Solar Wind Sources and Their Variations Over the Solar Cycle

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Catalog of large-scale solar wind phenomena during 1976–2000 (2009, background): “It is worthwhile to note that the SLOW plasma stream represents denser and colder solar wind than hot and rarefied high-velocity FAST stream [ 31 , 32].”
Slow Solar Wind: Observations and Modeling (2016, unknown): “…density, lower proton temperature, higher electron temperature, larger temporal variability, higher heavy ion ionization states and higher first ionization potential (FIP) bias in elemental abundances (e.g., review by Schwenn 2006; Geiss et al. 1995; von Steiger et al. 2000, and references within).”
Bulk properties of the slow and fast solar wind and interplanetary coronal mass ejections measured by Ulysses: Three polar orbits of observations (2009, background): “That the slow wind is cooler and more variable has been discussed in a number of studies [Bame et al., 1977; see review by Schwenn, 2006].”
DEPENDENCE OF SOLAR-WIND POWER SPECTRA ON THE DIRECTION OF THE LOCAL MEAN MAGNETIC FIELD (2009, background): “The ratio Tp/Te = 2 is a typical value in high-speed wind (Marsch 1991a; Schwenn 2006; Marsch 2006), however, here it is assumed for simplicity that Tp/Te = 1.”