Turbulence and Magnetic Fields in Astrophysical Plasmas

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dc.creatorSchekochihin, A. A.
dc.creatorCowley, S. C.
dc.date2005-07-29
dc.date2007-05-14
dc.date.accessioned2026-07-07T08:01:01Z
dc.date.available2026-07-07T08:01:01Z
dc.descriptionWe discuss the current understanding of the most basic properties of astrophysical MHD turbulence and trace the origins of the modern views and theoretical uncertainties to the ideas set forth in 1950s and 1960s by Iroshnikov, Kraichnan, Batchelor, Schlueter and Biermann. Universal aspects of the theory are emphasised. Two main astrophysical applications are touched upon: turbulence in the solar wind and in clusters of galaxies. These are, in a certain (very approximate) sense, two ``pure'' cases of small-scale turbulence, where theoretical models of the two main regimes of MHD turbulence -- with and without a strong mean magnetic field -- can be put to the test. They are also good examples of a complication that is more or less generic in astrophysical plasmas: the MHD description is, in fact, insufficient for astrophysical turbulence and plasma physics must make an entrance.
dc.descriptionlatex, 30 pages, 7 figures. Minor corrections. Version with better-resolved Figs. 1, 4, 6 is available from http://www.damtp.cam.ac.uk/user/as629/ or by e-mail upon request. Invited chapter in "Magnetohydrodynamics: Historical Evolution and Trends", S. Molokov et al., Eds, Springer (2007), pp. 85-115
dc.identifierhttps://arxiv.org/abs/astro-ph/0507686
dc.identifierhttp://arxiv.org/abs/astro-ph/0507686
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/128823
dc.subjectAstrophysics
dc.subjectChaotic Dynamics
dc.subjectHistory and Philosophy of Physics
dc.subjectPlasma Physics
dc.subjectSpace Physics
dc.titleTurbulence and Magnetic Fields in Astrophysical Plasmas
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