The three‐dimensional solar wind around solar maximum

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Solar Wind Helium Abundance as a Function of Speed and Heliographic Latitude: Variation through a Solar Cycle (2007, methodology): “The correlation between wind speed and heliographic latitude during solar minimum has been demonstrated using the first Ulysses fast latitude scan in 1994/1995 (McComas et al. 2003 and references therein).”
Weaker solar wind from the polar coronal holes and the whole Sun (2008, background): “... large (nearly factor of 2) variation from 1991 through 2001 was noted by Richardson et al. [2001], with the near ecliptic dynamic pressure again rising steeply just after solar maximum and then slowly decreasing over the rest of the SC. The Ulysses observations through 2002, however, did not sho”
The Heliospheric Magnetic Field (2013, methodology): “This solar wind structure was observed by Ulysses (McComas et al., 2003) and is shown in the right-hand column of Figure 4.”
The Solar Probe Plus Mission: Humanity’s First Visit to Our Star (2016, background): “A mixture of fast flows from smaller coronal holes and transients, embedded in a slow-to-moderate-speed wind, appears at all latitudes (e.g., McComas et al. 2003, Fig.”
Bulk properties of the slow and fast solar wind and interplanetary coronal mass ejections measured by Ulysses: Three polar orbits of observations (2009, background): “This orbit coincided with a period of rising and enhanced solar activity, including solar maximum [McComas et al., 2003].”