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Coupling from the Photosphere to the Chromosphere and the Corona

  • Chapter
The Origin and Dynamics of Solar Magnetism

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

Abstract

The atmosphere of the Sun is characterized by a complex interplay of competing physical processes: convection, radiation, conduction, and magnetic fields. The most obvious imprint of the solar convection and its overshooting in the low atmosphere is the granulation pattern. Beside this dominating scale there is a more or less smooth distribution of spatial scales, both towards smaller and larger scales, making the Sun essentially a multi-scale object. Convection and overshooting give the photosphere its face but also act as drivers for the layers above, namely the chromosphere and corona. The magnetic field configuration effectively couples the atmospheric layers on a multitude of spatial scales, for instance in the form of loops that are anchored in the convection zone and continue through the atmosphere up into the chromosphere and corona. The magnetic field is also an important structuring agent for the small, granulation-size scales, although (hydrodynamic) shock waves also play an important role—especially in the internetwork atmosphere where mostly weak fields prevail. Based on recent results from observations and numerical simulations, we attempt to present a comprehensive picture of the atmosphere of the quiet Sun as a highly intermittent and dynamic system.

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Authors and Affiliations

  1. Institute of Theoretical Astrophysics, University of Oslo, Oslo, Norway

    S. Wedemeyer-Böhm

  2. MPI für Sonnensystemforschung, Katlenburg-Lindau, Germany

    A. Lagg

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

    Å. Nordlund

Authors
  1. S. Wedemeyer-Böhm
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  2. A. Lagg
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  3. Å. Nordlund
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Correspondence to S. Wedemeyer-Böhm .

Editor information

Editors and Affiliations

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

    M. J. Thompson

  2. International Space Science Institute, Bern, Switzerland

    A. Balogh

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

    J. L. Culhane

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

    Å. Nordlund

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

    S. K. Solanki

  6. LUTH, Observatoire de Paris, Meudon, France

    J.-P. Zahn

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Wedemeyer-Böhm, S., Lagg, A., Nordlund, Å. (2008). Coupling from the Photosphere to the Chromosphere and the Corona. In: Thompson, M.J., Balogh, A., Culhane, J.L., Nordlund, Å., Solanki, S.K., Zahn, JP. (eds) The Origin and Dynamics of Solar Magnetism. Space Sciences Series of ISSI, vol 32. Springer, New York, NY. https://doi.org/10.1007/978-1-4419-0239-9_17

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