Abstract
The atomic physics relevant to the interpretation of solar spectra produced by plasmas at temperatures ≳ 105 K are discussed. Methods for determining relative abundance ratios are presented and examples provided from the Coronal Diagnostic Spectrometer on board SOHO. In particular, the Fe/Si ratio in the corona is found to be close to photospheric; the Mg/Ne ratio in the transition region is found to vary by an order of magnitude in different solar features. The Mg/Ne ratios in supergranule cell centres and the network are separated for the first time, although no significant differences are found.
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Young, P., Mason, H. Atomic Physics for Atmospheric Composition Measurements. Space Science Reviews 85, 315–326 (1998). https://doi.org/10.1023/A:1005119005133
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DOI: https://doi.org/10.1023/A:1005119005133