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Fine structure of a solar flare region at 3.7 and 11.1 cm wavelengths

โœ Scribed by M. R. Kundu; T. Velusamy; R. H. Becker

Publisher
Springer
Year
1974
Tongue
English
Weight
273 KB
Volume
34
Category
Article
ISSN
0038-0938

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โœฆ Synopsis

On June 9, 1973, a flare associated burst was observed with the NRAO 3-element interferometer at 3.7 and 11.1 cm wavelength. The burst was of 'gradual rise and fall' type. Comparing the fringe amplitudes at 3.7 cm to the visibility computed for model flare regions we found that the precursor data are best fitted by a region of 3" in size while at the time of the peak, the flare appears to have a size of 2". During the post-maximum phase a size of 5" is the best estimate. Similar computations have been done for 11.1 cm data. The peak brightness temperatures are 1.2 โ€ข 109 K and 1.65 โ€ข l0 s K at 3.7 and 11.1 cm respectively. Such high temperatures would imply that a significant fraction of the burst radiation has a non-thermal origin.

๐Ÿ“œ SIMILAR VOLUMES

Fine structure of a solar active region
Fine structure of a solar active region at 3.7 and 11.1 cm wavelengths
โœ M. R. Kundu; R. H. Becker; T. Velusamy ๐Ÿ“‚ Article ๐Ÿ“… 1974 ๐Ÿ› Springer ๐ŸŒ English โš– 698 KB

The three-element interferometer of the National Radio Astronomy Observatory was used to observe the Sun at 3.7 and 11.1 cm wavelengths during the period June 5-9, 1973. The baselines of the interferometer were 900, 1800 and 2700 meters, with maximum angular resolution of 3" at 3.7 and 9" at 11.1 cm

Radio interferometric observations of so
Radio interferometric observations of solar bursts at 3.7 and 11.1 cm wavelengths
โœ M. R. Kundu; P. E. Angerhofer ๐Ÿ“‚ Article ๐Ÿ“… 1979 ๐Ÿ› Springer ๐ŸŒ English โš– 219 KB

Several solar active regions were observed during the 1976 vernal equinox with the 3-element interferometer of the National Radio Astronomy Observatory. The element spacings for these observations were 600, 2100, and 2700 m, resulting in maximum angular resolutions of about 3 arc sec at 3.7 cm and 8