The Height Variations of the Solar Chromosphere

Details The Height Variations of the Solar Chromosphere The Height Variations of the Solar Chromosphere

May 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agusm..sh21b03a&link_type=abstract

American Geophysical Union, Spring Meeting 2001, abstract #SH21B-03

Other

7507 Chromosphere, 7511 Coronal Holes, 7524 Magnetic Fields, 7536 Solar Activity Cycle (2162)

Scientific paper

We present a five year survey of the height of the solar chromosphere, as observed by the Extreme Ultraviolet Imaging Telescope (EIT) in its four bandpasses : 17.1 nm (FeIX/FeX), 19.5 nm (FeXII), 28.4 nm (FeXV), and 30.4 nm (HeII). Spatial pole-equator variations, as well as long-term temporal variations were investigated. The chromosphere was found to be prolate in all four wavelengths, with typical values of Δ D/D = 5x 10-3 in HeII and 1x 10-3 in the three iron lines. We found a very good correlation of the prolateness effect with the presence of polar coronal holes, and could follow its vanishing as the solar cycle peaked. The similitude between our results and previous observations made in various other lines suggest that the prolateness is a fundamental aspect of the solar atmosphere.

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