Solar abundances as derived from solar energetic particles

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Abstract
Recent studies have shown that there are well defined average abundances of heavy (Z≳2) solar energetic particles (SEPs), with variations in the acceleration and propagation producing a systematic flare‐to‐flare fractionation that depends on the charge per unit mass of the ion. Correcting the average SEP abundances for the fractionation yields SEP‐derived coronal abundances for 20 elements. Higher resolution SEP studies have also provided isotopic abundances for 5 elements. SEP‐derived abundances indicate that elements with high first ionization potentials (≳10 eV) are depleted in the corona relative to the photosphere and provide new information on the solar abundance of C and 2 2Ne. Future SEP observations offer the prospect of a significant reduction of the uncertainties in solar elemental and isotopic abundances.

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