The evolution of an impact-generated atmosphere

Details The evolution of an impact-generated atmosphere The evolution of an impact-generated atmosphere

Jul 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982icar...51...96l&link_type=abstract

Icarus, vol. 51, July 1982, p. 96-120. Research supported by the Rotary Foundation and Deutsche Forschungsgemeinschaft;

Astronomy and Astrophysics

Astronomy

51

Astronomical Models, Planetary Atmospheres, Planetary Evolution, Shock Wave Interaction, Thermodynamics, Water, Atmospheric Moisture, Chemical Composition, Chemical Evolution, Hydration, Impact Loads, Planetology

Scientific paper

The minimum impact velocities and pressures required to form a primary H2O atmosphere during planetary accretion from chondritelike planetessimals are determined by means of shock wave and thermodynamic data for rock-forming and volatile-bearing minerals. Attenuation of impact-induced shock pressure is modelled to the extent that the amount of released water can be estimated as a function of projectile radius, impact velocity, weight fraction of target water, target porosity, and dehydration efficiency. The two primary processes considered are the impact release of water bound in such hydrous minerals as serpentine, and the subsequent reincorporation of free water by hydration of forsterite and enstatite. These processes are described in terms of model calculations for the accretion of the earth. It is concluded that the concept of dehydration efficiency is of dominant importance in determining the degree to which an accreting planet acquires an atmosphere during its formation.

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