Elemental Abundances in the Solar Upper Atmosphere Derived by Spectroscopic Means |
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Authors: | Feldman U Widing KG |
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Institution: | (1) Artep Inc, 2922 Excelsior Spring Circle, Ellicott City, Columbia MD, 21042;(2) E.O. Hulburt Center for Space Research, Naval Research laboratory, Washington DC, 20375-5352, USA;(3) Computational Physics Inc, Fairfax, VA, 22031;(4) E.O. Hulburt Center for Space Research, Naval Research laboratory Washington DC, 20375-5352, USA |
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Abstract: | The composition of the solar photosphere is believed to be uniform. Indeed a quantity that does not vary with solar surface
location or with a particular solar feature, i.e., no observational evidence is available to indicate that the photospheric
composition near the solar equator is different from the photospheric composition near the solar poles or that the photospheric
composition in quiet regions is different from the composition in active regions. In contrast, the composition of the solar
upper atmosphere is not well defined. Solar composition work in recent decades has brought the recognition that there are
systematic differences between the composition of the corona and the photosphere and revealed evidence for spatial and time
variability in the composition of various coronal features. We review the spectroscopic techniques used and the progress that
was made in recent years in deriving the plasma compositions of various solar upper atmosphere structures.
This revised version was published online in August 2006 with corrections to the Cover Date. |
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