Hydrostatic Structure of a Hot Plasma and X-Ray Morphology in Non-Spherical Clusters of Galaxies : Is the Perseus Cluster Rotating?

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The hydrostatic equilibrium solutions for the hot gas in non-spherical clusters of galaxies have been studied assuming the polytropic relation. As a gravitational potential form, we assume the model proposed by Miyamoto and Nagai. The equilibrium distributions of density and X-ray emissivity of hot intracluster gas are calculated for both cases with and without rotation. In the case without rotaion, the profiles of gas density and the X-ray emissivity are nearly spherical even if the distribution of galaxies is highly flattened. The reason is that the shape of gravitational potential is not so elongated as yet. On the other hand, in the case with rotation the more flattened distributions of gas density and X-ray emissivity than that of galaxies are possible. These results are applied to the extended X-ray souse in the Perseus cluster. It can be concluded that both the intracluster gas and the Perseus cluster itself are rotating. In relation to this conclusion, some comments of future theoretical and observational studies are given.
理論物理学刊行会の論文
1978-11-25