Some physical processes in the solar wind

The ‘standard physics’ of the solar wind is reviewed, and arguments that this standard physics is inadequate are summarized. A variety of suggestions for modifying the physics of the solar wind are then reviewed, with emphasis on effects of MHD waves of solar origin and collisionless or instability‐limited electron heat conduction. The basic effects of the modified physics are demonstrated in a two‐fluid model of the solar wind flow. The predictions of this model are carefully compared with observations, and the need for further observations is emphasized. The review concludes with suggestions for future theoretical efforts.