Abstract
Slitless flash spectrograms in heights below 8000 km above the solar limb were obtained by the University of Kyoto Expedition at Atar, Mauritania. The integrated intensities of Fexiv λ5303, Fex λ6374, Fexi λ7892, and the continuum are measured as a function of height above the solar limb at eleven points (P.A. = 284–300°) around the third contact point. It is found that a significant amount of the emission in Fex λ6374 originates in chromospheric levels well below 8000 km. This implies that the interspicular region of the chromosphere is occupied by coronal material. The average values of the electron temperature and the electron density in the interspicular region are derived from the Fex λ6374 and the Fexi λ7892 intensities on the assumption of spherical symmetry: T e = 0.9–1.1 × 106 K and N e = 9–10 × 108 cm−3. The intensity variations of the coronal lines and the continuum with position angle are also studied. Strong correlations between Fexiv λ5303 and the continuum and between Fex λ6374 and Fexi λ7892 are found. From the Fex λ6374 intensities it is inferred that there is a density fluctuation in the innermost corona by at least a factor of two.
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Contributions from the Kwasan and Hida Observatories, University of Kyoto, No. 271.
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Hanaoka, Y., Kanno, M., Kurokawa, H. et al. The innermost corona observed at the 1973 June 30 eclipse. Sol Phys 106, 95–106 (1986). https://doi.org/10.1007/BF00161357
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DOI: https://doi.org/10.1007/BF00161357