Lecture5

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Unformatted text preview: se most meteorites come from shattered asteroids • Stony - silicate rock, varying amounts of metal, former asteroid crust/mantle • Metallic - mostly Fe-Ni metal, former asteroid core • Carbonaceous - primitive, unprocessed solar nebula material • Silicates, organic compounds (amino acids, hydrocarbons, saccharides, etc.) Silicates, • Icy - rare in Asteroid Belt, objects made mostly of ice • Probably from outer solar system originally, captured comets or Kuiper objects Probably Asteroids 951 Gaspra (~18 km) Ceres (950 km) (950 Meteorites ! ! ! Largely, meteorites are residue from Solar System formation and condensation Comprise a wide range of compositions, which formed at various epochs in our system’s early history Chondrites • • • ! Achondrites • • • ! Partially differentiated meteorites May derive from planetoids that underwent partial chemical differentiation Differ in mineral composition Irons • ! Most common type of meteorite, date to 4.5 Ga Most Undifferentiated, congealed directly by condensation from solar nebula Relative concentrations of elements is close to solar (sans H, He) Thought to derive from earliest phases of solar nebula condensation, or from cores of differentiated planetoids that were subsequently shattered by impact Carbonaceous Chondrites • • Most primitive meteorites, fairly rare Contain abundant organic carbon, amino acids, hydrocarbons… r...
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This document was uploaded on 04/05/2014.

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