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NWA 1152 and Sahara 00182: New primitive carbonaceous chondrites with affinities to the CR and CV groups

Identifieur interne : 000977 ( Istex/Corpus ); précédent : 000976; suivant : 000978

NWA 1152 and Sahara 00182: New primitive carbonaceous chondrites with affinities to the CR and CV groups

Auteurs : Caroline L. Smith ; Sara S. Russell ; Matthieu Gounelle ; Richard C. Greenwood ; Ian A. Franchi

Source :

RBID : ISTEX:DCCF794ED51299F2F54BFD179C76C8E15545FA45

Abstract

Abstract— We have investigated the mineralogy, petrography, bulk chemistry, and light element isotope composition of the ungrouped chondrites North West Africa (NWA) 1152 and Sahara 00182.

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DOI: 10.1111/j.1945-5100.2004.tb00093.x

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ISTEX:DCCF794ED51299F2F54BFD179C76C8E15545FA45

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<p>Abstract— We have investigated the mineralogy, petrography, bulk chemistry, and light element isotope composition of the ungrouped chondrites North West Africa (NWA) 1152 and Sahara 00182.</p>
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<p>NWA 1152 contains predominantly type 1 porphyritic olivine (PO) and porphyritic olivinepyroxene (POP) chondrules. Chondrule silicates are magnesium‐rich (Fo98.8 ± 1.2, n = 36; Fs2.3 ± 2.1 Wo1.2 ± 0.3, n = 23). Matrix comprises ˜40 vol% of the sample and is composed of a micron sized silicate groundmass with larger silicate, sulfide, magnetite, and Fe‐Ni metal (Ni ˜50 wt%) grains. Phyllosilicates were not observed in the matrix. Refractory inclusions are rare (0.3 vol%) and are spinel pyroxene aggregates or amoeboid olivine aggregates; melilite is absent from the refractory inclusions. Sahara 00182 contains predominantly type 1 PO chondrules, POP chondrules are less common. Most chondrules contain blebs of, and are often rimmed with, Fe‐Ni metal and sulfide. Chondrule phenocrysts are magnesium‐rich (Fo92.2 ± 0.6, n = 129; Fs4.4 ± 1.8 Wo1.3 ± 1.1, n = 16). Matrix comprises ˜30 vol% of the meteorite and is predominantly sub‐micron silicates, with rare larger silicate gains. Matrix Fe‐Ni metal (mean Ni = 5.8 wt%) and sulfide grains are up to mm scale. No phyllosilicates were observed in the matrix. Refractory inclusions are rare (1.1 vol%) and melilite is absent. The oxygen isotope composition of NWA 1152 falls within the range of the CV chondrites with δ17O = −3.43%0 δ18O = 0.70%0 and is similar to Sahara 00182, δ17O = −3.89%0, δ18O = −0.19%0 (Grossman and Zipfel 2001).</p>
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<p>Based on mineralogical and petrographic characteristics, we suggest NWA 1152 and Sahara 00182 show many similarities with the CR chondrites, however, oxygen isotopes suggest affinity with the CVs. Thus, neither sample can be assigned to any of the currently known carbonaceous chondrite groups based on traditionally recognized characteristics. Both samples demonstrate the complexity of inter‐ and intra‐group relationships of the carbonaceous chondrites. Whatever their classification, N WA 1152 and Sahara 00182 represent a source of relatively pristine solar system material.</p>
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<b>Abstract—</b>
We have investigated the mineralogy, petrography, bulk chemistry, and light element isotope composition of the ungrouped chondrites North West Africa (NWA) 1152 and Sahara 00182.</p>
<p>NWA 1152 contains predominantly type 1 porphyritic olivine (PO) and porphyritic olivinepyroxene (POP) chondrules. Chondrule silicates are magnesium‐rich (Fo
<sub>98.8 ± 1.2</sub>
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<sub>2.3 ± 2.1</sub>
Wo
<sub>1.2 ± 0.3</sub>
, n = 23). Matrix comprises ˜40 vol% of the sample and is composed of a micron sized silicate groundmass with larger silicate, sulfide, magnetite, and Fe‐Ni metal (Ni ˜50 wt%) grains. Phyllosilicates were not observed in the matrix. Refractory inclusions are rare (0.3 vol%) and are spinel pyroxene aggregates or amoeboid olivine aggregates; melilite is absent from the refractory inclusions. Sahara 00182 contains predominantly type 1 PO chondrules, POP chondrules are less common. Most chondrules contain blebs of, and are often rimmed with, Fe‐Ni metal and sulfide. Chondrule phenocrysts are magnesium‐rich (Fo
<sub>92.2 ± 0.6</sub>
, n = 129; Fs
<sub>4.4 ± 1.8</sub>
Wo
<sub>1.3 ± 1.1</sub>
, n = 16). Matrix comprises ˜30 vol% of the meteorite and is predominantly sub‐micron silicates, with rare larger silicate gains. Matrix Fe‐Ni metal (mean Ni = 5.8 wt%) and sulfide grains are up to mm scale. No phyllosilicates were observed in the matrix. Refractory inclusions are rare (1.1 vol%) and melilite is absent. The oxygen isotope composition of NWA 1152 falls within the range of the CV chondrites with δ
<sup>17</sup>
O = −3.43%0 δ
<sup>18</sup>
O = 0.70%0 and is similar to Sahara 00182, δ
<sup>17</sup>
O = −3.89%0, δ
<sup>18</sup>
O = −0.19%0 (Grossman and Zipfel 2001).</p>
<p>Based on mineralogical and petrographic characteristics, we suggest NWA 1152 and Sahara 00182 show many similarities with the CR chondrites, however, oxygen isotopes suggest affinity with the CVs. Thus, neither sample can be assigned to any of the currently known carbonaceous chondrite groups based on traditionally recognized characteristics. Both samples demonstrate the complexity of inter‐ and intra‐group relationships of the carbonaceous chondrites. Whatever their classification, N WA 1152 and Sahara 00182 represent a source of relatively pristine solar system material.</p>
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<p>Division of Earth Sciences, Centre for Geosciences, University of Glasgow, Gregory Building, Lilybank Gardens, Glasgow, G12 8QQ, UK</p>
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<title>NWA 1152 and Sahara 00182: New primitive carbonaceous chondrites with affinities to the CR and CV groups</title>
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<title>NWA 1152 and Sahara 00182: New primitive carbonaceous chondrites with affinities to the CR and CV groups</title>
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<name type="personal">
<namePart type="given">Caroline L.</namePart>
<namePart type="family">SMITH</namePart>
<affiliation>Department of Mineralogy, The Natural History Museum, Cromwell Road, London, SW7 5BD, UK</affiliation>
<description>Division of Earth Sciences, Centre for Geosciences, University of Glasgow, Gregory Building, Lilybank Gardens, Glasgow, G12 8QQ, UK</description>
<description>Correspondence: </description>
<role>
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<name type="personal">
<namePart type="given">Sara S.</namePart>
<namePart type="family">RUSSELL</namePart>
<affiliation>Department of Mineralogy, The Natural History Museum, Cromwell Road, London, SW7 5BD, UK</affiliation>
<role>
<roleTerm type="text">author</roleTerm>
</role>
</name>
<name type="personal">
<namePart type="given">Matthieu</namePart>
<namePart type="family">GOUNELLE</namePart>
<affiliation>Department of Mineralogy, The Natural History Museum, Cromwell Road, London, SW7 5BD, UK</affiliation>
<affiliation>Centre de Spectrométrie Nucléaire et de Spectrométrie de Masse, Université Paris 11, Bâtiment 104, 91405 Orsay Campus, France</affiliation>
<role>
<roleTerm type="text">author</roleTerm>
</role>
</name>
<name type="personal">
<namePart type="given">Richard C.</namePart>
<namePart type="family">GREENWOOD</namePart>
<affiliation>Planetary and Space Sciences Research Institute, The Open University, Walton Hall, Milton Keynes, Bucks, MK7 6AA, UK</affiliation>
<role>
<roleTerm type="text">author</roleTerm>
</role>
</name>
<name type="personal">
<namePart type="given">Ian A.</namePart>
<namePart type="family">FRANCHI</namePart>
<affiliation>Planetary and Space Sciences Research Institute, The Open University, Walton Hall, Milton Keynes, Bucks, MK7 6AA, UK</affiliation>
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<place>
<placeTerm type="text">Oxford, UK</placeTerm>
</place>
<dateIssued encoding="w3cdtf">2004-12</dateIssued>
<edition>Received 10 September 2003; revision accepted 4 October 2004</edition>
<copyrightDate encoding="w3cdtf">2004</copyrightDate>
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<languageTerm type="code" authority="iso639-2b">eng</languageTerm>
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<abstract>Abstract— We have investigated the mineralogy, petrography, bulk chemistry, and light element isotope composition of the ungrouped chondrites North West Africa (NWA) 1152 and Sahara 00182.</abstract>
<abstract>NWA 1152 contains predominantly type 1 porphyritic olivine (PO) and porphyritic olivinepyroxene (POP) chondrules. Chondrule silicates are magnesium‐rich (Fo98.8 ± 1.2, n = 36; Fs2.3 ± 2.1 Wo1.2 ± 0.3, n = 23). Matrix comprises ˜40 vol% of the sample and is composed of a micron sized silicate groundmass with larger silicate, sulfide, magnetite, and Fe‐Ni metal (Ni ˜50 wt%) grains. Phyllosilicates were not observed in the matrix. Refractory inclusions are rare (0.3 vol%) and are spinel pyroxene aggregates or amoeboid olivine aggregates; melilite is absent from the refractory inclusions. Sahara 00182 contains predominantly type 1 PO chondrules, POP chondrules are less common. Most chondrules contain blebs of, and are often rimmed with, Fe‐Ni metal and sulfide. Chondrule phenocrysts are magnesium‐rich (Fo92.2 ± 0.6, n = 129; Fs4.4 ± 1.8 Wo1.3 ± 1.1, n = 16). Matrix comprises ˜30 vol% of the meteorite and is predominantly sub‐micron silicates, with rare larger silicate gains. Matrix Fe‐Ni metal (mean Ni = 5.8 wt%) and sulfide grains are up to mm scale. No phyllosilicates were observed in the matrix. Refractory inclusions are rare (1.1 vol%) and melilite is absent. The oxygen isotope composition of NWA 1152 falls within the range of the CV chondrites with δ17O = −3.43%0 δ18O = 0.70%0 and is similar to Sahara 00182, δ17O = −3.89%0, δ18O = −0.19%0 (Grossman and Zipfel 2001).</abstract>
<abstract>Based on mineralogical and petrographic characteristics, we suggest NWA 1152 and Sahara 00182 show many similarities with the CR chondrites, however, oxygen isotopes suggest affinity with the CVs. Thus, neither sample can be assigned to any of the currently known carbonaceous chondrite groups based on traditionally recognized characteristics. Both samples demonstrate the complexity of inter‐ and intra‐group relationships of the carbonaceous chondrites. Whatever their classification, N WA 1152 and Sahara 00182 represent a source of relatively pristine solar system material.</abstract>
<relatedItem type="host">
<titleInfo>
<title>Meteoritics & Planetary Science</title>
</titleInfo>
<genre type="journal">journal</genre>
<identifier type="ISSN">1086-9379</identifier>
<identifier type="eISSN">1945-5100</identifier>
<identifier type="DOI">10.1111/(ISSN)1945-5100</identifier>
<identifier type="PublisherID">MAPS</identifier>
<part>
<date>2004</date>
<detail type="volume">
<caption>vol.</caption>
<number>39</number>
</detail>
<detail type="issue">
<caption>no.</caption>
<number>12</number>
</detail>
<extent unit="pages">
<start>2009</start>
<end>2032</end>
<total>24</total>
</extent>
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<identifier type="DOI">10.1111/j.1945-5100.2004.tb00093.x</identifier>
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<accessCondition type="use and reproduction" contentType="copyright">2004 The Meteoritical Society</accessCondition>
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