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Coronal Heating and Reduced MHD

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Turbulence and Magnetic Fields in Astrophysics

Part of the book series: Lecture Notes in Physics ((LNP,volume 614))

Abstract

We review the use of reduced magnetohydrodynamics (RMHD) in coronal heating models, with particular emphasis on models for magnetically open regions. A brief review of the nature of the coronal heating problem is presented first, followed by detailed discussion regarding the assumptions and features of RMHD and its applicability to the dynamics of the solar corona. We then review a class of heating models based on quasi-2D turbulent cascades driven by low-frequency Alfvén waves.

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Authors and Affiliations

  1. Department of Mathematics, University of Waikato, Hamilton, New Zealand

    Sean Oughton

  2. Bartol Research Institute, University of Delaware, DE19716, Newark, USA

    Pablo Dmitruk & William H. Matthaeus

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  1. Sean Oughton
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  2. Pablo Dmitruk
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  3. William H. Matthaeus
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Editors and Affiliations

  1. Laboratoire de Radioastronomie, Ecole Normale Supérieure, 24, Rue Lhomond, 75231, Paris Cedex 05, France

    Edith Falgarone

  2. Observatoire de la Côte d’azur, CNRS, B.P.4229, 06304, Nice Cédex 4, France

    Thierry Passot

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Oughton, S., Dmitruk, P., Matthaeus, W.H. (2003). Coronal Heating and Reduced MHD. In: Falgarone, E., Passot, T. (eds) Turbulence and Magnetic Fields in Astrophysics. Lecture Notes in Physics, vol 614. Springer, Berlin, Heidelberg. https://doi.org/10.1007/3-540-36238-X_2

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  • DOI: https://doi.org/10.1007/3-540-36238-X_2

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