Empirical Models of Temperature, Densities, and Velocities in the Solar Corona

Details Empirical Models of Temperature, Densities, and Velocities in the Solar Corona Empirical Models of Temperature, Densities, and Velocities in the Solar Corona

Apr 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998eostr..79..278f&link_type=abstract

Eos Trans. AGU, 79(17), Spring Mtg. Suppl., S278

Computer Science

Solar Corona, Solar Wind

Scientific paper

We present empirical results for temperatures, densities, and outflow velocities of constituents of the solar corona from 1 to 3 Ro in polar coronal holes and an equatorial streamer. Data were obtained from a variety of space and ground-based instruments during August 1996 as part of the SOHO Whole Sun Month Campaign. From white light data obtained with the SOHO/LASCO/C2 and HAO/Mauna Loa coronagraphs, we determine electron densities and compare them to those determined from the density-sensitive EUV line ratio of Si IX 350/342 Angstroms observed by the SOHO/Coronal Diagnostic Spectrometer (CDS). Moreover, from the white light density profiles we calculate temperature profiles and compare to temperature diagnostic information from EUV lines and soft X-ray images from Yohkoh. H I Ly alpha and O VI 1032/1037 Angstrom intensities from the SOHO Ultraviolet Coronagraph Spectrometer (UVCS) are used to estimate both the direction and magnitude of plasma outflow velocities in coronal holes and streamers above 1.5 Ro. The velocities are derived using densities from white light coronagraph data and coronal electron temperature estimates derived from Ulysses/SWICS ion composition data. Near the base of the corona we find the white light and spectral analysis produce consistent density and temperature information. In the extended corona we find results consistent with high outflow velocities and a superradial outflow geometry in polar coronal holes.

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