Astronomy and Astrophysics – Astrophysics
Scientific paper
Sep 1987
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987apj...320..430t&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 320, Sept. 1, 1987, p. 430-436.
Astronomy and Astrophysics
Astrophysics
1
Condensing, Meteoritic Composition, Protostars, Solar Corona, Stellar Composition, Stellar Mass Ejection, Abundance, Cosmochemistry, Stellar Evolution, Stellar Models, T Tauri Stars, Meteorites, Chemistry, Condensation, Abundance, Solar Nebula, Models, Hypotheses, Temperature, Formation, Pressure, Gases, Flow, Minerals, Fractionation, Stony Meteorites, Ci Chondrites, Carbonaceous Chondrites, Thermometry, Barometry, Mass, Parameters, Carbon, Hydrogen, Cais, Inclusions, Enrichment, Aluminum, Anomalies
Scientific paper
For the past 20 years, cosmochemists have been interpreting meteoritic mineralogy in terms of chemical condensation in a hot and monotonically cooling solar nebula. However, there is some question as to whether the solar nebula was ever hot enough (>2000K) at the site of meteorite formation, 2 - 4 AU from the Sun. The author proposes an alternative model, which is based on the observations of nebular disks around young solar-type stars in their T Tauri phase and the evidence that these disks formed from the material condensed from the outflowing gases from these stars. Consequently, it is suggested that chemical condensation took place in the outflowing matter from the proto-Sun and that the solar nebula formed from this condensed material. The duration of the T Tauri phase is ≡106yr. During this period, the gas and the condensed dust would accumulate in the protosolar cavity to form the solar nebula. The characteristics of this nebula and the chemical condensation sequence in it are discussed.
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