Properties of the Solar Corona Outside the West Solar Limb

Details Properties of the Solar Corona Outside the West Solar Limb Properties of the Solar Corona Outside the West Solar Limb

May 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agusmsp21b..08d&link_type=abstract

American Geophysical Union, Spring Meeting 2005, abstract #SP21B-08

Physics

7509 Corona, 7549 Ultraviolet Emissions

Scientific paper

We discuss the analysis of 36 spectral observations recorded by the SUMER spectrometer on SOHO on April 22-23, 1998, at the onset of the new solar cycle. The observations were made with the 4" x 300" slit, and are distributed over the west hemisphere between 1.02 and 1.5 solar radii along the equatorial direction and between -0.9 solar radii south of the equator and +0.9 solar radii north of it. At the far corners of the studied region the solar distance was 1.74 solar radii. We have found that the physical characteristics of the central part of the region are typical of quiet Sun coronal plasmas. The regions furthest from the equator resemble coronal hole plasmas and the intermediate regions are consistent with a transition between the two. We believe that this is the most comprehensive work of its kind undertaken thus far using UV spectral lines. We use the recorded line intensities and line shapes to describe, as a function of coronal position, electron temperatures, electron densities, elemental abundances, line-of-sight emission measures (EM), nonthermal mass motions, and mass dependent elemental settling. By using intensity ratios between the two component resonance lines of Li-like O VI, Ne VIII and Mg X, we determine the fractional excitation in the Li-like lines produced by electron collisions and the fractional excitation produced by photo-excitation of transition region radiation emitted just above the photosphere.

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