The Radial and Angular Variation of Electron Density in the Solar Corona.

Details The Radial and Angular Variation of Electron Density in the Solar Corona. The Radial and Angular Variation of Electron Density in the Solar Corona.

Oct 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000spd....31.0234g&link_type=abstract

American Astronomical Society, SPD Meeting #31, #02.34; Bulletin of the American Astronomical Society, Vol. 32, p.1290

Astronomy and Astrophysics

Astronomy

Scientific paper

We derive, for the first time, electron densities as a function of both radius (R) and position angle (θ ) for the south-west quadrant of the off-limb corona, using the density-sensitive Si ix (349.9 Å/341.9 Å) and Si x (356.0 Å/347.7 Å) extreme ultraviolet line ratios. The observations were made with the Coronal Diagnostic Spectrometer (cds) on board the Solar and Heliospheric Observatory (soho), over the range 1.00R&sun; < R < 1.20R&sun; and 180° < θ < 270° . Within the south polar coronal hole, the density varies from 2.3 x 108 cm-3 at 1.0R&sun; to 8.3x 107 cm-3 at 1.20R&sun; , while at the equator the density varies from 6.3 x 108 cm-3 at 1.0R&sun; to 1.6x 108 cm-3 at 1.20R&sun; . The density falloff with height is therefore faster in the equatorial region. We also find that electron densities are, on average, a factor of 2.7 larger in the equatorial regions than in the polar coronal hole at a given radial distance. Finally, we find remarkable agreement between our measured densities as a function of radius and position angle and those predicted by a recent analytic MHD model of the solar wind, strongly supporting its basic premises.

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