Fig. 5.
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Coronal hole expansion. Distribution of the expansion factors of magnetic field lines at the source surface (2.5 solar radii), traced from the coronal hole sections identified with dashed boxes in Figs. 1E and 3E. The gray curve is for the case of the fast wind, while the black curve is for the case of the Alfvénic slow wind. See Appendices C and D for details.
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