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Fine structure and time variation of the quiet Sun at 1.3 cm

โœ Scribed by A. Pramesh Rao; M. R. Kundu

Publisher
Springer
Year
1978
Tongue
English
Weight
382 KB
Volume
59
Category
Article
ISSN
0038-0938

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๐Ÿ“œ SIMILAR VOLUMES

Fine structure of the Sun at 1.3 cm wave
Fine structure of the Sun at 1.3 cm wavelength
โœ M. R. Kundu; T. Velusamy ๐Ÿ“‚ Article ๐Ÿ“… 1974 ๐Ÿ› Springer ๐ŸŒ English โš– 308 KB

The two-element interferometer at Hat Creek Observatory was used at 1.3 cm wavelength to study the fine structure of the radio emissive regions on the Sun. Observations of the quiet Sun at 1.3 cm show sudden changes in the fringe amplitude and phase, lasting for typically about 5-8 min. Assuming tha

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

Fine structure of a solar flare region a
Fine structure of a solar flare region at 3.7 and 11.1 cm wavelengths
โœ M. R. Kundu; T. Velusamy; R. H. Becker ๐Ÿ“‚ Article ๐Ÿ“… 1974 ๐Ÿ› Springer ๐ŸŒ English โš– 273 KB

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 ar