Coronal Holes and Solar Wind High-Speed Streams: I. Forecasting the Solar Wind Parameters

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Rotating solar coronal holes and periodic modulation of the upper atmosphere (2008, background): “They are most prevalent at low solar latitudes during the declining phase of solar maximum and in solar minimum and are stable structures that can persist for many solar rotations [e.g., Borovsky and Denton, 2006; Vršnak et al., 2007].”
Space weather: the solar perspective (2021, methodology): “After a coronal hole passed the central part of the solar disk, in-situ measurements reveal about 1–2 days later an increase in the density and magnetic field, and about 3–4 days later in the plasma speed (Vršnak et al. 2007).”