Origins of the Solar Wind in the Corona

Abstract

Coronal holes are the most well-established coronal source of steady-state solar wind. Coronal mass ejections associated with flares and/or eruptive prominences are another clearly identified source of solar wind, a transient component that accounts for approximately 5% of the total solar mass loss. The role of other coronal structures in the generation of the solar wind is less clear. Streamers and the interfaces between streamers and other coronal regions are potential sources of low speed wind, a hypothesis consistent with existing observations. However, measurements of mass flows in these features are needed to confirm this. The necessary data can be obtained using recently developed remote sensing techniques, particularly if acquired in conjunction with Ulysses. Small-scale dynamical phenomena observed at the base of the corona (spicules, macrospicules and high speed jets) and small-scale structures observed in polar coronal holes (polar plumes) may or may not play a significant role in supplying mass, momentum and energy to the solar wind. New measurements are required to determine the role, if any, of small-scale structures in the generation of the solar wind.