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Properties of MHD turbulence and its consequences for the ISM and ICM

Published online by Cambridge University Press:  21 October 2010

D. Falceta-Gonçalves ,
G. Kowal  and
A. Lazarian
D. Falceta-Gonçalves
Affiliation:
Núcleo de Astrofísica Teórica, Universidade Cruzeiro do Sul - Rua Galvão Bueno 868, CEP 01506-000, São Paulo, Brazil
G. Kowal
Affiliation:
Jagiellonian University, ul. Orla 171, 30-244 Kraków, Poland
A. Lazarian
Affiliation:
University of Wisconsin, Madison, 475 N. Charter St., WI 53711, USA
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Abstract

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It is well known that the interstellar (ISM) and intergalactic (ICM) media are threaded by large scale magnetic fields. The understanding of its role on the dynamics of the media is, however, still in progress. For the ISM, magnetic fields may control or, at least, play a major role on the turbulence cascade leading to the star formation process. The ICM, on the other hand, is assumed to be thermally dominated but still the magnetic field may play an important role on the processes of acceleration and propagation of cosmic rays. In this work we provide a review of the latest theoretical results on the evolution of MHD turbulence under collisional and collisionless plasma approaches.

Keywords

hydrodynamicsturbulencemethods: numericalISM: magnetic fieldsgalaxies: clusters: general
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Highlights H15: Highlights of Astronomy , November 2009 , pp. 464 - 465
Copyright
Copyright © International Astronomical Union 2010

References

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