Abstract
The abundances of atmospheric gases in planetary atmospheres impose certain boundary conditions upon the planetary formation theories. One of the most important is that the present volatiles did probably not undergo a hot phase during early accretion and must have been added at a later stage if there was such a hot phase.
While in the outer planets, especially Jupiter, a primordial or solar composition of element abundances could survice, the inner planets have suffered major transformations. At Venus and Mars water must have been dissociated and hydrogen escaped. CO2 was probably chemically bound in the Martian crust while it could not react with the crust material at Venus because of the high temperatures which developed soon due to the greenhouse effect. At Earth, because of its intermediate temperatures, a number of reactions occurred but the most significant change was due to the generation of life which changed the formerly reducing atmosphere into an oxidizing one.
Finally a short overview is given of the present knowledge about the structure of the planetary atmospheres.
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Bolle, HJ. (1982). Atmospheric Evolution. In: Coradini, A., Fulchignoni, M. (eds) The Comparative Study of the Planets. NATO Advanced Study Institutes Series, vol 85. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-7810-2_17
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DOI: https://doi.org/10.1007/978-94-009-7810-2_17
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