Magnetohydrodynamic experiments on cosmic magnetic fields

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dc.creatorStefani, Frank
dc.creatorGailitis, Agris
dc.creatorGerbeth, Gunter
dc.date2008-07-02
dc.date2008-10-13
dc.date.accessioned2026-07-07T13:13:50Z
dc.date.available2026-07-07T13:13:50Z
dc.descriptionIt is widely known that cosmic magnetic fields, i.e. the fields of planets, stars, and galaxies, are produced by the hydromagnetic dynamo effect in moving electrically conducting fluids. It is less well known that cosmic magnetic fields play also an active role in cosmic structure formation by enabling outward transport of angular momentum in accretion disks via the magnetorotational instability (MRI). Considerable theoretical and computational progress has been made in understanding both processes. In addition to this, the last ten years have seen tremendous efforts in studying both effects in liquid metal experiments. In 1999, magnetic field self-excitation was observed in the large scale liquid sodium facilities in Riga and Karlsruhe. Recently, self-excitation was also obtained in the French "von Karman sodium" (VKS) experiment. An MRI-like mode was found on the background of a turbulent spherical Couette flow at the University of Maryland. Evidence for MRI as the first instability of an hydrodynamically stable flow was obtained in the "Potsdam Rossendorf Magnetic Instability Experiment" (PROMISE). In this review, the history of dynamo and MRI related experiments is delineated, and some directions of future work are discussed.
dc.description25 pages, 26 figures, to appear in ZAMM
dc.identifierhttps://arxiv.org/abs/0807.0299
dc.identifierhttp://arxiv.org/abs/0807.0299
dc.identifierZ. Angew. Math. Mech. 88, 930-954, 2008
dc.identifierdoi:10.1002/zamm.200800102
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/230019
dc.subjectAstrophysics
dc.subjectFluid Dynamics
dc.titleMagnetohydrodynamic experiments on cosmic magnetic fields
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