Abstract
Iron L-shell transitions, which lie in the energy range 0.7 – 1.5 keV, can provide a wealth of important information about physical conditions in diverse astronomical sources. Although few data sets of adequate statistical quality are currently available for analysis, the next series of X-ray satellite experiments will provide order-of-magnitude improvements in both resolution and sensitivity for this kind of work. We review the important physical processes that underlie the diagnostic potential of these features. We specifically consider corona) plasmas, X-ray photoionized nebulae, and the ionizing plasmas believed to be present in young supernova remnants.
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Kahn, S.M., Liedahl, D.A. (1991). Iron L-shell line formation in diverse astrophysical environments. In: Treves, A., Perola, G.C., Stella, L. (eds) Iron Line Diagnostics in X-ray Sources. Lecture Notes in Physics, vol 385. Springer, Berlin, Heidelberg. https://doi.org/10.1007/BFb0031265
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DOI: https://doi.org/10.1007/BFb0031265
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