Loop interaction in the visible emission corona: Morphological details

Details Loop interaction in the visible emission corona: Morphological details Loop interaction in the visible emission corona: Morphological details

Sep 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987nascp2483..129s&link_type=abstract

In NASA-Goddard Space Flight Center, Theoretical Problems in High Resolution Solar Physics, 2 p 129-132 (SEE N88-11609 02-92)

Physics

5

Coronal Loops, Electron Density (Concentration), Solar Flares, Solar Granulation, Solar Spectra, Emission Spectra, Iron, Line Spectra, Spectrum Analysis

Scientific paper

Coronagraph observations of two post-flare loop systems, recorded photographically in the emissions of Fe XIV (5303 Å) and Fe X (6374 Å), show occasional enhancements at the intersections of some loops. The brightness of such enhancements in the green-line gradually increases to a maximum value several times greater than that of the legs of the loops and then declines with a typical lifetime ≡30 - 60 minutes. In red-line emission the loop systems are usually very faint, but show the same overall type of enhancement, with a lag in maximum brightness relative to that of the green line ≡10 minutes. The electron density, derived from the cooling times, is ≡1012cm-3.

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