On the basis of the model proposed by Matsui and Abe, we will show that two major factors - distance from the Sun and the efficiency of retention of accretional energy - control the early evolution of the terrestrial planets. A diagram of accretional energy versus the optical depth of a proto-atmosphere provides a means to follow the evolutionary track of surface temperature of the terrestrial planets and an explanation for why the third planet in our solar system is an 'aqua'-planet. © 1987 D. Reidel Publishing Company.
CITATION STYLE
Matsui, T., & Abe, Y. (1987). Evolutionary tracks of the terrestrial planets. Earth, Moon and Planets, 39(3), 207–214. https://doi.org/10.1007/BF00055050
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