UVCS Observations of Slow Plasma Flow in the Corona Above Active Regions

Details UVCS Observations of Slow Plasma Flow in the Corona Above Active Regions UVCS Observations of Slow Plasma Flow in the Corona Above Active Regions

May 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agusmsh31a..04w&link_type=abstract

American Geophysical Union, Spring Meeting 2005, abstract #SH31A-04

Physics

2164 Solar Wind Plasma, 2169 Sources Of The Solar Wind

Scientific paper

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.

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