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Fine structure of a very bright active region at a wavelength of 2.8 cm

โœ Scribed by M. Felli; P. Pampaloni; G. Tofani

Publisher
Springer
Year
1974
Tongue
English
Weight
488 KB
Volume
37
Category
Article
ISSN
0038-0938

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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

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

The structure and intensity evolution of
The structure and intensity evolution of a solar burst at 2.8 cm and the relation with the soft X-ray emitting region
โœ Marcello Felli; Roberto Pallavicini; Gianni Tofani ๐Ÿ“‚ Article ๐Ÿ“… 1975 ๐Ÿ› Springer ๐ŸŒ English โš– 696 KB

The decay phase of a microwave burst was observed with a one-dimensional angular resolution of 16" at 2.8 cm. The structure was found to be composed of several bursting regions with different evolution. The event was also observed in soft X-rays by full-disk detectors. The joint analysis of these da