints on the physical
processes shaping the solar wind.
