The continuum of the extreme limb and the chromosphere at the 1970 eclipse
β Scribed by H. Kurokawa; K. Nakayama; T. Tsubaki; M. Kanno
- Publisher
- Springer
- Year
- 1974
- Tongue
- English
- Weight
- 970 KB
- Volume
- 36
- Category
- Article
- ISSN
- 0038-0938
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β¦ Synopsis
The flash spectra of the partial Sun and the chromosphere were obtained at the total solar eclipse on 7 March, 1970. We studied the distributions of the surface brightness of the continuum at six wavelengths in the visual region to compare them with the previous observations and the existing model atmospheres. All of the distributions show a shallow dip and a small hump similar to those of Heintze's observation at the 1954 eclipse. But the hump in our results is of quite a different type from that given by Heintze's revised model. It was found that none of the existing model atmospheres can reproduce this hump. The intensity distribution in the low chromosphere was also examined.
π SIMILAR VOLUMES
Spectrographic observations of the flash spectrum were made by the Kwasan Observatory at the total solar eclipse on 7 March, 1970. The integrated intensities of Fexiv ,~ 5303, Fex ~ 6374, and the continuum were measured on the spectrograms as a function of height above the Sun's limb. It was found t
Photoelectric observations of the light intensity from the solar crescent before and after totality were made during the eclipses of 7 March, 1970 and 26 February, 1979. Effective wavelengths were determined by interference filters of 20 nm bandwidth. To obtain the limb darkening function, the resul
Observations are reported of an Ha filament clearly visible in the image of the chromosphere at the limb as well as in the Hc~ spectrum of the same part of the chromosphere. Observations of this kind may give valuable information about the absorption mechanism at work in filaments.
The intensity variation at the sun's limb has been studied in order to derive the gradient of the temperature in the low chromosphere. Eclipse observations show that in the continuum the height gradients of the total intensity vary systematically with wavelength; the observed gradient in the red is