Computer Science
Scientific paper
Jan 1998
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998lpico.957....9g&link_type=abstract
Origin of the Earth and Moon, Proceedings of the Conference held 1-3 December, 1998 in Monterey, California. LPI Contribution N
Computer Science
Atmospheric Composition, Degassing, Impact Velocity, Protoplanets, Trapping, Water, Primitive Earth Atmosphere, Planetary Evolution, Planetary Environments, Carbon Dioxide, Hydrocarbons, Planetary Mass, Silicates, Sulfur Dioxides, Atmospheric Models
Scientific paper
The Earth's primordial atmosphere is considered to be the result of impact degassing during planetary accretion. Experiments on the decomposition of a serpentine and calcite during a shock wave loading showed that a rather efficient decomposition could be achieved beginning with the impact velocities that corresponded to escape velocities of a relatively small (about Moon-sized) planetary embryo. During further accumulation of planetary mass, the decomposition of serpentine and carbonates with the release of H2O and CO2 (gases considered to be the main product of impact degassing) into the primordial atmosphere was considered to be complete. The sink rate of H2O and CO2 from the primordial atmosphere was evaluated mainly as atmospheric impact erosion, thermal and EW-driven escape from the atmosphere, hydration and carboniza60n of surface minerals, dissolution of gases in magma ocean, loss of water for oxidation of Fe, etc. The growth of the atmosphere was considered to be a result of source and sink processes during each impact event. The rehydration of 100% of degassed material during an impact is considered to be an end effect when no hydrous atmosphere is formed. But even a small efficiency of impact degassing (the ratio of volatiles that remain in the atmosphere after an impact to the amount delivered by a planetesimal) was calculated to produce an abundant H2O-CO2 atmosphere. During a set of impact simulation experiments we have investigated the chemistry of volatiles and their interaction behavior with condensing silicates at conditions similar to impact vaporization. First, the experiments showed that the gas mixture was not limited only by H20 and CO2 during high-temperature vaporization of silicates, a wide variety of gases were formed, including oxides [SO2, CO2, CO (CO/CO2 approximately 1), H20] and reduced gas components (H2, H2S, CS2, COS, and hydrocarbons). Second, experiments on high-temperature vaporization of mafic and ultramafic rocks and minerals in water and/or CO2 containing atmospheres showed that condensing silicates provide intense trapping of water and/or CO2 during the hot stage of vapor cloud expansion. The amount of water trapped by formation of different hydroxides could be about 10 wt% of silicate mass. The trapping of atmospheric CO2 is proceeded by the formation of carbonates, carbides, hydrocarbons, and elemental C phases. Preliminary results indicate that Ni is also trapped by formation of -NO3, -H2N, and -CN phases. The maximum concentrations of trapped CO2 and N were measured up to 4 wt% and 0.1 wt% respectively. Trapping is efficient even at low partial gas pressures. Impact-induced trapping of atmospheric gases was not accounted for by theoretical models, but it seems to be an efficient process controlling the atmospheric mass. The ratio of volatiles added to the atmosphere after an impact to the amount delivered by a planetesimal can only be positive but sufficiently negative as well. During the impact of a planetesimal analogous to an ordinary chondrite on the growing Earth with a dense atmosphere, the removal of gases from the atmosphere seems to be more probable as a result of release and trapping processes. The capacity of the sink buffer exceeds the whole planetary volatile inventory. The trapping efficiency of gases inside the vapor plume suggests a model for the formation of a primordial atmosphere of moderate density.
Dikov Yu. P.
Gerasimov M. V.
Wlotzka Frank
Yakovlev O. I.
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