Abstract
In the large solar energetic particle (SEP) events, coronal mass ejections (CMEs) drive shock waves out through the corona that accelerate elements of the ambient material to MeV energies in a fairly democratic, temperature-independent manner. These events provide the most complete source of information on element abundances in the corona. Relative abundances of 22 elements from H through Zn display the well-known dependence on the first ionization potential (FIP) that distinguishes coronal and photospheric material. For most elements, the main abundance variations depend upon the gyrofrequency, and hence on the charge-to-mass ratio, Q/A, of the ion. Abundance variations in the dominant species, H and He, are not Q/A dependent, presumably because of non-linear wave-particle interactions of H and He during acceleration. Impulsive flares provide a different sample of material that confirms the Ne:Mg:Si and He/C abundances in the corona.
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Reames, D.V. (1998). Solar Energetic Particles: Sampling Coronal Abundances. In: Fröhlich, C., Huber, M.C.E., Solanki, S.K., Von Steiger, R. (eds) Solar Composition and its Evolution — from Core to Corona. Space Sciences Series of ISSI, vol 5. Springer, Dordrecht. https://doi.org/10.1007/978-94-011-4820-7_29
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