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We study the impact of an intracluster magnetic field on the main structuralproperties of clusters and groups of galaxies: the radial density and entropyprofiles, the S-T relation and the L_X-T relation for groups and clusters ofgalaxies. To this aim, we develop a description of the intra-cluster gas basedon the Hydrostatic Equilibrium condition and on the Magnetic Virial Theorem inthe presence of a radial distribution of the magnetic field B(r)=B_* \times[\rho_g(r)]^alpha, with alpha \sim 0.9, as indicated by observations andnumerical simulation. Our analysis shows that such a description is able toprovide a possible explanation of three problematic aspects of the clusterstructure: i) the flattening of the entropy profile in the cluster center; ii)the flatness of the S-T relation; iii) the increasing steepening of the L_X-Trelation from the cluster scale towards the group scales. The available entropyand X-ray luminosity data indicate that an increase of the magnetic field B_*\sim T^0.5 is required to reproduce at the same time both the S-T and the L_X-Trelations. It follows that a consistent description of the magnetized ICM canprovide a simple explanation of several (or of all) of these still openproblems, and thus weakens the need for the inclusion of othernon-gravitational effects which have been proposed so far for the explanationof some of these features. This (initial, but not conclusive) analysis can beregarded as a starting point for a more refined analytical exploration of thephysics of the magnetized intra-cluster medium, and it provides testablepredictions that can be proven or disproven with the next coming sensitiveobservations of groups and clusters in the X-ray band and in the radiofrequency band.Comment: 18 pages, 19 figures, A&A in pres

Structure and evolution of magnetized clusters: entropy profiles,S–TandLX–Trelations

Structure and evolution of magnetized clusters: entropy profiles,S–TandL_X–Trelations