Magnetised plasma turbulence in clusters of galaxies

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dc.creatorSchekochihin, A. A.
dc.creatorCowley, S. C.
dc.creatorKulsrud, R. M.
dc.creatorHammett, G. W.
dc.creatorSharma, P.
dc.date2004-11-30
dc.date.accessioned2026-07-07T02:16:05Z
dc.date.available2026-07-07T02:16:05Z
dc.descriptionCluster plasmas are magnetised already at very low magnetic field strength. Low collisionality implies that conservation of the first adiabatic invariant results in an anisotropic viscous stress (Braginskii viscosity) or, equivalently, anisotropic plasma pressure. This triggers firehose and mirror instabilities, which have growth rates proportional to the wavenumber down to scales of the order of ion Larmor radius. This means that MHD equations with Braginskii viscosity are not well posed and fully kinetic description is necessary. In this paper, we review the basic picture of small-scale dynamo in the cluster plasma and attempt to reconcile it with the existence of plasma instabilities at collisionless scales.
dc.descriptionlatex, 6 pages, 1 figure; Proceedings of "Magnetized Plasma in Galaxy Evolution", Sep. 27th-Oct. 1st 2004, Jagiellonian University, Krakow, Poland, Eds. K. T. Chyzy, R.-J. Dettmar, K. Otmianowska-Mazur and M. Soida
dc.identifierhttps://arxiv.org/abs/astro-ph/0411781
dc.identifierhttp://arxiv.org/abs/astro-ph/0411781
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/8653
dc.subjectAstrophysics
dc.subjectPlasma Physics
dc.titleMagnetised plasma turbulence in clusters of galaxies
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