Atmospheric Evolution of the Terrestrial Planets

@article{Hunten1993AtmosphericEO,
  title={Atmospheric Evolution of the Terrestrial Planets},
  author={Donald M. Hunten},
  journal={Science},
  year={1993},
  volume={259},
  pages={915 - 920}
}
The major atmospheric gases on Earth, Venus, and Mars were probably CO[sub 2], H[sub 2]O, and N[sub 2]. Most of the Earth's CO[sub 2] is tied up in minerals such as limestone, and Venus has lost most of its H[sub 2]O, leaving the CO[sub 2] in the atmosphere. Much of Mars' atmosphere may have been eroded in impacts by large meteoroids early in solar-system history. Noble gases are very underabundant everywhere, and must have been lost during an early period; they were probably dragged along… Expand
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The current composition of the mantle indicates that much of the re-equilibration took place in a deep (> 400 km) molten silicate layer, or ‘magma ocean’, and that conditions became more oxidizing with time as the Earth grew. Expand
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The evolution and escape of the martian atmosphere and the planet’s water inventory can be separated into an early and late evolutionary epoch. The first epoch started from the planet’s origin andExpand
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A Comparative Study of the Influence of the Active Young Sun on the Early Atmospheres of Earth, Venus, and Mars
Abstract Because the solar radiation and particle environment plays a major role in all atmospheric processes such as ionization, dissociation, heating of the upper atmospheres, and thermal andExpand
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