On the coronal lines in the chromosphere at the 1970 eclipse

Abstract

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 that a large amount of emission in the coronal lines originates in the interspicular regions of the chromosphere. Analysis of the data yielded that the interspicular regions consist of coronal material of Te= 1.6 x 106-1.2 x 106 and log Ne=8.5-9.5, and that a decrease in T, and an increase in N~ occur with decreasing height.

The innermost corona observed at the 1973 June 30 eclipse

“…Athay and Roberts (1955), analyzing the slitless spectra of FexI 27892 obtained at the 1952 eclipse, were able to show that coronal temperature extended far below 10 000 km. This conclusion has been strengthened by Weart (1968) and by Kanno et aL (1971) from eclipse data of Fexlv 25303 and Fex 26374 in both cases, who agree in placing the base of the corona much below 10000 kin.…”

The coronal condensation observed at the 1973 eclipse

“…The outline of our program and preliminary results have been described by Kanno (1973) and Kanno et al (1974a). Only the essential aspects related to the flash spectrograms on which this investigation is based are summerized as follows.…”

Comments on the paper ?on the reliability of the structure of the low corona as derived from flash spectra? by R. Giovanelli

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In spite of the ambiguity in analyzing the eclipse flash spectrum, pointed out by Giovanelli (1975), the general conclusion of Kanno et al (1971) is shown to be still valid.

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