Structure and emission of the solar chromosphere in the helium D3 line from observations of total Solar eclipses

Details Structure and emission of the solar chromosphere in the helium D3 line from observations of total Solar eclipses Structure and emission of the solar chromosphere in the helium D3 line from observations of total Solar eclipses

Apr 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002kfnt...18..136a&link_type=abstract

Kinematika i Fizika Nebesnykh Tel, vol. 18, no. 2, p. 136-148

Physics

1

Scientific paper

Maps of the chromospheric emission in the helium D3 line as functions of heliographic latitude and height obtained from cinematographic observations of the total solar eclipses 1972 July 10 and 1981 July 31 are presented. The helium emission is found to be observed in separate features with a characteristic supergranule size of 20000-30000 km along the limb mainly. The features are concentrated at a height of about 1400 km but can be observed at heights up to 3000-4000 km. These are also present at the base of the chromosphere, and the height distribution of surface brightness reveals two peaks at heights of about 1400 and 250 km. The energy emitted by the chromosphere over the height range of the lower maximum is about 5% and 10% of the total energy emitted by the chromosphere in the D3 line for the eclipses of 1972 and 1981, respectively. It is found that the integral brightness of the quiet chromosphere for the eclipse of 1981 was twice that of the 1972 eclipse. This difference is connected with the fact that the eclipses occurred at different phases of sunspot cycle. It is shown that the helium emission at the height range of the temperature minimum in an the inhomogeneous chromosphere can be explained by the penetration of the coronal radiation with λ<6 nm to these heights.

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