Abstract
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.
