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Turbulence in Space Plasmas pp 129–155Cite as

The Solar Atmosphere

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Part of the book series: Lecture Notes in Physics ((LNP,volume 778))

Looking at the solar photosphere, we see the top of the convection zone in the form of granulation: hot gas rising from the solar interior as part of the energy transport process reaches a position where the opacity is no longer sufficient to prevent the escape of radiation. The gas expands, radiates, and cools and in so doing loses its buoyancy and descends. These motions, ultimately driven by the requirement that the energy generated by nuclear fusion in the Sun’s core be transported in the most efficient manner, represent a vast reservoir of “mechanical” energy flux.

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  1. Institute of Theoretical Astrophysics, University of Oslo, PB 1029 Blindern, 0315 Oslo, Norway

    V.H. Hansteen & M. Carlsson

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  1. V.H. Hansteen
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  2. M. Carlsson
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Correspondence to V.H. Hansteen .

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    Hansteen, V., Carlsson, M. (2009). The Solar Atmosphere. In: Cargill, P., Vlahos, L. (eds) Turbulence in Space Plasmas. Lecture Notes in Physics, vol 778. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-642-00210-6_4

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    • DOI: https://doi.org/10.1007/978-3-642-00210-6_4

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