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Because of its distinctive compositional properties and variability,low-speed ($\lesssim 450$ km s$^{-1}$) solar wind is widely believed tooriginate from coronal streamers, unlike high-speed wind, which comes fromcoronal holes. An alternative scenario is that the bulk of the slow wind(excluding that in the immediate vicinity of the heliospheric current sheet)originates from rapidly diverging flux tubes rooted inside small coronal holesor just within the boundaries of large holes. This viewpoint is based largelyon photospheric field extrapolations, which are subject to considerableuncertainties and do not include dynamical effects, making it difficult to becertain whether a source is located just inside or outside a hole boundary, orwhether a high-latitude hole will be connected to Earth. To minimize thedependence on field-line extrapolations, we have searched for cases whereequatorial coronal holes at central meridian are followed by low-speed streamsat Earth. We describe 14 examples from the period 2014--2017, involving Fe XIV21.1 nm coronal holes located near active regions and having equatorial widthsof $\sim$3$^\circ$--10$^\circ$. The associated in situ wind was characterizedby speeds $v\sim 300$--450 km s$^{-1}$ and by O$^{7+}$/O$^{6+}$ ratios of$\sim$0.05--0.15, with $v$ showing the usual correlation with protontemperature. In addition, consistent with other recent studies, this slow windhad remarkably high Alfv\'enicity, similar to that in high-speed streams. Weconclude that small coronal holes are a major contributor to the slow solarwind during the maximum and early post-maximum phases of the solar cycle.

Observations of Slow Solar Wind from Equatorial Coronal Holes