Abstract
Over a range of spatial scales, the onset regions of the fast solar wind are influenced or controlled by the structure of the local magnetic fields. This is demonstrated for the large scale structures that determine coronal holes, as well as for the supergranulation network. It is likely that reconnexion effects in small-scale emerging fields play a role in the initial accelerating mechanism. The role of magnetic fields in outflowing solar plumes is at present less clear.
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