What do Measurements of Abundance Variations Tell us About the Origin and Evolution of the Solar Wind

Connections between the Sun and solar wind have recently been made based on observations of density, velocity, and magnetic field. These have led to fundamental changes in our understanding of coronal magnetic topology and the origin and evolution of the solar wind. During solar minimum, polar coronal holes are neither the only regions of open magnetic field lines nor the sole source of fast solar wind. Instead, open magnetic field lines thread the entire corona, and solar wind flowing along them carries the imprint of coronal holes, quiet Sun, and active regions into interplanetary space. The purpose of this paper is to show how measurements of abundance variations in the corona and solar wind reinforce and complete this picture, providing key insight into where and how the solar wind, especially the slow wind, is produced.