Abstract
The dependence of iron abundance on cluster temperature is subject to continuous debate. There are some evidences of decreasing abundances from ~0.7 to ~0.3 times the solar metallicity in the temperature range of ~3 — 10 keV [1], while a roughly constant value of ~0.3 times solar is claimed [2]. Physical interpretation of these ambiguous observational results calls for robust theoretical models that can predict systematic trends for the enrichment of clusters of different masses.
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Cora, S., Tornatore, L., Borgani, S. (2007). Comparing Semi-Analytical and Numerical Modelling of the ICM Chemical Enrichment. In: Saviane, I., Ivanov, V.D., Borissova, J. (eds) Groups of Galaxies in the Nearby Universe. ESO ASTROPHYSICS SYMPOSIA. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-540-71173-5_59
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