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Interplanetary Dust Close to the Sun

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Origin and Evolution of Interplanetary Dust

Part of the book series: Astrophysics and Space Science Library ((ASSL,volume 173))

Abstract

The optical and infrared brightness of the Fraunhofer-corona is produced by light scattering at the zodiacal dust particles and by their thermal emission (see Koutchmy and Lamy 1985). It is modelled within the ecliptic (4 Ro ≤ ε ≤ 15 Ro) taking into account investigations of the global zodiacal dust cloud due to remote sensing and in situ experiments. The input of near solar dust to the corona brightness is discussed.

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References

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Author information

Author notes

  1. Ingrid Mann

    Present address: Max-Planck-Institut für Aeronomie, D 3411, Katlenburg-Lindau, Germany

Authors and Affiliations

  1. Ruhr-Universität Bochum, D 4630, Bochum, Germany

    Ingrid Mann

Authors
  1. Ingrid Mann
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Editor information

Editors and Affiliations

  1. Aeronomie CNRS, Université Paris VI, Verrières-le-Buisson, France

    A. C. Levasseur-Regourd

  2. Osaka Sangyo University, Osaka, Japan

    H. Hasegawa

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© 1991 Springer Science+Business Media Dordrecht

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Mann, I. (1991). Interplanetary Dust Close to the Sun. In: Levasseur-Regourd, A.C., Hasegawa, H. (eds) Origin and Evolution of Interplanetary Dust. Astrophysics and Space Science Library, vol 173. Springer, Dordrecht. https://doi.org/10.1007/978-94-011-3640-2_38

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  • DOI: https://doi.org/10.1007/978-94-011-3640-2_38

  • Publisher Name: Springer, Dordrecht

  • Print ISBN: 978-94-010-5616-8

  • Online ISBN: 978-94-011-3640-2

  • eBook Packages: Springer Book Archive

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