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The Origin and Dynamics of Solar Magnetism

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  • © 2009

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Editors:
  1. M. J. Thompson

    1. School of Mathematics & Statistics, University of Sheffield, Sheffield, UK

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  2. A. Balogh

    1. International Space Science Institute, Bern, Switzerland

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  3. J. L. Culhane

    1. Mullard Space Science Laboratory, University College London, Dorking, UK

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  4. Å. Nordlund

    1. Niels Bohr Institute, University of Copenhagen, Copenhagen, Denmark

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  5. S. K. Solanki

    1. Max-Planck-Institut für Sonnensystemforschung Katlenburg-Lindau, Germany

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  6. J.-P. Zahn

    1. LUTH, Observatoire de Paris, Meudon, France

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  • Treats the topics of solar variability and how the solar dynamo works in great detail
  • Dynamics and evolution of magnetic fields that drive solar activity are treated in a very comprehensive way

Part of the book series: Space Sciences Series of ISSI (SSSI, volume 32)

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Table of contents (22 chapters)

  1. Front Matter

    Pages i-iv
    Download chapter PDF

  2. Introduction to Solar Magnetism: The Early Years

    • A. Balogh, M. J. Thompson
    Pages 1-14

  3. Solar Magnetism: The State of Our Knowledge and Ignorance

    • E. N. Parker
    Pages 15-24

  4. Chaos and Intermittency in the Solar Cycle

    • Edward A. Spiegel
    Pages 25-51

  5. The Solar Dynamo

    • N. O. Weiss, M. J. Thompson
    Pages 53-66

  6. Flux-Transport Solar Dynamos

    • Mausumi Dikpati, Peter A. Gilman
    Pages 67-75

  7. The Solar Dynamo: The Role of Penetration, Rotation and Shear on Convective Dynamos

    • Steven M. Tobias
    Pages 77-86

  8. Advances in Theory and Simulations of Large-Scale Dynamos

    • Axel Brandenburg
    Pages 87-104

  9. Planetary Dynamos from a Solar Perspective

    • U. R. Christensen, D. Schmitt, M. Rempel
    Pages 105-126

  10. Observations of Photospheric Dynamics and Magnetic Fields: From Large-Scale to Small-Scale Flows

    • N. Meunier, J. Zhao
    Pages 127-149

  11. Large Scale Flows in the Solar Convection Zone

    • Allan Sacha Brun, Matthias Rempel
    Pages 151-173

  12. Photospheric and Subphotospheric Dynamics of Emerging Magnetic Flux

    • A. G. Kosovichev
    Pages 175-195

  13. The Topology and Behavior of Magnetic Fields Emerging at the Solar Photosphere

    • B. W. Lites
    Pages 197-212

  14. Sunspots: From Small-Scale Inhomogeneities Towards a Global Theory

    • Rolf Schlichenmaier
    Pages 213-228

  15. Recent Evidence for Convection in Sunspot Penumbrae

    • Göran B. Scharmer
    Pages 229-247

  16. Helioseismology of Sunspots: A Case Study of NOAA Region 9787

    • L. Gizon, H. Schunker, C. S. Baldner, S. Basu, A. C. Birch, R. S. Bogart et al.
    Pages 249-273

  17. Small-Scale Solar Magnetic Fields

    • A. G. de Wijn, J. O. Stenflo, S. K. Solanki, S. Tsuneta
    Pages 275-315

  18. Coupling from the Photosphere to the Chromosphere and the Corona

    • S. Wedemeyer-Böhm, A. Lagg, Å. Nordlund
    Pages 317-350

  19. Magnetic Flux Emergence, Activity, Eruptions and Magnetic Clouds: Following Magnetic Field from the Sun to the Heliosphere

    • L. van Driel-Gesztelyi, J. L. Culhane
    Pages 351-381

  20. Coronal Holes and Open Magnetic Flux

    • Y.-M. Wang
    Pages 383-399
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Keywords

About this book

Starting in 1995 numerical modeling of the Earth’s dynamo has ourished with remarkable success. Direct numerical simulation of convection-driven MHD- ow in a rotating spherical shell show magnetic elds that resemble the geomagnetic eld in many respects: they are dominated by the axial dipole of approximately the right strength, they show spatial power spectra similar to that of Earth, and the magnetic eld morphology and the temporal var- tion of the eld resembles that of the geomagnetic eld (Christensen and Wicht 2007). Some models show stochastic dipole reversals whose details agree with what has been inferred from paleomagnetic data (Glatzmaier and Roberts 1995; Kutzner and Christensen 2002; Wicht 2005). While these models represent direct numerical simulations of the fundamental MHD equations without parameterized induction effects, they do not match actual pla- tary conditions in a number of respects. Speci cally, they rotate too slowly, are much less turbulent, and use a viscosity and thermal diffusivity that is far too large in comparison to magnetic diffusivity. Because of these discrepancies, the success of geodynamo models may seem surprising. In order to better understand the extent to which the models are applicable to planetary dynamos, scaling laws that relate basic properties of the dynamo to the fundamental control parameters play an important role. In recent years rst attempts have been made to derive such scaling laws from a set of numerical simulations that span the accessible parameter space (Christensen and Tilgner 2004; Christensen and Aubert 2006).

Editors and Affiliations

  • School of Mathematics & Statistics, University of Sheffield, Sheffield, UK

    M. J. Thompson

  • International Space Science Institute, Bern, Switzerland

    A. Balogh

  • Mullard Space Science Laboratory, University College London, Dorking, UK

    J. L. Culhane

  • Niels Bohr Institute, University of Copenhagen, Copenhagen, Denmark

    Å. Nordlund

  • Max-Planck-Institut für Sonnensystemforschung Katlenburg-Lindau, Germany

    S. K. Solanki

  • LUTH, Observatoire de Paris, Meudon, France

    J.-P. Zahn

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