Orbital evolution of impact ejecta from Mars

Details Orbital evolution of impact ejecta from Mars Orbital evolution of impact ejecta from Mars

Mar 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984metic..19....1w&link_type=abstract

Meteoritics (ISSN 0026-1114), vol. 19, March 31, 1984, p. 1-13.

Computer Science

45

Achondrites, Ejecta, Impact Acceleration, Mars Craters, Orbit Calculation, Solar Orbits, Escape Velocity, Hypervelocity Impact, Meteorite Collisions, Radioactive Age Determination, Mars, Orbits, Evolution, Impacts, Ejecta, Origin, Source, Meteorites, Shergotty, Makhlite, Chassigny, Achondrites, Models, Comparisons, Collisions, Parent Bodies, Fragmentation, Velocity, Escape, Flux, Snc Meteorites, Exposure Age, Eeta 79001, Elephant Moraine Meteorites, Antarctic Meteorites, Mercury (Planet)

Scientific paper

The orbital evolution of material ejected from Mars into heliocentric orbits is investigated, with emphasis on the origin of the shergottite, nakhlite, and chassignite achondrites. Two models are considered. In the first, meteorite-size bodies are ejected directly from Mars. In the second, the ejecta are approximately 15 m diameter bodies, that are subsequently fragmented by collisions in space. In both cases about 35 percent of the objects that will ever reach earth do so within 10 m y. For the small body model, it is found that about 0.03 percent of the Mars crater ejecta must be accelerated to the Mars escape velocity; the large body model requires an efficiency of 0.4 percent. The results indicate that meteorites originating as small bodies should dominate the terrestrial flux of Mars ejecta. This is in general agreement with data from SNC meteorites. The yield of meteorites from Mercury is found to be at least a factor of 100 lower than from Mars.

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