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Chemistry of the solar nebula

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Abstract

The composition, mineralogy and texture of chondritic meteorites suggest they are relatively unaltered relicts of the condensation and accretion processes which took place in the primitive solar nebula. Chondrites thus are thought to contain a unique record of the physico-chemical conditions which prevailed at the time and place (asteroid belt) of their origin. Elemental abundance patterns are an important clue to the events and processes. Most elements can be placed in one of four groups according to their observed fractionation behavior in chondritic material: refractory, siderophile, normally depleted and strongly depleted. This grouping can be explained in terms of four events which presumably took place during cooling, condensation and accretion in the nebula. In order of inferred occurrence these are: (1) partial loss of the initial condensates rich in refractory elements at T > 1300K, (2) partial loss of metallic Fe-Ni grains, perhaps because they were magnetic, at 1000 to 700K, (3) partial remelting and outgassing of the condensate (chondrule formation) at 600 to 350K, and (4) accretion, when the P-T conditions controlled the volatile content (500 to 350K). Total gas pressure at the time and place of accretion is estimated to fall between 10-−6 and 10−-4 atm.

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Authors and Affiliations

  1. Dept. of Geology and Center for Meteorite Studies, Arizona State University, 85281, Tempe, Ariz., U.S.A

    John W. Larimer

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  1. John W. Larimer
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Contribution No. 80, Center for Meteorite Studies.

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Larimer, J.W. Chemistry of the solar nebula. Space Sci Rev 15, 103–119 (1973). https://doi.org/10.1007/BF00172439

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