MAGNETIC FIELD AMPLIFICATION AND EVOLUTION IN TURBULENT COLLISIONLESS MAGNETOHYDRODYNAMICS: AN APPLICATION TO THE INTRACLUSTER MEDIUM

The amplification of magnetic fields (MFs) in the intracluster medium (ICM) is attributed to turbulent dynamo (TD) action, which is generally derived in the collisional-MHD framework. However, this assumption is poorly justified a priori, since in the ICM the ion mean free path between collisions is...

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Bibliographic Details
Published in:The Astrophysical journal 2014-02, Vol.781 (2), p.1-21
Main Authors: Santos-Lima, R, DAL PINO, E M DE GOUVEIA, Kowal, G, FALCETA-GONCALVES, D, Lazarian, A, NAKWACKI, M S
Format: Article
Language:English
Subjects:
Amplification
ANISOTROPY
ASTROPHYSICS, COSMOLOGY AND ASTRONOMY
COLLISIONS
Computational fluid dynamics
Computer simulation
COMPUTERIZED SIMULATION
DENSITY
EVOLUTION
FEEDBACK
GALAXY CLUSTERS
HOSE INSTABILITY
Instability
MAGNETIC FIELDS
MAGNETOHYDRODYNAMICS
Mathematical models
MEAN FREE PATH
PLASMA PRESSURE
RELAXATION
STAR CLUSTERS
TURBULENCE
Turbulent flow
VELOCITY
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Summary:The amplification of magnetic fields (MFs) in the intracluster medium (ICM) is attributed to turbulent dynamo (TD) action, which is generally derived in the collisional-MHD framework. However, this assumption is poorly justified a priori, since in the ICM the ion mean free path between collisions is of the order of the dynamical scales, thus requiring a collisionless MHD description. The present study uses an anisotropic plasma pressure that brings the plasma within a parametric space where collisionless instabilities take place. In this model, a relaxation term of the pressure anisotropy simulates the feedback of the mirror and firehose instabilities, in consistency with empirical studies. Our three-dimensional numerical simulations of forced transonic turbulence, aiming the modeling of the turbulent ICM, were performed for different initial values of the MF intensity and different relaxation rates of the pressure anisotropy. We found that in the high- beta plasma regime corresponding to the ICM conditions, a fast anisotropy relaxation rate gives results that are similar to the collisional-MHD model, as far as the statistical properties of the turbulence are concerned. Also, the TD amplification of seed MFs was found to be similar to the collisional-MHD model. The simulations that do not employ the anisotropy relaxation deviate significantly from the collisional-MHD results and show more power at the small-scale fluctuations of both density and velocity as a result of the action of the instabilities. For these simulations, the large-scale fluctuations in the MF are mostly suppressed and the TD fails in amplifying seed MFs.
ISSN:0004-637X
1538-4357
DOI:10.1088/0004-637X/781/2/84