A Model of the Primordial Lunar Atmosphere

@article{Saxena2017AMO,
  title={A Model of the Primordial Lunar Atmosphere},
  author={P. Saxena and L. Elkins-Tanton and N. Petro and A. Mandell},
  journal={Earth and Planetary Science Letters},
  year={2017},
  volume={474},
  pages={198-205}
}
Abstract We create the first quantitative model for the early lunar atmosphere, coupled with a magma ocean crystallization model. Immediately after formation, the moon's surface was subject to a radiative environment that included contributions from the early Sun, a post-impact Earth that radiated like a mid-type M dwarf star, and a cooling global magma ocean. This radiative environment resulted in a largely Earth-side atmosphere on the Moon, ranging from ∼104 to ∼102 pascals, composed of heavy… Expand

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References

SHOWING 1-10 OF 46 REFERENCES
The Tethered Moon
Emergence of a Habitable Planet
Earthshine on a Young Moon: Explaining the Lunar Farside Highlands
LUNAR VOLATILE DEPLETION DUE TO INCOMPLETE ACCRETION WITHIN AN IMPACT-GENERATED DISK.
On lunar asymmetries 1. Tilted convection and crustal asymmetry
A multiple-impact origin for the Moon
...
1
2
3
4
5
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