Differences in Plasma Conditions Among 85 Large Coronal Holes

Details Differences in Plasma Conditions Among 85 Large Coronal Holes Differences in Plasma Conditions Among 85 Large Coronal Holes

May 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004agusmsh41a..03m&link_type=abstract

American Geophysical Union, Spring Meeting 2004, abstract #SH41A-03

Astronomy and Astrophysics

Astrophysics

2164 Solar Wind Plasma, 2169 Sources Of The Solar Wind, 7511 Coronal Holes, 7536 Solar Activity Cycle (2162), 7549 Ultraviolet Emissions

Scientific paper

We have measured ultraviolet spectroscopic parameters as a function of heliocentric distance for more than 85 coronal holes, in order to characterize the physical properties of coronal holes at different phases of the solar cycle. The Ultraviolet Coronagraph Spectrometer (UVCS) aboard SOHO was used to observed O VI (103.2 and 103.7 nm) and H I Lyman alpha (121.6 nm) emission lines to determine kinetic temperatures, average densities, and outflow speeds in coronal holes. UVCS observations provide unique information on the heating and acceleration processes in the corona. Our previous analyses of UVCS observations have shown that solar minimum (polar) and solar maximum (equatorial) coronal holes produce different acceleration profiles and have different oxygen kinetic temperatures. We also examine the differences in the characteristics of representative coronal holes producing a variety of high-speed conditions (550-800 km/s) at 1 AU. These analyses provide limits on the coronal plasma properties and put constraints on the physical processes that are responsible for the heating of the extended corona and the acceleration of the solar wind. This work is supported by NASA under Grant NAG5-12865 to the Smithsonian Astrophysical Observatory, by the Italian Space Agency and by PRODEX (Swiss contribution).

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