Abstract
It has always been evident that the classical picture of the solar atmosphere as a smooth spherically symmetrical layer was only an approximation, since horizontal inhomogeneities, like the granular appearance of the photosphere, are plainly visible. Theoretical requirements of mechanisms for the mechanical transfer of energy from the granulation layer into the high chromosphere and corona have spurred the study of these inhomogeneities, a most important aspect of which is the motion of material in the solar atmosphere.
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© 1965 Springer Science+Business Media Dordrecht
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Evans, J.W. (1965). Observational Study of the Dynamics of the Solar Atmosphere. In: Chang, C.C., Huang, S.S. (eds) Proceedings of the Plasma Space Science Symposium. Astrophysics and Space Science Library, vol 3. Springer, Dordrecht. https://doi.org/10.1007/978-94-011-7542-5_6
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DOI: https://doi.org/10.1007/978-94-011-7542-5_6
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