Amino acids in Antarctic CM1 meteorites and their relationship to other carbonaceous chondrites
Abstract— CM2 carbonaceous chondrites are the most primitive material present in the solar system, and some of their subtypes, the CM and CI chondrites, contain up to 2 wt% of organic carbon. The CM2 carbonaceous chondrites contain a wide variety of complex amino acids, while the CI1 meteorites Orgu...
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crwiley:10.1111/j.1945-5100.2007.tb00219.x 2024-09-30T14:26:43+00:00 Amino acids in Antarctic CM1 meteorites and their relationship to other carbonaceous chondrites BOTTA, Oliver MARTINS, Zita EHRENFREUND, Pascale 2007 http://dx.doi.org/10.1111/j.1945-5100.2007.tb00219.x https://api.wiley.com/onlinelibrary/tdm/v1/articles/10.1111%2Fj.1945-5100.2007.tb00219.x https://onlinelibrary.wiley.com/doi/pdf/10.1111/j.1945-5100.2007.tb00219.x en eng Wiley http://onlinelibrary.wiley.com/termsAndConditions#vor Meteoritics & Planetary Science volume 42, issue 1, page 81-92 ISSN 1086-9379 1945-5100 journal-article 2007 crwiley https://doi.org/10.1111/j.1945-5100.2007.tb00219.x 2024-09-19T04:19:18Z Abstract— CM2 carbonaceous chondrites are the most primitive material present in the solar system, and some of their subtypes, the CM and CI chondrites, contain up to 2 wt% of organic carbon. The CM2 carbonaceous chondrites contain a wide variety of complex amino acids, while the CI1 meteorites Orgueil and Ivuna display a much simpler composition, with only glycine and β‐alanine present in significant abundances. CM1 carbonaceous chondrites show a higher degree of aqueous alteration than CM2 types and therefore provide an important link between the CM2 and CI1 carbonaceous chondrites. Relative amino acid concentrations have been shown to be indicative for parent body processes with respect to the formation of this class of compounds. In order to understand the relationship of the amino acid composition between these three types of meteorites, we have analyzed for the first time three Antarctic CM1 chondrites, Meteorite Hills (MET) 01070, Allan Hills (ALH) 88045, and LaPaz Icefield (LAP) 02277, using gas chromatography‐mass spectrometry (GC‐MS) and high performance liquid chromatography‐fluorescence detection (HPLC‐FD). The concentrations of the eight most abundant amino acids in these meteorites were compared to those of the CM2s Murchison, Murray, Mighei, Lewis Cliff (LEW) 90500, ALH 83100, as well as the CI1s Orgueil and Ivuna. The total amino acid concentration in CM1 carbonaceous chondrites was found to be much lower than the average of the CM2s. Relative amino acid abundances were compared in order to identify synthetic relationships between the amino acid compositions in these meteorite classes. Our data support the hypothesis that amino acids in CM‐ and CI‐type meteorites were synthesized under different physical and chemical conditions and may best be explained with differences in the abundances of precursor compounds in the source regions of their parent bodies in combination with the decomposition of amino acids during extended aqueous alteration. Article in Journal/Newspaper Antarc* Antarctic Wiley Online Library Antarctic Allan Hills ENVELOPE(159.667,159.667,-76.717,-76.717) Murchison ENVELOPE(144.250,144.250,-67.317,-67.317) Lewis Cliff ENVELOPE(161.083,161.083,-84.283,-84.283) Meteorite Hills ENVELOPE(155.600,155.600,-79.667,-79.667) Meteoritics & Planetary Science 42 1 81 92 |
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Open Polar |
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Wiley Online Library |
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crwiley |
language |
English |
description |
Abstract— CM2 carbonaceous chondrites are the most primitive material present in the solar system, and some of their subtypes, the CM and CI chondrites, contain up to 2 wt% of organic carbon. The CM2 carbonaceous chondrites contain a wide variety of complex amino acids, while the CI1 meteorites Orgueil and Ivuna display a much simpler composition, with only glycine and β‐alanine present in significant abundances. CM1 carbonaceous chondrites show a higher degree of aqueous alteration than CM2 types and therefore provide an important link between the CM2 and CI1 carbonaceous chondrites. Relative amino acid concentrations have been shown to be indicative for parent body processes with respect to the formation of this class of compounds. In order to understand the relationship of the amino acid composition between these three types of meteorites, we have analyzed for the first time three Antarctic CM1 chondrites, Meteorite Hills (MET) 01070, Allan Hills (ALH) 88045, and LaPaz Icefield (LAP) 02277, using gas chromatography‐mass spectrometry (GC‐MS) and high performance liquid chromatography‐fluorescence detection (HPLC‐FD). The concentrations of the eight most abundant amino acids in these meteorites were compared to those of the CM2s Murchison, Murray, Mighei, Lewis Cliff (LEW) 90500, ALH 83100, as well as the CI1s Orgueil and Ivuna. The total amino acid concentration in CM1 carbonaceous chondrites was found to be much lower than the average of the CM2s. Relative amino acid abundances were compared in order to identify synthetic relationships between the amino acid compositions in these meteorite classes. Our data support the hypothesis that amino acids in CM‐ and CI‐type meteorites were synthesized under different physical and chemical conditions and may best be explained with differences in the abundances of precursor compounds in the source regions of their parent bodies in combination with the decomposition of amino acids during extended aqueous alteration. |
format |
Article in Journal/Newspaper |
author |
BOTTA, Oliver MARTINS, Zita EHRENFREUND, Pascale |
spellingShingle |
BOTTA, Oliver MARTINS, Zita EHRENFREUND, Pascale Amino acids in Antarctic CM1 meteorites and their relationship to other carbonaceous chondrites |
author_facet |
BOTTA, Oliver MARTINS, Zita EHRENFREUND, Pascale |
author_sort |
BOTTA, Oliver |
title |
Amino acids in Antarctic CM1 meteorites and their relationship to other carbonaceous chondrites |
title_short |
Amino acids in Antarctic CM1 meteorites and their relationship to other carbonaceous chondrites |
title_full |
Amino acids in Antarctic CM1 meteorites and their relationship to other carbonaceous chondrites |
title_fullStr |
Amino acids in Antarctic CM1 meteorites and their relationship to other carbonaceous chondrites |
title_full_unstemmed |
Amino acids in Antarctic CM1 meteorites and their relationship to other carbonaceous chondrites |
title_sort |
amino acids in antarctic cm1 meteorites and their relationship to other carbonaceous chondrites |
publisher |
Wiley |
publishDate |
2007 |
url |
http://dx.doi.org/10.1111/j.1945-5100.2007.tb00219.x https://api.wiley.com/onlinelibrary/tdm/v1/articles/10.1111%2Fj.1945-5100.2007.tb00219.x https://onlinelibrary.wiley.com/doi/pdf/10.1111/j.1945-5100.2007.tb00219.x |
long_lat |
ENVELOPE(159.667,159.667,-76.717,-76.717) ENVELOPE(144.250,144.250,-67.317,-67.317) ENVELOPE(161.083,161.083,-84.283,-84.283) ENVELOPE(155.600,155.600,-79.667,-79.667) |
geographic |
Antarctic Allan Hills Murchison Lewis Cliff Meteorite Hills |
geographic_facet |
Antarctic Allan Hills Murchison Lewis Cliff Meteorite Hills |
genre |
Antarc* Antarctic |
genre_facet |
Antarc* Antarctic |
op_source |
Meteoritics & Planetary Science volume 42, issue 1, page 81-92 ISSN 1086-9379 1945-5100 |
op_rights |
http://onlinelibrary.wiley.com/termsAndConditions#vor |
op_doi |
https://doi.org/10.1111/j.1945-5100.2007.tb00219.x |
container_title |
Meteoritics & Planetary Science |
container_volume |
42 |
container_issue |
1 |
container_start_page |
81 |
op_container_end_page |
92 |
_version_ |
1811632835281289216 |