Summary
We carried out 2D and 3D magnetohydrodynamic simulations including radiative cooling and anisotropic thermal conduction of a magnetically turbulent intracluster medium. In 3D simulations, we found that magnetic pressure increases by a factor of 2 at 1.4 Gyr because magnetic fields accumulate in the center along with the plasma contracting by the cooling instability. In 2D simulations including thermal conduction, we found that a low temperature region exists along the loop-shaped magnetic field lines. Thus, the restriction of thermal conduction across magnetic field lines enables the coexistence of hot and cool plasmas in cluster cores.
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© 2007 Springer-Verlag Berlin Heidelberg
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Asai, N., Fukuda, N., Matsumoto, R. (2007). MHD Simulations of Clusters of Galaxies Including Radiative Cooling. In: Böhringer, H., Pratt, G., Finoguenov, A., Schuecker, P. (eds) Heating versus Cooling in Galaxies and Clusters of Galaxies. Eso Astrophysics Symposia. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-540-73484-0_40
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DOI: https://doi.org/10.1007/978-3-540-73484-0_40
Publisher Name: Springer, Berlin, Heidelberg
Print ISBN: 978-3-540-73483-3
Online ISBN: 978-3-540-73484-0
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