Other
Scientific paper
May 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011iaus..280e..18a&link_type=abstract
The Molecular Universe, Proceedings of the 280th Symposium of the International Astronomical Union held in Toledo, Spain, May 30
Other
Scientific paper
Chondritic meteorites formed in, and preserve a record of, the first few million years of Solar System history. Most, if not all, chondrites probably accreted some organic matter, but generally processes in their parent asteroids have destroyed or heavily modified it. In three groups (CI, CM, and CR), the organic matter has been reasonably well preserved. The organic matter in CI-CM-CRs is broadly divided into solvent soluble (SOM) and insoluble (IOM) fractions. The IOM (>70% of total organic C) is a structurally complex, macromolecular material composed of small aromatic moieties that are cross-linked by short, highly branched aliphatic chains. The aliphatic IR C-H stretch region of IOM is very similar to that of diffuse ISM dust. The abundance of IOM, up to ~2 wt% C, is equivalent to ~7% of cosmic C. IOM has a bulk composition of ~C100 H75 N3 O15, which is similar to the average of comet Halley CHON particles. In bulk, the IOM is significantly enriched in D and 15N. Even more extreme isotopic enrichments, that can overlap the range for simple gas phase ISM molecules, can be found in hotspots. Some hotspots are associated with spherical to irregular organic globules. Similar globules, isotopic hotspots and bulk isotopic enrichments are found in chondritic IDPs and comet Wild 2 samples, suggesting that there is a genetic link between organics in meteorites and comets. The SOM is a complex suite of compounds that include: amino acids, N-heterocycles, hydroxy acids, carboxylic acids, sulphonic and phosphonic acids, polyols, amines, amides, alcohols, aldehydes, ketones, and aliphatic and aromatic hydrocarbons. Concentrations range from hundreds of ppm to a few ppb. Many of these compounds show almost complete structural diversity for a given C number, and also have large enrichments in D and 15N. Some CI-CM-CRs contain α-dialkyl amino acids that do not readily racemize and that are not common terrestrial contaminants, but exhibit up to ~20% L-enantiomeric excesses that appear to be products of hydrothermal alteration. The origins of SOM and IOM have yet to be definitively established. The D and 15N isotopic enrichments point to synthesis in very cold environments, either in the early Solar System or in the protosolar MC. However, it is less clear whether it was the existing organic material or its precursors that formed there.
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