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2007•GAMM-MitteilungenOpen access

Forward and inverse problems in MHD: Numerical and experimental results

Frank Stefani, A. Gailītis, G. Gerbeth, Thomas Gundrum, Mingtian Xu

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Abstract

Abstract When a conducting fluid comes under the influence of a magnetic field, electrical currents are induced that give rise to a modification of this magnetic field. The ratio of induced magnetic field to applied magnetic field is characterized by the magnetic Reynolds number Rm of the flow. For large Rm, even self‐excitation of a magnetic field can occur. Thishydromagnetic dynamo effectis responsible for the maintenance of the magnetic fields of planets, stars and galaxies. In the present paper, we delineate some recent developments in the numerical treatment of induction effects in arbitrary geometry, and their application for dynamo experiments as well as for a “Contactless Inductive Flow Tomography (CIFT)”. (© 2007 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)

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Abstract When a conducting fluid comes under the influence of a magnetic field, electrical currents are induced that give rise to a modification of this magnetic field. The ratio of induced magnetic field to applied magnetic field is characterized by the magnetic Reynolds number Rm of the flow. For large Rm, even self‐excitation of a magnetic field can occur. Thishydromagnetic dynamo effectis responsible for the maintenance of the magnetic fields of planets, stars and galaxies. In the present paper, we delineate some recent developments in the numerical treatment of induction effects in arbitrary geometry, and their application for dynamo experiments as well as for a “Contactless Inductive Flow Tomography (CIFT)”. (© 2007 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)

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Available abstract

Abstract When a conducting fluid comes under the influence of a magnetic field, electrical currents are induced that give rise to a modification of this magnetic field. The ratio of induced magnetic field to applied magnetic field is characterized by the magnetic Reynolds number Rm of the flow. For large Rm, even self‐excitation of a magnetic field can occur. Thishydromagnetic dynamo effectis responsible for the maintenance of the magnetic fields of planets, stars and galaxies. In the present paper, we delineate some recent developments in the numerical treatment of induction effects in arbitrary geometry, and their application for dynamo experiments as well as for a “Contactless Inductive Flow Tomography (CIFT)”. (© 2007 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)

Key concepts: Dynamo, Magnetic Reynolds number, Magnetohydrodynamics, Magnetic field, Physics, Dynamo theory, Excitation, Reynolds number

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