Astronomy and Astrophysics – Astronomy
Scientific paper
Jul 1995
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995adspr..15q..13s&link_type=abstract
Advances in Space Research (ISSN 0273-1177), vol. 15, no. 7, p. (7)13-(7)22
Astronomy and Astrophysics
Astronomy
19
Abundance, Ionization Potentials, Photosphere, Solar Corona, Solar Wind, Spectroscopic Analysis, Ultraviolet Astronomy, Variations, X Ray Astronomy, Correlation, Data Processing, Data Reduction, Neon, Oxygen, Skylab Program, Solar Atmosphere, Solar Flares, Solar Maximum Mission
Scientific paper
Solar wind and solar energetic particle (SEP) data yield systematic differences between elemental abundances in the corona and in the photosphere related to the first ionization potential (FIP) of the elements: low-FIP elements are preferentially enhanced relative to high-FIP elements by about a factor of four. Spectroscopic studies of the inner corona show that such a pattern may apply on average but not in detail for coronal loops: substantial abundance differences occur between different types of coronal structures, and variations have been found from flare to flare, from one active region to another, and over time in the same region; further, in some flares, anomalies such as enhanced Ne:O ratios, distinctly at odds with the FIP pattern, show that a competing element selection mechanism sometimes operates. Details of the observed abundance variability -- such as the magnitude of the variations, the relevant temporal and spatial scales, and correlations with other properties of the given coronal structure -- may give important clues to the processes which supply and heat the corona, or they may reflect the changing physical conditions or locations where those processes take place. However, many such details remain to be established definitively. At present, abundance variability is primarily a major complication to data analysis and interpretation. However, once it is better understood, it may provide a new diagnostic tool for probing the lower layers of the solar atmosphere.
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