Emergence of two types of terrestrial planet on solidification of magma ocean

  title={Emergence of two types of terrestrial planet on solidification of magma ocean},
  author={Keiko Hamano and Yutaka Abe and Hidenori Genda},
Understanding the origins of the diversity in terrestrial planets is a fundamental goal in Earth and planetary sciences. In the Solar System, Venus has a similar size and bulk composition to those of Earth, but it lacks water. Because a richer variety of exoplanets is expected to be discovered, prediction of their atmospheres and surface environments requires a general framework for planetary evolution. Here we show that terrestrial planets can be divided into two distinct types on the basis of… 
Planetary science: Evolutionary dichotomy for rocky planets
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Mars and Venus: Different destinies of terrestrial planets
  • O. Korablev
  • Physics, Geology
    Herald of the Russian Academy of Sciences
  • 2016
Being insignificantly different in distance from the Sun, the main terrestrial planets—Venus, the Earth, and Mars—fall, with due account for inaccuracies, within the so-called habitable zone, i.e.,
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It is now understood that the accretion of terrestrial planets naturally involves giant collisions, the moon-forming impact being a well-known example. In the aftermath of such collisions, the
Magma Ocean Evolution of the TRAPPIST-1 Planets.
MmOc, a versatile magma-ocean evolution model, validated against the rocky super-Earth GJ 1132b and early Earth and finds that only 3-5% of the initial water will be locked in the mantle after the magma ocean solidified.


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