Magnetic Fields and Turbulences in Clusters of Galaxies

Details Magnetic Fields and Turbulences in Clusters of Galaxies Magnetic Fields and Turbulences in Clusters of Galaxies

Aug 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009rmxac..36..262k&link_type=abstract

Magnetic Fields in the Universe II: From Laboratory and Stars to the Primordial Universe - Supplementary CD (Eds. A. Esquivel, J

Astronomy and Astrophysics

Astronomy

Galaxies: Clusters, Galaxies: Magnetic Fields, Turbulences

Scientific paper

Magnetic fields and turbulences are among the most important non-thermal components in the intra-cluster medium (ICM), estimated to be 10% or more of the total thermal energy. We study the influence of large-scale magnetic fields by completing the hydrostatic equilibrium equation with the magnetic field pressure component. In a perturbative approach we derive a new gas density profile for the ICM which takes into account the magnetic field strength. The new gas density varies by up to 20% in the cluster core. Similarly, we parametrize the ICM turbulences assuming a uniform large-scale component generated by the cluster merger history and a radius dependent small-scale component from the motion of galaxies in the cluster core. We study the two contributions as a function of the model parameters and we point out their functional difference.

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