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CI chondrites typically contain a high proportion of water (up to 22%),<ref name=norton /> and organic matter in the form of [[amino acid]]s<ref name=ehrenfreund>{{cite journal |last=Ehrenfreund |first=Pascale |author2=Daniel P. Glavin |author3=Oliver Botta |author4=George Cooper |author5=Jeffrey L. Bada |year=2001 |title=Extraterrestrial amino acids in Orgueil and Ivuna: Tracing the parent body of CI type carbonaceous chondrites |journal=Proceedings of the National Academy of Sciences |volume=98 |issue=5 |pages=2138–2141 |doi=10.1073/pnas.051502898 |pmid=11226205 |pmc=30105|bibcode = 2001PNAS...98.2138E |doi-access=free }}</ref> and [[Polycyclic aromatic hydrocarbon|PAH]]s.<ref>{{cite journal |last=Wing |first=Michael R. |author2=Jeffrey L. Bada |year=1992 |title=The origin of the polycyclic aromatic hydrocarbons in meteorites |journal=Origins of Life and Evolution of the Biosphere |volume=21 |issue=5–6 |pages=375–383 |doi=10.1007/BF01808308 |bibcode = 1991OLEB...21..375W |s2cid=11504324 }}</ref> Aqueous alteration promotes a composition of hydrous [[Silicate minerals#Phyllosilicates|phyllosilicate]]s, [[magnetite]], and [[olivine]] crystals occurring in a black matrix, and a possible lack of [[chondrule]]s. It is thought they have not been heated above {{convert|50|°C|°F|abbr=on}}, indicating that they condensed in the cooler outer portion of the solar nebula. |
CI chondrites typically contain a high proportion of water (up to 22%),<ref name=norton /> and organic matter in the form of [[amino acid]]s<ref name=ehrenfreund>{{cite journal |last=Ehrenfreund |first=Pascale |author2=Daniel P. Glavin |author3=Oliver Botta |author4=George Cooper |author5=Jeffrey L. Bada |year=2001 |title=Extraterrestrial amino acids in Orgueil and Ivuna: Tracing the parent body of CI type carbonaceous chondrites |journal=Proceedings of the National Academy of Sciences |volume=98 |issue=5 |pages=2138–2141 |doi=10.1073/pnas.051502898 |pmid=11226205 |pmc=30105|bibcode = 2001PNAS...98.2138E |doi-access=free }}</ref> and [[Polycyclic aromatic hydrocarbon|PAH]]s.<ref>{{cite journal |last=Wing |first=Michael R. |author2=Jeffrey L. Bada |year=1992 |title=The origin of the polycyclic aromatic hydrocarbons in meteorites |journal=Origins of Life and Evolution of the Biosphere |volume=21 |issue=5–6 |pages=375–383 |doi=10.1007/BF01808308 |bibcode = 1991OLEB...21..375W |s2cid=11504324 }}</ref> Aqueous alteration promotes a composition of hydrous [[Silicate minerals#Phyllosilicates|phyllosilicate]]s, [[magnetite]], and [[olivine]] crystals occurring in a black matrix, and a possible lack of [[chondrule]]s. It is thought they have not been heated above {{convert|50|°C|°F|abbr=on}}, indicating that they condensed in the cooler outer portion of the solar nebula. |
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Five CI chondrites have been observed to fall: [[Ivuna meteorite|Ivuna]], [[Orgueil (meteorite)|Orgueil]], [[Alais meteorite|Alais]], [[Tonk meteorite|Tonk]], and [[Revelstoke meteorite|Revelstoke]]. |
Five CI chondrites have been observed to fall: [[Ivuna meteorite|Ivuna]], [[Orgueil (meteorite)|Orgueil]], [[Alais meteorite|Alais]], [[Tonk meteorite|Tonk]], and [[Revelstoke meteorite|Revelstoke]]. Several others have been found by Japanese field parties in Antarctica. In general, the extreme fragility of CI chondrites causes them to be highly susceptible to terrestrial weathering, and they do not survive on Earth's surface for long after they fall. |
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===CV group=== |
===CV group=== |
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