HR: 0830h
AN: SH41B-0470    [PDF]
TI: What do Measurements of Abundance Variations Tell us About the Origin and Evolution of the Solar Wind
AU: * Woo, R
EM: richard.woo@jpl.nasa.gov
AF: Jet Propulsion Laboratory, 4800 Oak Grove Drive MS 238-725, Pasadena, CA 91109 United States
AU: Habbal, S R
EM: sdh@aber.ac.uk
AF: University of Wales at Aberystwyth, Department of Physics, Aberystwyth, SY23 3BZ United Kingdom
AU: Habbal, S R
EM: sdh@aber.ac.uk
AF: Harvard Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 United States
AU: Feldman, U
EM: uri.feldman@nrl.navy.mil
AF: Artep Inc., 2922 Excelsior Springs Ct., Ellicott City, MD 21042 United States
AU: Feldman, U
EM: uri.feldman@nrl.navy.mil
AF: E.O. Hulbert Center for Space Research, Naval Research Laboratory, Washington, DC 20375 United States
AB: 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.
DE: 2164 Solar wind plasma
DE: 2169 Sources of the solar wind
DE: 7509 Corona
DE: 7524 Magnetic fields
DE: 7538 Solar irradiance
SC: SPA - Solar and Heliospheric Physics [SH]
MN: 2003 Fall Meeting