Solar Cycle Dependence of Coronal Hole Properties

Details Solar Cycle Dependence of Coronal Hole Properties Solar Cycle Dependence of Coronal Hole Properties

Jul 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005iaga...10...79m&link_type=abstract

"10th IAGA Scientific Assembly, GAIV.01 Symposium "The Sun: Its interior, atmosphere and wind", Oral Presentation IAGA2005-A-01

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Scientific paper

The SOHO Ultraviolet Coronagraph Spectrometer (UVCS) has been used to measure the properties of hundreds of large coronal holes, that produced a variety of high-speed solar wind streams, during the past nine years. In the cases where UVCS and in situ measurements were made of the same coronal-hole plasma, high speeds in excess of 600 km/s were found in interplanetary space. UVCS has been 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. The analysis of their spectroscopic parameters allows us to identify similarities and differences among coronal holes at different phases of the solar cycle. From such measurements we can derive plasma parameters (densities, temperatures, velocity distribution anisotropies, and outflow speeds) for O5+ and protons as a function of heliocentric distance in the coronal holes. These properties, combined with other observed quantities such as white-light polarization brightness and the magnetic fluxes measured on-disk, let us analyze the coronal hole plasma properties more fully than ever before. We will present the solar cycle dependence of the above plasma parameters from the last solar minimum in 1996 to present and compare them, where possible, with the in situ solar wind properties.
This work is supported by NASA under Grant NNG04GE84G to the Smithsonian Astrophysical Observatory, by the Italian Space Agency, and by PRODEX (Swiss contribution).

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