Abstract
Abstract The digitized images of 350 eclipse chromospheric spectra obtained with a special automatic photometer have been used to construct the image of the D 3 He I chromosphere over the range of 36°N–42°S in latitude. The chromospheric emission comes from two very irregular bands with peaks of intensities at heights of 1100–1700 km for the bands with the dominant emission, and at a height of around 300 km for the lower bands. The distribution of the surface brightness averaged over all measured latitudes (36°N–42°S) versus height also reveals two peaks. The energy emitted by the upper layer is determined to be seven times larger than that emitted by the lower one. The chromospheric D 3 emission is well correlated with the emission of the green corona (503.3 nm) at low heights. The correlation disappears at heights of more than 1500 km. The chromosphere above active regions and spots is lower. It is supposed that such behavior is caused by large-scale magnetic fields of the Sun and by structural elements, such as spicules and fibrils.
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