Distribution of the Green- and Red-Line Coronal Emissions and Their Contribution to the K-Corona

Details Distribution of the Green- and Red-Line Coronal Emissions and Their Contribution to the K-Corona Distribution of the Green- and Red-Line Coronal Emissions and Their Contribution to the K-Corona

May 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agusm..sh41b06t&link_type=abstract

American Geophysical Union, Spring Meeting 2001, abstract #SH41B-06

Physics

7509 Corona

Scientific paper

We have made a detailed analysis of the high-resolution images of the corona obtained during the total solar eclipse on 1991, July 11. The purpose of the analysis is to derive the temperature and density structure of the observed corona as reliable as possible by using the absolute intensities of the the green (530.3 nm) and red (637.4 nm) coronal emission lines and then contrasted to the continuum intensity. First, we focus our attention to the loops appeared distinctly in emission-line images. With the help of a structure-enhancement algorithm, we show the following results in a quantitative way. (1) The green- and red-line loops are quite separately distributed in space. (2) In the innermost corona, structures in the red-line tend to contribute more to the total column density than the green-line structures. Second, we study individual emission-line loops and find that, (1) The electron densities are almost the same between the two wavelengths. (2) Density-falls with height are nearly hydrostatic in most loops, while some red-line loops significantly deflected from the hydrostatic curve. (3) Column density of the analysed loops only explains 0.1 to 0.2 of the total column density derived from the continuum intensity at the same point. Then, we propose a method to determine the contribution of the non-loop component of these emission lines to the total column density. It is found that the total column density in the analyzed region can be reasonably explained by a mixture of the 530.3 nm component with a line-of-sight length comparable to the size of the active region, and the 637.4 nm component, which tends to concentrate in loop structures. We thereby conclude that the observed corona is well explained by plasma of temperatures ranging from 1 MK to 2 MK.

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