Astronomy and Astrophysics – Astronomy
Scientific paper
Jun 1981
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981soph...71..311s&link_type=abstract
Solar Physics, vol. 71, June 1981, p. 311-328.
Astronomy and Astrophysics
Astronomy
13
H Alpha Line, Radio Astronomy, Solar Prominences, Solar Radio Emission, Lines Of Force, Radio Telescopes, Solar Limb, Solar Magnetic Field, Solar Oscillations, Solar Spectra, Spatial Distribution, Statistical Distributions
Scientific paper
Radio depressions frequently appear broader than their associated H-alpha filaments and often persist after a filament disappears. The reported study is concerned with the relative contributions of filament and the filament channel to the depth of radio depressions. Although the contribution cannot readily be determined in an individual case, the apportionment can be assessed statistically by extensive multi-frequency observations of many filaments and channels using the same telescope over a period of days. In principle it is possible to determine the evolution, geometry, and physical properties of filaments and filament channels with a widely based set of radio observations. It is found that all but a few percent of the microwave depressions lie on magnetic neutral lines or their natural extensions. The only possible exceptions are coronal holes on the disk, which are small or non-existent during the period of the conducted observations. The diversity of microwave filaments is striking. Even quiescent filaments show considerable variation.
Bobrowsky Matthew
Kundu Mukul R.
Schmahl Ed. J.
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