Towards a Physical Characterization of Large Coronal Holes

Details Towards a Physical Characterization of Large Coronal Holes Towards a Physical Characterization of Large Coronal Holes

May 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004aas...204.7106m&link_type=abstract

American Astronomical Society Meeting 204, #71.06; Bulletin of the American Astronomical Society, Vol. 36, p.797

Astronomy and Astrophysics

Astrophysics

Scientific paper

The Ultraviolet Coronagraph Spectrometer (UVCS) aboard SOHO was used to observe O VI (103.2 and 103.7 nm) and H I Lyman alpha (121.6 nm) emission lines as a function of heliocentric distance in more than 85 coronal holes, in order to characterize the physical properties of coronal holes at different phases of the solar cycle. Our previous analyses of UVCS observations have shown that polar and equatorial coronal holes produce different acceleration profiles and have different oxygen kinetic temperatures. We examine the variation in the characteristics of representative large coronal holes producing a variety of high-speed conditions at 1 AU.
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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