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The ultraviolet spectra of carbonaceous chondrites
Celestial Mechanics and Dynamical Astronomy, 1992Optical spectroscopy of meteorites is an important laboratory tool for the study of the origin and evolution of solar and galactic interstellar minor bodies. In the region from the visible to the ultraviolet, the absorption spectra have hitherto been measured on the Bruderheim (Egan and Hilgeman, 1975), the Orgueil (Huffman, 1977), the Murchison ...
T. Inagaki, S. Yabushita, K. Wada
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On the origins of organic matter in carbonaceous chondrites [PDF]
Pure and Applied Chemistry, 1993 Abstract
Reisse, Jacques, Mullie, Françoise C.
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A search for C60 in carbonaceous chondrites
Geochimica et Cosmochimica Acta, 1993Analysis of interior samples of the Murchison meteorite by two routes yielded an upper limit of 2 ppb for its C60 content, as compared to parts per million levels for individual polycyclic aromatic hydrocarbons (PAHs). Provided the samples contain an interstellar component, which is probable since Murchison hydrocarbons contain excess deuterium, this ...
M S, De Vries +7 more
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Deuterium in carbonaceous chondrites
Earth and Planetary Science Letters, 1980Hydrogen isotopic compositions in seven carbonaceous chondrites lie in the range -70 to +771 per thousand relative to standard mean ocean water. These values decrease, to a range from -145 to +219 per thousand, after low-temperature oxidation in an oxygen plasma.
Y KOLODNY, J KERRIDGE, I KAPLAN
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Xenon in Carbonaceous Chondrites
Nature Physical Science, 1972Carbonaceous chondrites contain two isotopically distinct components of trapped xenon which cannot be explained by the occurrence of nuclear or fractionation processes within these meteorites.
O. K. MANUEL, E. W. HENNECKE, D. D. SABU
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Amino Acids in an Antarctic Carbonaceous Chondrite
Science, 1979Amino acids have been found in aqueous extracts of a C2 carbonaceous chondrite recovered from Antarctica. The composition of the amino acids strongly suggests that they have a meteoritic origin. Comparison of these results with those obtained with other C2 chondrites supports the view that Antarctic meteorites have not been significantly altered by ...
J R, Cronin, S, Pizzarello, C B, Moore
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Space Science Reviews, 1963
The carbonaceous chondrites are a group of stony meteorites characterized by the presence of an appreciable amount of carbonaceous material other than free carbon (diamond and graphite). They have been divided into three subgroups known respectively as Type I, Type II, and Type III.
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The carbonaceous chondrites are a group of stony meteorites characterized by the presence of an appreciable amount of carbonaceous material other than free carbon (diamond and graphite). They have been divided into three subgroups known respectively as Type I, Type II, and Type III.
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Organic Matter in Carbonaceous Chondrites
1986Carbonaceous chondrites are objects of great interest for chemists and astrophysicists. They contain a large number of abiogenic organic molecules and they are fragments of the least metamorphized bodies which exist in the solar system. Therefore, the study of carbonaceous chondrites affords information about the state of matter 4.5 Gyr ago.
Françoise Mullie, Jacques Reisse
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Atlas of bacteriomorphs in carbonaceous chondrites
SPIE Proceedings, 2004During the past few years, there has appeared much new and interesting data concerning the distribution of bacteriomorphic structures in both meteorites (carbonaceous chondrites) and in Earth rocks of different ages (Achaean to Recent). The bacterial forms studied are of very diverse morphologies including cocci, filaments, rod-shaped forms, etc.
Alexei Y. Rozanov, Richard B. Hoover
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Boron in Carbonaceous Chondrites
Nature, 1968BORON is remarkable in that its compounds are common and inexpensive although the element occurs quite low on the cosmic abundance scale, alongside lithium and beryllium. The cosmic scarcity of these three light elements is related to the ease with which their nuclei are disintegrated during nucleogenesis, whereas the terrestrial familiarity of borates
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