Chemical and isotopic fractionation by grain size separates

Details Chemical and isotopic fractionation by grain size separates Chemical and isotopic fractionation by grain size separates

Apr 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980e%26psl..47..199c&link_type=abstract

Earth and Planetary Science Letters, vol. 47, no. 2, Apr. 1980, p. 199-210. Research supported by the Max-Planck-Institut für K

Physics

22

Chemical Fractionation, Interstellar Matter, Isotope Separation, Particle Size Distribution, Size Separation, Aluminum, Chemical Evolution, Cosmic Dust, Meteoritic Composition, Rare Earth Elements, Solar System, Chemistry, Isotopes, Fractionation, Grain Size, Refractory Elements, Models, Condensation, Accretion, Dust, Gases, Aluminum/Magnesium, Enrichment, Rare Earth Elements, Anomalies, Ages, Xenon 129, Data, Iodine 127, Calcium/Aluminum, Meteorites, C3 Meteorites, Inclusions, Cosmic Dust, Solar System, Fo

Scientific paper

Fractionation of refractory elements according to grain size is argued to occur during their growth. Two major modes should exist: (1) during thermal condensation sequences whenever the condensing phase (e.g. Mg2SiO4) does not alloy with the precondensed phase (e.g. MgAl2O4); (2) during accretion of gaseous atoms in the nonequilibrated interstellar medium. Processes dynamically sorting grains according to size (e.g. sedimentation) therefore are potentially capable of achieving fractionations normally attributed to separations of dust and gas. This paper considers the first mode during supernova condensation; however, it also can occur in an equilibrium solar condensation sequence owing to an overlooked freedom in that simplified description.

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