Some consequences of nonuniformity of solar wind velocity

Parker [1960] has derived the magnetic field configuration in interplanetary space that would result from a steady solar wind flowing radially with uniform velocity from all heliolongitudes. Ahluwalia and Dessler [1962] have pointed out that the Archimedes spiral formed by the field lines would corotate with the sun even though the plasma moves radially. In this note we examine conditions in interplanetary space along the solar equatorial plane that are likely to arise when the radial velocity of the solar wind is a function of solar longitude, a most likely possibility judging by localized zones of enhanced coronal temperatures and intensity of 5303°λ which are observed on the sun. Moreover, we consider some broad consequences of the growth and decay of regions of activity and enhanced wind velocity as a function of time.