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The Magnetic Chromosphere

  • Chapter
Solar Surface Magnetism

Part of the book series: NATO ASI Series ((ASIC,volume 433))

Abstract

Chromospheres - hot luminous shells surrounding stars - radiate predominantly in spectral lines at temperatures exceeding the underlying photospheric temperatures. This temperature inversion can be created and sustained only by non-radiative processes. Although they exist in almost every spectral class, chromospheres are more conspicuous in stars with convective envelopes. The identity of sources of mechanical or electrodynamic energy remains elusive. Chromospheres compel attention because of their challenging physics, their significance to the photochemistry of the terrestrial atmosphere, and their role in the variable luminosity of stars. Observations show that magnetic fields are closely related to the distribution, fine structure, and dynamism of chromospheric emission. This review considers recent research aimed at defining their role in chromospheric physics.

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  1. Herzberg Institute of Astrophysics, National Research Council of Canada, 100 Sussex Drive, Ottawa, K1A 0R6, Canada

    V. Gaizauskas

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  1. Sterrekundig Instituut, Utrecht University, Utrecht, The Netherlands

    Robert J. Rutten  & Carolus J. Schrijver  & 

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Gaizauskas, V. (1994). The Magnetic Chromosphere. In: Rutten, R.J., Schrijver, C.J. (eds) Solar Surface Magnetism. NATO ASI Series, vol 433. Springer, Dordrecht. https://doi.org/10.1007/978-94-011-1188-1_11

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  • DOI: https://doi.org/10.1007/978-94-011-1188-1_11

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