Impact versus internal origins for mesosiderites

Details Impact versus internal origins for mesosiderites Impact versus internal origins for mesosiderites

Nov 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983lpsc...14..257h&link_type=abstract

(American Geophysical Union and NASA, Lunar and Planetary Science Conference, 14th, Houston, TX, Mar. 14-18, 1983) Journal of Ge

Physics

3

Hypervelocity Impact, Iron Meteorites, Meteoritic Composition, Stony-Iron Meteorites, Chemical Composition, Cores, Cosmochemistry, Crusts, Deposition, Evolution (Development), Mathematical Models, Petrology, Stony Meteorites, Temperature Effects, Textures, Meteorites, Stony-Iron Meteorites, Mesosiderites, Origin, Formation, Breccias, Cooling, Impacts, Parent Bodies, Size, Models, Mineralogy, Hypotheses, Texture, Temperature, Thermal Effects, Thermal History, Cratering, Segregation, Diagrams, Accretion, Core

Scientific paper

The textures, mineral compositions, and thermal history of mesosiderites are examined to see whether they are compatible with any kind of impact process or internal process which might produce stony-iron breccias. It was proposed that cratering by metal projectiles is not an adequate origin mechanism since it would not deposit enough metal in the stony-iron breccias. It was also proposed that such mechanisms as accretion of differentiated planitesimals must be considered for mesosiderite origins. But no single model for origins is fully satisfactory. Disruption and reassembly of two colliding bodies could form stony-iron breccias at depth, but, as with the previous models, the easiest way to explain the low olivine of mesosiderites is to postulate derivation from olivine-poor chondritic material. Turbulent metal-crust mixing during core formation and crustal blocks sinking into the core withhold olivine from the breccia but do not explain how the silicate and metal liquids in subgroup IV could have failed to segregate.

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