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Fig. 2

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Alfvén wave-turbulence-based solar wind models incorporating effects of field line shape. Radial profiles are shown for a) the solar wind speed v, and b) the electron and proton temperatures Te and Tp. The curved (straight) case in which the field line shape is considered (neglected) is given by the solid (dashed) lines. In a), the asterisks indicate the sonic point where v equals the effective sonic speed cS defined by Eq. (6), while the vertical bars represent wind speeds measured by tracking small density inhomogeneities (blobs) in SOHO/LASCO images as given by Wang et al. (2000). The triangles in b) give the hydrogen kinetic temperatures derived from H I Lyα measurements with SOHO/UVCS for a typical solar minimum streamer (Strachan et al. 2002).

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