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Galaxy clusters as hydrodynamics laboratories

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The intra-cluster medium (ICM) of galaxy clusters shows a wealth of hydrodynamical features that trace the growth of clusters via the infall of galaxies or smaller subclusters. Such hydrodynamical features include the wakes of the infalling objects as well as the interfaces between the host cluster’s ICM and the atmosphere of the infalling object. Furthermore, the cluster dynamics can be traced by merger shocks, bow shocks, and sloshing motions of the ICM . Additionally, the prominence of each of these features is modified by transport coefficients in the ICM , i.e., its viscosity and thermal conductivity. I will give an overview of our recent work on understanding and deciphering such traces of cluster growth, regarding both the growth history of clusters as well as transport properties of the ICM .

This talk is part of the Institute of Astronomy Colloquia series.

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