Growth mechanism and additional constraints on FeNi metal condensation in the solar nebula

Details Growth mechanism and additional constraints on FeNi metal condensation in the solar nebula Growth mechanism and additional constraints on FeNi metal condensation in the solar nebula

Dec 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001jgr...10632797m&link_type=abstract

Journal of Geophysical Research, Volume 106, Issue E12, p. 32797-32802

Physics

11

Mineralogy And Petrology, Mineralogy And Petrology: Meteorites, Mineralogy And Petrology: Mineral Occurrences And Deposits, Planetology: Solar System Objects: Asteroids And Meteoroids

Scientific paper

Chemically zoned FeNi metal grains in the metal-rich chondrites QUE 94411 and Hammadah at Hamra 237 formed by gas-solid condensation in the temperature range from ~1500 to 1400 K during highly energetic thermal events in the solar nebula. We observe a linear correlation between the apparent diameter of the zoned FeNi metal grains and their inferred condensation temperature interval, which indicates that the grain growth rate was essentially constant. This lends strong support for a kinetic ``hit-and-stick'' growth model that yields growth timescales of ~20-85 hours and gas cooling rates of ~1-2 Kh-1 for six representative zoned metal grains studied in QUE 94411. In the core regions of the zoned metal grains the Ni concentration is systematically lower than the thermodynamically predicted values, suggesting that solid-state diffusion played an important role in shaping the zoning profiles. Combined with existing data, our observations provide a set of constraints on the physics and chemistry of large-scale, high-temperature processes in the earliest solar nebula, which present astrophysicists with profound challenges.

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