Dynamo in the Intra-Cluster Medium: Simulation of CGL-MHD Turbulent Dynamo

Details Dynamo in the Intra-Cluster Medium: Simulation of CGL-MHD Turbulent Dynamo Dynamo in the Intra-Cluster Medium: Simulation of CGL-MHD Turbulent Dynamo

2011-02-25

arxiv.org/abs/1102.5139v1

Astronomy and Astrophysics

Astrophysics

Cosmology and Extragalactic Astrophysics

3 pages, 1 figure, 274 IAU Symposium: Advances in Plasma Astrophysics

Scientific paper

The standard magnetohydrodynamic (MHD) description of the plasma in the hot, magnetized gas of the intra-cluster (ICM) medium is not adequate because it is weakly collisional. In such collisionless magnetized gas, the microscopic velocity distribution of the particles is not isotropic, giving rise to kinetic effects on the dynamical scales. These kinetic effects could be important in understanding the turbulence, as so as the amplification and maintenance of the magnetic fields in the ICM. It is possible to formulate fluid models for collisonless or weakly collisional gas by introducing modifications in the MHD equations. These models are often referred as kinetic MHD (KMHD). Using a KMHD model based on the CGL-closure, which allows the adiabatic evolution of the two components of the pressure tensor (the parallel and perpendicular components with respect to the local magnetic field), we performed 3D numerical simulations of forced turbulence in order to study the amplification of an initially weak seed magnetic field. We found that the growth rate of the magnetic energy is comparable to that of the ordinary MHD turbulent dynamo, but the magnetic energy saturates in a level smaller than of the MHD case. We also found that a necessary condition for the dynamo works is to impose limits to the anisotropy of the pressure.

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