Density and temperature of quiescent solar prominences from observations in the radio range

Details Density and temperature of quiescent solar prominences from observations in the radio range Density and temperature of quiescent solar prominences from observations in the radio range

Oct 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985azh....62..992a&link_type=abstract

(Astronomicheskii Zhurnal, vol. 62, Sept.-Oct. 1985, p. 992-994) Soviet Astronomy (ISSN 0038-5301), vol. 29, Sept.-Oct. 1985, p.

Astronomy and Astrophysics

Astronomy

2

Brightness Temperature, Electron Density (Concentration), Solar Prominences, Solar Radio Emission, Wavelengths

Scientific paper

A decrease in the relative brightness temperature of a filament (prominence) with a decrease in size is observed at wavelengths of 0.4, 0.6, 0.8, and 0.85 cm, which can be explained by the dependence nT is approximately const. A comparison of the results of observations of the same filament at different wavelengths reveals a difference in the physical conditions (n, T) of the layers responsible for the emission at one wavelength or another.

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