Atmospheric Evolution of the Terrestrial Planets

  title={Atmospheric Evolution of the Terrestrial Planets},
  author={Donald M. Hunten},
  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
Although the planets Mercury, Venus, Earth, and Mars have masses within a single order of magnitude range, they possess atmospheres with extremely different properties (Table 1). These bodies mayExpand
Comparative Planetary Evolution
This chapter focuses on the Earth as a member of the solar system by comparing it to other planets. In its early stages of growth, the Earth probably had a magma ocean sustained by the heat sourcesExpand
Escape of Planetary Atmospheres
The extreme radiation and plasma environments during the period of the young active Sun/Stars have important implications for the evolution of planetary atmospheres and may be responsible thatExpand
Atmospheric and water loss from early Venus
Abstract Previous interpretations of the Pioneer Venus mass spectrometer data of the deuterium to hydrogen ( D / H ) ratio of 1.9 × 10 - 2 or 120 ± 40 times the terrestrial value indicate that VenusExpand
Pathways to Earth-Like Atmospheres
It is shown that planets even in orbits within the habitable zone of their host stars might not lose nebular- or catastrophically outgassed initial protoatmospheres completely and could end up as water worlds with CO2 and hydrogen- or oxygen-rich upper atmospheres. Expand
Isotopic constraints on the origin and nature of primitive material in the Solar System and on early Earth
The Earth formed some 4.5 Ga from the accumulation of dust, rocks and gas. The composition of these primitive materials is today recorded in meteorites. However, the origin of volatile elementsExpand
Accretion of the Earth and segregation of its core
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
Outgassing History and Escape of the Martian Atmosphere and Water Inventory
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
Origin and solar activity driven evolution of Mars' atmosphere
The evolution of the martian atmosphere and its H2O inventory can be divided into early and late evolutionary epochs. Volatiles such as H2O and CO2 could have built up a dense water vapour dominatedExpand
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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