Thermal and Density Structure of Polar Plumes

Details Thermal and Density Structure of Polar Plumes Thermal and Density Structure of Polar Plumes

Dec 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993soph..148..239w&link_type=abstract

Solar Physics, Volume 148, Issue 2, pp.239-252

Physics

36

Scientific paper

Normal incidence multilayer coated EUV/XUV optical systems provide a powerful technique for the study of the structure of the solar corona. Such systems permit the imaging of the full solar disk and corona with high angular resolution in narrow wavelength bands that are dominated by a single line or a line multiplet excited over a well defined range of temperatures. We have photometrically analysed, and derived temperature and density information from, images of polar plumes obtained with a multilayer Cassegrain telescope operating in the wavelength interval λ = 171 to 175 Å, which is dominated by Fe IX and Fe X emission. This observation was obtained in October 1987, and is the first high resolution observation of an astronomical object obtained with normal incidence multilayer optics techniques. We find that photometric data taken from this observation, applied to a simple, semi-empirical model of supersonic solar wind flow, are consistent with the idea that polar plumes are a source of the solar wind. However, we are not able to uniquely trace high speed streams to polar plumes. The temperatures that we observed are typically ˜ 1 500 000 K for both the plumes and the interplume regions, with the plume temperatures slightly higher than those of the surrounding atmosphere. Typical electron densities of the plume and interplume regions, respectively, are 5 × 109 cm-3 and 1 × 108 cm-3 at the limb of the Sun.

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