HR: 09:15h
AN: SH31A-04    [Abstracts]
TI: UVCS Observations of Slow Plasma Flow in the Corona Above Active Regions
AU: * Woo, R
EM: richard.woo@jpl.nasa.gov
AF: Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, MS 238-725, Pasadena, CA 91109 United States
AU: Habbal, S R
EM: sdh@ifa.hawaii.edu
AF: Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822 United States
AB: The elusive source of slow solar wind has been the subject of ongoing discussion and debate. Observations of solar wind speed near the Earth orbit, first with IPS (interplanetary scintillation) and later with Ulysses in situ measurements, have suggested that some slow solar wind may be associated with active regions (Kojima & Kakinuma 1987; Woo, Habbal & Feldman 2004). The ability of SOHO UVCS Doppler dimming measurements to provide estimates of solar wind speed in the corona (Kohl et al. 1995) has made it possible to investigate the distribution of flow near the Sun. In this paper, we will present results confirming that active regions are one of the sources of slow wind. Insight into the relationship between coronal streamers, active regions and plasma flow will also be discussed.
DE: 2164 Solar wind plasma
DE: 2169 Sources of the solar wind
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2005 Joint Assembly