Abstract
Oxygen isotopic variations in carbonaceous chondrites and in ordinary chondrites can each be interpreted as mixtures of two isotopically different reservoirs, one consisting of solids, enriched in
16
O , the other of a gas, depleted in
16
O relative to terrestrial abundances. The data suggest a common source of the solids for each of the two classes of meteorites, but a different gas reservoir for each. These conditions might prevail in gaseous protoplanets. Radiogenic
26
Mg is variable in abundance among some classes of Allende inclusions, implying either nebular heterogeneity with respect to
26
A1/
27
Al ratios, or time differences of crystal formation of 1 or 2 x 10
6
a. The presence of excess
107
Ag from decay of extinct
107
Pd supports the evidence from
26
Mg for a time interval of at most a few million years between the last nucleosynthetic event and accretion of substantial bodies in the Solar System. The widespread small excess of
50
Ti in Allende inclusions is tantalizing, but unexplained. An exceptional hibonite-rich inclusion from Allende contains strongly fractionated isotopes of oxygen and calcium, but isotopically normal magnesium. Its trace elements imply association with a hot, oxidized gas. Among the volatile elements, neon-E has been shown to be essentially pure
22
Ne, and appears to be the decay product of extinct
22
Na. If so, condensation of some stellar ejecta must take place on a time scale of a year or so. The problem of reconciling the
26
A1 time scale of about 10
6
years between nucleosynthesis and Solar System condensation with the 10
8
year scale implied by the decay of
129
I to
129
Xe and fission of
244
Pu requires that at most a small fraction of the
129
I and
244
Pu be formed in the most recent event. Progress has been made in establishing the carrier phases of isotopically anomalous xenon and krypton. The apparent location of anomalous xenon and
14
N-rich nitrogen in identical carriers supports the notion that nucleosynthetic anomalies in nitrogen are also present in Allende.
Reference3 articles.
1. Interstellar Cloud Material: Contribution to Planetary Atmospheres
2. Geiss J. Buehler H. Cerutti P. E berhardt P. & Filleux G. 1972 15. W ashington D .C .: N.A.S.A.
3. J . geophys;Hoffman J .;Res.,1980
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