Mass-independent and mass-dependent Cr isotopic composition of the Rumuruti (R) chondrites: Implications for their origin and planet formation
Chromium (Cr) isotopes play an important role in cosmochemistry and planetary science because they are powerful tools for dating (53Mn–53Cr short-lived chronometry), tracing (54Cr nucleosynthetic anomalies) the origins of the materials, and studying the processes involved in volatile element fractio...
Ausführliche Beschreibung
Gespeichert in:
| Autor*in: |
Zhu (朱柯), Ke [verfasserIn] Moynier, Frédéric [verfasserIn] Schiller, Martin [verfasserIn] Alexander, Conel M.O'D. [verfasserIn] Barrat, Jean-Alix [verfasserIn] Bischoff, Addi [verfasserIn] Bizzarro, Martin [verfasserIn] |
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| Format: |
E-Artikel |
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| Sprache: |
Englisch |
| Erschienen: |
2020 |
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| Schlagwörter: |
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| Übergeordnetes Werk: |
Enthalten in: Geochimica et cosmochimica acta - New York, NY [u.a.] : Elsevier, 1950, 293, Seite 598-609 |
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| Übergeordnetes Werk: |
volume:293 ; pages:598-609 |
| DOI / URN: |
10.1016/j.gca.2020.10.007 |
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ELV005229383 |
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| 100 | 1 | |a Zhu (朱柯), Ke |e verfasserin |4 aut | |
| 245 | 1 | 0 | |a Mass-independent and mass-dependent Cr isotopic composition of the Rumuruti (R) chondrites: Implications for their origin and planet formation |
| 264 | 1 | |c 2020 | |
| 336 | |a nicht spezifiziert |b zzz |2 rdacontent | ||
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| 520 | |a Chromium (Cr) isotopes play an important role in cosmochemistry and planetary science because they are powerful tools for dating (53Mn–53Cr short-lived chronometry), tracing (54Cr nucleosynthetic anomalies) the origins of the materials, and studying the processes involved in volatile element fractionation and planetary differentiation (Cr stable isotopic fractionation). To use Cr isotopes for these purposes, it is essential to precisely know the compositions of the various chondritic reservoirs. However, the Cr isotope composition of Rumuruti (R) chondrites remains unknown. Here, we report high-precision mass-independent (average 2SE uncertainty of ∼0.02 and ∼0.06 for ε53Cr and ε54Cr, respectively; ε indicates 10,000 deviation) and mass-dependent (uncertainty of average 0.03‰ for δ53Cr; δ indicates 1000 deviation) Cr isotope data for 12 bulk R chondrites of petrologic types 3–6 (including R chondrite breccias), and one R chondrite-like clast (MS-CH) in the Almahata Sitta polymict ureilite. All the R chondrites show homogeneous bulk ε54Cr values, −0.06 ± 0.08 (2SD), similar only to those of the Earth–Moon system and enstatite chondrites. This first ε54Cr dataset for R chondrites provides significant addition to the ε54Cr–Δ17O diagram, and positions them as a potential endmember for planetary precursors. The R chondrites possess a higher 55Mn/52Cr of 0.68 ± 0.04 relative to most of carbonaceous chondrites and higher ε53Cr values 0.23 ± 0.05 (2SD) relative to most of chondrite groups. This likely results from the lower chondrule abundance in R chondrites compared to that of ordinary and enstatite chondrites. The stable Cr isotope composition of R chondrites is homogeneous with a δ53Cr = −0.12 ± 0.03‰ (2SD). Combined with previous data of other groups of chondrites, we show that the stable Cr isotopic composition of all the chondrites is homogeneous with δ53Cr of −0.12 ± 0.04‰ (2SD, N = 42) and is independent of the petrologic type and redox conditions. The lack of mass-dependent fractionation between all groups of chondrites suggests that the average chondrite δ53Cr value is also representative for the initial composition of all differentiated planets in the Solar System. Finally, the MS–CH clast in Almahata Sitta has a Cr isotopic composition (ε53Cr = 0.18 ± 0.04, ε54Cr = −0.16 ± 0.07, and δ53Cr = −0.11 ± 0.05‰) that is consistent (within error) with it being an R chondrite-like clast. | ||
| 650 | 4 | |a Rumuruti Chondrites | |
| 650 | 4 | |a Cr stable isotopes | |
| 650 | 4 | |a Chondritic clast | |
| 700 | 1 | |a Moynier, Frédéric |e verfasserin |4 aut | |
| 700 | 1 | |a Schiller, Martin |e verfasserin |4 aut | |
| 700 | 1 | |a Alexander, Conel M.O'D. |e verfasserin |4 aut | |
| 700 | 1 | |a Barrat, Jean-Alix |e verfasserin |4 aut | |
| 700 | 1 | |a Bischoff, Addi |e verfasserin |0 (orcid)0000-0002-7362-6712 |4 aut | |
| 700 | 1 | |a Bizzarro, Martin |e verfasserin |4 aut | |
| 773 | 0 | 8 | |i Enthalten in |t Geochimica et cosmochimica acta |d New York, NY [u.a.] : Elsevier, 1950 |g 293, Seite 598-609 |h Online-Ressource |w (DE-627)300898797 |w (DE-600)1483679-8 |w (DE-576)120883465 |x 0016-7037 |7 nnns |
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10.1016/j.gca.2020.10.007 doi (DE-627)ELV005229383 (ELSEVIER)S0016-7037(20)30639-6 DE-627 ger DE-627 rda eng 550 DE-600 38.32 bkl 39.29 bkl Zhu (朱柯), Ke verfasserin aut Mass-independent and mass-dependent Cr isotopic composition of the Rumuruti (R) chondrites: Implications for their origin and planet formation 2020 nicht spezifiziert zzz rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Chromium (Cr) isotopes play an important role in cosmochemistry and planetary science because they are powerful tools for dating (53Mn–53Cr short-lived chronometry), tracing (54Cr nucleosynthetic anomalies) the origins of the materials, and studying the processes involved in volatile element fractionation and planetary differentiation (Cr stable isotopic fractionation). To use Cr isotopes for these purposes, it is essential to precisely know the compositions of the various chondritic reservoirs. However, the Cr isotope composition of Rumuruti (R) chondrites remains unknown. Here, we report high-precision mass-independent (average 2SE uncertainty of ∼0.02 and ∼0.06 for ε53Cr and ε54Cr, respectively; ε indicates 10,000 deviation) and mass-dependent (uncertainty of average 0.03‰ for δ53Cr; δ indicates 1000 deviation) Cr isotope data for 12 bulk R chondrites of petrologic types 3–6 (including R chondrite breccias), and one R chondrite-like clast (MS-CH) in the Almahata Sitta polymict ureilite. All the R chondrites show homogeneous bulk ε54Cr values, −0.06 ± 0.08 (2SD), similar only to those of the Earth–Moon system and enstatite chondrites. This first ε54Cr dataset for R chondrites provides significant addition to the ε54Cr–Δ17O diagram, and positions them as a potential endmember for planetary precursors. The R chondrites possess a higher 55Mn/52Cr of 0.68 ± 0.04 relative to most of carbonaceous chondrites and higher ε53Cr values 0.23 ± 0.05 (2SD) relative to most of chondrite groups. This likely results from the lower chondrule abundance in R chondrites compared to that of ordinary and enstatite chondrites. The stable Cr isotope composition of R chondrites is homogeneous with a δ53Cr = −0.12 ± 0.03‰ (2SD). Combined with previous data of other groups of chondrites, we show that the stable Cr isotopic composition of all the chondrites is homogeneous with δ53Cr of −0.12 ± 0.04‰ (2SD, N = 42) and is independent of the petrologic type and redox conditions. The lack of mass-dependent fractionation between all groups of chondrites suggests that the average chondrite δ53Cr value is also representative for the initial composition of all differentiated planets in the Solar System. Finally, the MS–CH clast in Almahata Sitta has a Cr isotopic composition (ε53Cr = 0.18 ± 0.04, ε54Cr = −0.16 ± 0.07, and δ53Cr = −0.11 ± 0.05‰) that is consistent (within error) with it being an R chondrite-like clast. Rumuruti Chondrites Cr stable isotopes Chondritic clast Moynier, Frédéric verfasserin aut Schiller, Martin verfasserin aut Alexander, Conel M.O'D. verfasserin aut Barrat, Jean-Alix verfasserin aut Bischoff, Addi verfasserin (orcid)0000-0002-7362-6712 aut Bizzarro, Martin verfasserin aut Enthalten in Geochimica et cosmochimica acta New York, NY [u.a.] : Elsevier, 1950 293, Seite 598-609 Online-Ressource (DE-627)300898797 (DE-600)1483679-8 (DE-576)120883465 0016-7037 nnns volume:293 pages:598-609 GBV_USEFLAG_U SYSFLAG_U GBV_ELV SSG-OPC-GGO SSG-OPC-AST GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_150 GBV_ILN_151 GBV_ILN_224 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2027 GBV_ILN_2034 GBV_ILN_2038 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2056 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2118 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2190 GBV_ILN_2336 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4242 GBV_ILN_4251 GBV_ILN_4305 GBV_ILN_4313 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4326 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4393 38.32 Geochemie 39.29 Theoretische Astronomie: Sonstiges AR 293 598-609 |
| spelling |
10.1016/j.gca.2020.10.007 doi (DE-627)ELV005229383 (ELSEVIER)S0016-7037(20)30639-6 DE-627 ger DE-627 rda eng 550 DE-600 38.32 bkl 39.29 bkl Zhu (朱柯), Ke verfasserin aut Mass-independent and mass-dependent Cr isotopic composition of the Rumuruti (R) chondrites: Implications for their origin and planet formation 2020 nicht spezifiziert zzz rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Chromium (Cr) isotopes play an important role in cosmochemistry and planetary science because they are powerful tools for dating (53Mn–53Cr short-lived chronometry), tracing (54Cr nucleosynthetic anomalies) the origins of the materials, and studying the processes involved in volatile element fractionation and planetary differentiation (Cr stable isotopic fractionation). To use Cr isotopes for these purposes, it is essential to precisely know the compositions of the various chondritic reservoirs. However, the Cr isotope composition of Rumuruti (R) chondrites remains unknown. Here, we report high-precision mass-independent (average 2SE uncertainty of ∼0.02 and ∼0.06 for ε53Cr and ε54Cr, respectively; ε indicates 10,000 deviation) and mass-dependent (uncertainty of average 0.03‰ for δ53Cr; δ indicates 1000 deviation) Cr isotope data for 12 bulk R chondrites of petrologic types 3–6 (including R chondrite breccias), and one R chondrite-like clast (MS-CH) in the Almahata Sitta polymict ureilite. All the R chondrites show homogeneous bulk ε54Cr values, −0.06 ± 0.08 (2SD), similar only to those of the Earth–Moon system and enstatite chondrites. This first ε54Cr dataset for R chondrites provides significant addition to the ε54Cr–Δ17O diagram, and positions them as a potential endmember for planetary precursors. The R chondrites possess a higher 55Mn/52Cr of 0.68 ± 0.04 relative to most of carbonaceous chondrites and higher ε53Cr values 0.23 ± 0.05 (2SD) relative to most of chondrite groups. This likely results from the lower chondrule abundance in R chondrites compared to that of ordinary and enstatite chondrites. The stable Cr isotope composition of R chondrites is homogeneous with a δ53Cr = −0.12 ± 0.03‰ (2SD). Combined with previous data of other groups of chondrites, we show that the stable Cr isotopic composition of all the chondrites is homogeneous with δ53Cr of −0.12 ± 0.04‰ (2SD, N = 42) and is independent of the petrologic type and redox conditions. The lack of mass-dependent fractionation between all groups of chondrites suggests that the average chondrite δ53Cr value is also representative for the initial composition of all differentiated planets in the Solar System. Finally, the MS–CH clast in Almahata Sitta has a Cr isotopic composition (ε53Cr = 0.18 ± 0.04, ε54Cr = −0.16 ± 0.07, and δ53Cr = −0.11 ± 0.05‰) that is consistent (within error) with it being an R chondrite-like clast. Rumuruti Chondrites Cr stable isotopes Chondritic clast Moynier, Frédéric verfasserin aut Schiller, Martin verfasserin aut Alexander, Conel M.O'D. verfasserin aut Barrat, Jean-Alix verfasserin aut Bischoff, Addi verfasserin (orcid)0000-0002-7362-6712 aut Bizzarro, Martin verfasserin aut Enthalten in Geochimica et cosmochimica acta New York, NY [u.a.] : Elsevier, 1950 293, Seite 598-609 Online-Ressource (DE-627)300898797 (DE-600)1483679-8 (DE-576)120883465 0016-7037 nnns volume:293 pages:598-609 GBV_USEFLAG_U SYSFLAG_U GBV_ELV SSG-OPC-GGO SSG-OPC-AST GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_150 GBV_ILN_151 GBV_ILN_224 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2027 GBV_ILN_2034 GBV_ILN_2038 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2056 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2118 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2190 GBV_ILN_2336 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4242 GBV_ILN_4251 GBV_ILN_4305 GBV_ILN_4313 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4326 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4393 38.32 Geochemie 39.29 Theoretische Astronomie: Sonstiges AR 293 598-609 |
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10.1016/j.gca.2020.10.007 doi (DE-627)ELV005229383 (ELSEVIER)S0016-7037(20)30639-6 DE-627 ger DE-627 rda eng 550 DE-600 38.32 bkl 39.29 bkl Zhu (朱柯), Ke verfasserin aut Mass-independent and mass-dependent Cr isotopic composition of the Rumuruti (R) chondrites: Implications for their origin and planet formation 2020 nicht spezifiziert zzz rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Chromium (Cr) isotopes play an important role in cosmochemistry and planetary science because they are powerful tools for dating (53Mn–53Cr short-lived chronometry), tracing (54Cr nucleosynthetic anomalies) the origins of the materials, and studying the processes involved in volatile element fractionation and planetary differentiation (Cr stable isotopic fractionation). To use Cr isotopes for these purposes, it is essential to precisely know the compositions of the various chondritic reservoirs. However, the Cr isotope composition of Rumuruti (R) chondrites remains unknown. Here, we report high-precision mass-independent (average 2SE uncertainty of ∼0.02 and ∼0.06 for ε53Cr and ε54Cr, respectively; ε indicates 10,000 deviation) and mass-dependent (uncertainty of average 0.03‰ for δ53Cr; δ indicates 1000 deviation) Cr isotope data for 12 bulk R chondrites of petrologic types 3–6 (including R chondrite breccias), and one R chondrite-like clast (MS-CH) in the Almahata Sitta polymict ureilite. All the R chondrites show homogeneous bulk ε54Cr values, −0.06 ± 0.08 (2SD), similar only to those of the Earth–Moon system and enstatite chondrites. This first ε54Cr dataset for R chondrites provides significant addition to the ε54Cr–Δ17O diagram, and positions them as a potential endmember for planetary precursors. The R chondrites possess a higher 55Mn/52Cr of 0.68 ± 0.04 relative to most of carbonaceous chondrites and higher ε53Cr values 0.23 ± 0.05 (2SD) relative to most of chondrite groups. This likely results from the lower chondrule abundance in R chondrites compared to that of ordinary and enstatite chondrites. The stable Cr isotope composition of R chondrites is homogeneous with a δ53Cr = −0.12 ± 0.03‰ (2SD). Combined with previous data of other groups of chondrites, we show that the stable Cr isotopic composition of all the chondrites is homogeneous with δ53Cr of −0.12 ± 0.04‰ (2SD, N = 42) and is independent of the petrologic type and redox conditions. The lack of mass-dependent fractionation between all groups of chondrites suggests that the average chondrite δ53Cr value is also representative for the initial composition of all differentiated planets in the Solar System. Finally, the MS–CH clast in Almahata Sitta has a Cr isotopic composition (ε53Cr = 0.18 ± 0.04, ε54Cr = −0.16 ± 0.07, and δ53Cr = −0.11 ± 0.05‰) that is consistent (within error) with it being an R chondrite-like clast. Rumuruti Chondrites Cr stable isotopes Chondritic clast Moynier, Frédéric verfasserin aut Schiller, Martin verfasserin aut Alexander, Conel M.O'D. verfasserin aut Barrat, Jean-Alix verfasserin aut Bischoff, Addi verfasserin (orcid)0000-0002-7362-6712 aut Bizzarro, Martin verfasserin aut Enthalten in Geochimica et cosmochimica acta New York, NY [u.a.] : Elsevier, 1950 293, Seite 598-609 Online-Ressource (DE-627)300898797 (DE-600)1483679-8 (DE-576)120883465 0016-7037 nnns volume:293 pages:598-609 GBV_USEFLAG_U SYSFLAG_U GBV_ELV SSG-OPC-GGO SSG-OPC-AST GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_150 GBV_ILN_151 GBV_ILN_224 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2027 GBV_ILN_2034 GBV_ILN_2038 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2056 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2118 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2190 GBV_ILN_2336 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4242 GBV_ILN_4251 GBV_ILN_4305 GBV_ILN_4313 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4326 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4393 38.32 Geochemie 39.29 Theoretische Astronomie: Sonstiges AR 293 598-609 |
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10.1016/j.gca.2020.10.007 doi (DE-627)ELV005229383 (ELSEVIER)S0016-7037(20)30639-6 DE-627 ger DE-627 rda eng 550 DE-600 38.32 bkl 39.29 bkl Zhu (朱柯), Ke verfasserin aut Mass-independent and mass-dependent Cr isotopic composition of the Rumuruti (R) chondrites: Implications for their origin and planet formation 2020 nicht spezifiziert zzz rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Chromium (Cr) isotopes play an important role in cosmochemistry and planetary science because they are powerful tools for dating (53Mn–53Cr short-lived chronometry), tracing (54Cr nucleosynthetic anomalies) the origins of the materials, and studying the processes involved in volatile element fractionation and planetary differentiation (Cr stable isotopic fractionation). To use Cr isotopes for these purposes, it is essential to precisely know the compositions of the various chondritic reservoirs. However, the Cr isotope composition of Rumuruti (R) chondrites remains unknown. Here, we report high-precision mass-independent (average 2SE uncertainty of ∼0.02 and ∼0.06 for ε53Cr and ε54Cr, respectively; ε indicates 10,000 deviation) and mass-dependent (uncertainty of average 0.03‰ for δ53Cr; δ indicates 1000 deviation) Cr isotope data for 12 bulk R chondrites of petrologic types 3–6 (including R chondrite breccias), and one R chondrite-like clast (MS-CH) in the Almahata Sitta polymict ureilite. All the R chondrites show homogeneous bulk ε54Cr values, −0.06 ± 0.08 (2SD), similar only to those of the Earth–Moon system and enstatite chondrites. This first ε54Cr dataset for R chondrites provides significant addition to the ε54Cr–Δ17O diagram, and positions them as a potential endmember for planetary precursors. The R chondrites possess a higher 55Mn/52Cr of 0.68 ± 0.04 relative to most of carbonaceous chondrites and higher ε53Cr values 0.23 ± 0.05 (2SD) relative to most of chondrite groups. This likely results from the lower chondrule abundance in R chondrites compared to that of ordinary and enstatite chondrites. The stable Cr isotope composition of R chondrites is homogeneous with a δ53Cr = −0.12 ± 0.03‰ (2SD). Combined with previous data of other groups of chondrites, we show that the stable Cr isotopic composition of all the chondrites is homogeneous with δ53Cr of −0.12 ± 0.04‰ (2SD, N = 42) and is independent of the petrologic type and redox conditions. The lack of mass-dependent fractionation between all groups of chondrites suggests that the average chondrite δ53Cr value is also representative for the initial composition of all differentiated planets in the Solar System. Finally, the MS–CH clast in Almahata Sitta has a Cr isotopic composition (ε53Cr = 0.18 ± 0.04, ε54Cr = −0.16 ± 0.07, and δ53Cr = −0.11 ± 0.05‰) that is consistent (within error) with it being an R chondrite-like clast. Rumuruti Chondrites Cr stable isotopes Chondritic clast Moynier, Frédéric verfasserin aut Schiller, Martin verfasserin aut Alexander, Conel M.O'D. verfasserin aut Barrat, Jean-Alix verfasserin aut Bischoff, Addi verfasserin (orcid)0000-0002-7362-6712 aut Bizzarro, Martin verfasserin aut Enthalten in Geochimica et cosmochimica acta New York, NY [u.a.] : Elsevier, 1950 293, Seite 598-609 Online-Ressource (DE-627)300898797 (DE-600)1483679-8 (DE-576)120883465 0016-7037 nnns volume:293 pages:598-609 GBV_USEFLAG_U SYSFLAG_U GBV_ELV SSG-OPC-GGO SSG-OPC-AST GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_150 GBV_ILN_151 GBV_ILN_224 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2027 GBV_ILN_2034 GBV_ILN_2038 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2056 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2118 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2190 GBV_ILN_2336 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4242 GBV_ILN_4251 GBV_ILN_4305 GBV_ILN_4313 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4326 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4393 38.32 Geochemie 39.29 Theoretische Astronomie: Sonstiges AR 293 598-609 |
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10.1016/j.gca.2020.10.007 doi (DE-627)ELV005229383 (ELSEVIER)S0016-7037(20)30639-6 DE-627 ger DE-627 rda eng 550 DE-600 38.32 bkl 39.29 bkl Zhu (朱柯), Ke verfasserin aut Mass-independent and mass-dependent Cr isotopic composition of the Rumuruti (R) chondrites: Implications for their origin and planet formation 2020 nicht spezifiziert zzz rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Chromium (Cr) isotopes play an important role in cosmochemistry and planetary science because they are powerful tools for dating (53Mn–53Cr short-lived chronometry), tracing (54Cr nucleosynthetic anomalies) the origins of the materials, and studying the processes involved in volatile element fractionation and planetary differentiation (Cr stable isotopic fractionation). To use Cr isotopes for these purposes, it is essential to precisely know the compositions of the various chondritic reservoirs. However, the Cr isotope composition of Rumuruti (R) chondrites remains unknown. Here, we report high-precision mass-independent (average 2SE uncertainty of ∼0.02 and ∼0.06 for ε53Cr and ε54Cr, respectively; ε indicates 10,000 deviation) and mass-dependent (uncertainty of average 0.03‰ for δ53Cr; δ indicates 1000 deviation) Cr isotope data for 12 bulk R chondrites of petrologic types 3–6 (including R chondrite breccias), and one R chondrite-like clast (MS-CH) in the Almahata Sitta polymict ureilite. All the R chondrites show homogeneous bulk ε54Cr values, −0.06 ± 0.08 (2SD), similar only to those of the Earth–Moon system and enstatite chondrites. This first ε54Cr dataset for R chondrites provides significant addition to the ε54Cr–Δ17O diagram, and positions them as a potential endmember for planetary precursors. The R chondrites possess a higher 55Mn/52Cr of 0.68 ± 0.04 relative to most of carbonaceous chondrites and higher ε53Cr values 0.23 ± 0.05 (2SD) relative to most of chondrite groups. This likely results from the lower chondrule abundance in R chondrites compared to that of ordinary and enstatite chondrites. The stable Cr isotope composition of R chondrites is homogeneous with a δ53Cr = −0.12 ± 0.03‰ (2SD). Combined with previous data of other groups of chondrites, we show that the stable Cr isotopic composition of all the chondrites is homogeneous with δ53Cr of −0.12 ± 0.04‰ (2SD, N = 42) and is independent of the petrologic type and redox conditions. The lack of mass-dependent fractionation between all groups of chondrites suggests that the average chondrite δ53Cr value is also representative for the initial composition of all differentiated planets in the Solar System. Finally, the MS–CH clast in Almahata Sitta has a Cr isotopic composition (ε53Cr = 0.18 ± 0.04, ε54Cr = −0.16 ± 0.07, and δ53Cr = −0.11 ± 0.05‰) that is consistent (within error) with it being an R chondrite-like clast. Rumuruti Chondrites Cr stable isotopes Chondritic clast Moynier, Frédéric verfasserin aut Schiller, Martin verfasserin aut Alexander, Conel M.O'D. verfasserin aut Barrat, Jean-Alix verfasserin aut Bischoff, Addi verfasserin (orcid)0000-0002-7362-6712 aut Bizzarro, Martin verfasserin aut Enthalten in Geochimica et cosmochimica acta New York, NY [u.a.] : Elsevier, 1950 293, Seite 598-609 Online-Ressource (DE-627)300898797 (DE-600)1483679-8 (DE-576)120883465 0016-7037 nnns volume:293 pages:598-609 GBV_USEFLAG_U SYSFLAG_U GBV_ELV SSG-OPC-GGO SSG-OPC-AST GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_150 GBV_ILN_151 GBV_ILN_224 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2027 GBV_ILN_2034 GBV_ILN_2038 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2056 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2118 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2190 GBV_ILN_2336 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4242 GBV_ILN_4251 GBV_ILN_4305 GBV_ILN_4313 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4326 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4393 38.32 Geochemie 39.29 Theoretische Astronomie: Sonstiges AR 293 598-609 |
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Enthalten in Geochimica et cosmochimica acta 293, Seite 598-609 volume:293 pages:598-609 |
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Zhu (朱柯), Ke @@aut@@ Moynier, Frédéric @@aut@@ Schiller, Martin @@aut@@ Alexander, Conel M.O'D. @@aut@@ Barrat, Jean-Alix @@aut@@ Bischoff, Addi @@aut@@ Bizzarro, Martin @@aut@@ |
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<?xml version="1.0" encoding="UTF-8"?><collection xmlns="http://www.loc.gov/MARC21/slim"><record><leader>01000caa a22002652 4500</leader><controlfield tag="001">ELV005229383</controlfield><controlfield tag="003">DE-627</controlfield><controlfield tag="005">20230524142927.0</controlfield><controlfield tag="007">cr uuu---uuuuu</controlfield><controlfield tag="008">230504s2020 xx |||||o 00| ||eng c</controlfield><datafield tag="024" ind1="7" ind2=" "><subfield code="a">10.1016/j.gca.2020.10.007</subfield><subfield code="2">doi</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(DE-627)ELV005229383</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(ELSEVIER)S0016-7037(20)30639-6</subfield></datafield><datafield tag="040" ind1=" " ind2=" "><subfield code="a">DE-627</subfield><subfield code="b">ger</subfield><subfield code="c">DE-627</subfield><subfield code="e">rda</subfield></datafield><datafield tag="041" ind1=" " ind2=" "><subfield code="a">eng</subfield></datafield><datafield tag="082" ind1="0" ind2="4"><subfield code="a">550</subfield><subfield code="q">DE-600</subfield></datafield><datafield tag="084" ind1=" " ind2=" "><subfield code="a">38.32</subfield><subfield code="2">bkl</subfield></datafield><datafield tag="084" ind1=" " ind2=" "><subfield code="a">39.29</subfield><subfield code="2">bkl</subfield></datafield><datafield tag="100" ind1="1" ind2=" "><subfield code="a">Zhu (朱柯), Ke</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="245" ind1="1" ind2="0"><subfield code="a">Mass-independent and mass-dependent Cr isotopic composition of the Rumuruti (R) chondrites: Implications for their origin and planet formation</subfield></datafield><datafield tag="264" ind1=" " ind2="1"><subfield code="c">2020</subfield></datafield><datafield tag="336" ind1=" " ind2=" "><subfield code="a">nicht spezifiziert</subfield><subfield code="b">zzz</subfield><subfield code="2">rdacontent</subfield></datafield><datafield tag="337" ind1=" " ind2=" "><subfield code="a">Computermedien</subfield><subfield code="b">c</subfield><subfield code="2">rdamedia</subfield></datafield><datafield tag="338" ind1=" " ind2=" "><subfield code="a">Online-Ressource</subfield><subfield code="b">cr</subfield><subfield code="2">rdacarrier</subfield></datafield><datafield tag="520" ind1=" " ind2=" "><subfield code="a">Chromium (Cr) isotopes play an important role in cosmochemistry and planetary science because they are powerful tools for dating (53Mn–53Cr short-lived chronometry), tracing (54Cr nucleosynthetic anomalies) the origins of the materials, and studying the processes involved in volatile element fractionation and planetary differentiation (Cr stable isotopic fractionation). To use Cr isotopes for these purposes, it is essential to precisely know the compositions of the various chondritic reservoirs. However, the Cr isotope composition of Rumuruti (R) chondrites remains unknown. Here, we report high-precision mass-independent (average 2SE uncertainty of ∼0.02 and ∼0.06 for ε53Cr and ε54Cr, respectively; ε indicates 10,000 deviation) and mass-dependent (uncertainty of average 0.03‰ for δ53Cr; δ indicates 1000 deviation) Cr isotope data for 12 bulk R chondrites of petrologic types 3–6 (including R chondrite breccias), and one R chondrite-like clast (MS-CH) in the Almahata Sitta polymict ureilite. All the R chondrites show homogeneous bulk ε54Cr values, −0.06 ± 0.08 (2SD), similar only to those of the Earth–Moon system and enstatite chondrites. This first ε54Cr dataset for R chondrites provides significant addition to the ε54Cr–Δ17O diagram, and positions them as a potential endmember for planetary precursors. The R chondrites possess a higher 55Mn/52Cr of 0.68 ± 0.04 relative to most of carbonaceous chondrites and higher ε53Cr values 0.23 ± 0.05 (2SD) relative to most of chondrite groups. This likely results from the lower chondrule abundance in R chondrites compared to that of ordinary and enstatite chondrites. The stable Cr isotope composition of R chondrites is homogeneous with a δ53Cr = −0.12 ± 0.03‰ (2SD). Combined with previous data of other groups of chondrites, we show that the stable Cr isotopic composition of all the chondrites is homogeneous with δ53Cr of −0.12 ± 0.04‰ (2SD, N = 42) and is independent of the petrologic type and redox conditions. The lack of mass-dependent fractionation between all groups of chondrites suggests that the average chondrite δ53Cr value is also representative for the initial composition of all differentiated planets in the Solar System. 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Zhu (朱柯), Ke |
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Zhu (朱柯), Ke ddc 550 bkl 38.32 bkl 39.29 misc Rumuruti Chondrites misc Cr stable isotopes misc Chondritic clast Mass-independent and mass-dependent Cr isotopic composition of the Rumuruti (R) chondrites: Implications for their origin and planet formation |
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550 DE-600 38.32 bkl 39.29 bkl Mass-independent and mass-dependent Cr isotopic composition of the Rumuruti (R) chondrites: Implications for their origin and planet formation Rumuruti Chondrites Cr stable isotopes Chondritic clast |
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Mass-independent and mass-dependent Cr isotopic composition of the Rumuruti (R) chondrites: Implications for their origin and planet formation |
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Mass-independent and mass-dependent Cr isotopic composition of the Rumuruti (R) chondrites: Implications for their origin and planet formation |
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Zhu (朱柯), Ke |
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Zhu (朱柯), Ke Moynier, Frédéric Schiller, Martin Alexander, Conel M.O'D. Barrat, Jean-Alix Bischoff, Addi Bizzarro, Martin |
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mass-independent and mass-dependent cr isotopic composition of the rumuruti (r) chondrites: implications for their origin and planet formation |
| title_auth |
Mass-independent and mass-dependent Cr isotopic composition of the Rumuruti (R) chondrites: Implications for their origin and planet formation |
| abstract |
Chromium (Cr) isotopes play an important role in cosmochemistry and planetary science because they are powerful tools for dating (53Mn–53Cr short-lived chronometry), tracing (54Cr nucleosynthetic anomalies) the origins of the materials, and studying the processes involved in volatile element fractionation and planetary differentiation (Cr stable isotopic fractionation). To use Cr isotopes for these purposes, it is essential to precisely know the compositions of the various chondritic reservoirs. However, the Cr isotope composition of Rumuruti (R) chondrites remains unknown. Here, we report high-precision mass-independent (average 2SE uncertainty of ∼0.02 and ∼0.06 for ε53Cr and ε54Cr, respectively; ε indicates 10,000 deviation) and mass-dependent (uncertainty of average 0.03‰ for δ53Cr; δ indicates 1000 deviation) Cr isotope data for 12 bulk R chondrites of petrologic types 3–6 (including R chondrite breccias), and one R chondrite-like clast (MS-CH) in the Almahata Sitta polymict ureilite. All the R chondrites show homogeneous bulk ε54Cr values, −0.06 ± 0.08 (2SD), similar only to those of the Earth–Moon system and enstatite chondrites. This first ε54Cr dataset for R chondrites provides significant addition to the ε54Cr–Δ17O diagram, and positions them as a potential endmember for planetary precursors. The R chondrites possess a higher 55Mn/52Cr of 0.68 ± 0.04 relative to most of carbonaceous chondrites and higher ε53Cr values 0.23 ± 0.05 (2SD) relative to most of chondrite groups. This likely results from the lower chondrule abundance in R chondrites compared to that of ordinary and enstatite chondrites. The stable Cr isotope composition of R chondrites is homogeneous with a δ53Cr = −0.12 ± 0.03‰ (2SD). Combined with previous data of other groups of chondrites, we show that the stable Cr isotopic composition of all the chondrites is homogeneous with δ53Cr of −0.12 ± 0.04‰ (2SD, N = 42) and is independent of the petrologic type and redox conditions. The lack of mass-dependent fractionation between all groups of chondrites suggests that the average chondrite δ53Cr value is also representative for the initial composition of all differentiated planets in the Solar System. Finally, the MS–CH clast in Almahata Sitta has a Cr isotopic composition (ε53Cr = 0.18 ± 0.04, ε54Cr = −0.16 ± 0.07, and δ53Cr = −0.11 ± 0.05‰) that is consistent (within error) with it being an R chondrite-like clast. |
| abstractGer |
Chromium (Cr) isotopes play an important role in cosmochemistry and planetary science because they are powerful tools for dating (53Mn–53Cr short-lived chronometry), tracing (54Cr nucleosynthetic anomalies) the origins of the materials, and studying the processes involved in volatile element fractionation and planetary differentiation (Cr stable isotopic fractionation). To use Cr isotopes for these purposes, it is essential to precisely know the compositions of the various chondritic reservoirs. However, the Cr isotope composition of Rumuruti (R) chondrites remains unknown. Here, we report high-precision mass-independent (average 2SE uncertainty of ∼0.02 and ∼0.06 for ε53Cr and ε54Cr, respectively; ε indicates 10,000 deviation) and mass-dependent (uncertainty of average 0.03‰ for δ53Cr; δ indicates 1000 deviation) Cr isotope data for 12 bulk R chondrites of petrologic types 3–6 (including R chondrite breccias), and one R chondrite-like clast (MS-CH) in the Almahata Sitta polymict ureilite. All the R chondrites show homogeneous bulk ε54Cr values, −0.06 ± 0.08 (2SD), similar only to those of the Earth–Moon system and enstatite chondrites. This first ε54Cr dataset for R chondrites provides significant addition to the ε54Cr–Δ17O diagram, and positions them as a potential endmember for planetary precursors. The R chondrites possess a higher 55Mn/52Cr of 0.68 ± 0.04 relative to most of carbonaceous chondrites and higher ε53Cr values 0.23 ± 0.05 (2SD) relative to most of chondrite groups. This likely results from the lower chondrule abundance in R chondrites compared to that of ordinary and enstatite chondrites. The stable Cr isotope composition of R chondrites is homogeneous with a δ53Cr = −0.12 ± 0.03‰ (2SD). Combined with previous data of other groups of chondrites, we show that the stable Cr isotopic composition of all the chondrites is homogeneous with δ53Cr of −0.12 ± 0.04‰ (2SD, N = 42) and is independent of the petrologic type and redox conditions. The lack of mass-dependent fractionation between all groups of chondrites suggests that the average chondrite δ53Cr value is also representative for the initial composition of all differentiated planets in the Solar System. Finally, the MS–CH clast in Almahata Sitta has a Cr isotopic composition (ε53Cr = 0.18 ± 0.04, ε54Cr = −0.16 ± 0.07, and δ53Cr = −0.11 ± 0.05‰) that is consistent (within error) with it being an R chondrite-like clast. |
| abstract_unstemmed |
Chromium (Cr) isotopes play an important role in cosmochemistry and planetary science because they are powerful tools for dating (53Mn–53Cr short-lived chronometry), tracing (54Cr nucleosynthetic anomalies) the origins of the materials, and studying the processes involved in volatile element fractionation and planetary differentiation (Cr stable isotopic fractionation). To use Cr isotopes for these purposes, it is essential to precisely know the compositions of the various chondritic reservoirs. However, the Cr isotope composition of Rumuruti (R) chondrites remains unknown. Here, we report high-precision mass-independent (average 2SE uncertainty of ∼0.02 and ∼0.06 for ε53Cr and ε54Cr, respectively; ε indicates 10,000 deviation) and mass-dependent (uncertainty of average 0.03‰ for δ53Cr; δ indicates 1000 deviation) Cr isotope data for 12 bulk R chondrites of petrologic types 3–6 (including R chondrite breccias), and one R chondrite-like clast (MS-CH) in the Almahata Sitta polymict ureilite. All the R chondrites show homogeneous bulk ε54Cr values, −0.06 ± 0.08 (2SD), similar only to those of the Earth–Moon system and enstatite chondrites. This first ε54Cr dataset for R chondrites provides significant addition to the ε54Cr–Δ17O diagram, and positions them as a potential endmember for planetary precursors. The R chondrites possess a higher 55Mn/52Cr of 0.68 ± 0.04 relative to most of carbonaceous chondrites and higher ε53Cr values 0.23 ± 0.05 (2SD) relative to most of chondrite groups. This likely results from the lower chondrule abundance in R chondrites compared to that of ordinary and enstatite chondrites. The stable Cr isotope composition of R chondrites is homogeneous with a δ53Cr = −0.12 ± 0.03‰ (2SD). Combined with previous data of other groups of chondrites, we show that the stable Cr isotopic composition of all the chondrites is homogeneous with δ53Cr of −0.12 ± 0.04‰ (2SD, N = 42) and is independent of the petrologic type and redox conditions. The lack of mass-dependent fractionation between all groups of chondrites suggests that the average chondrite δ53Cr value is also representative for the initial composition of all differentiated planets in the Solar System. Finally, the MS–CH clast in Almahata Sitta has a Cr isotopic composition (ε53Cr = 0.18 ± 0.04, ε54Cr = −0.16 ± 0.07, and δ53Cr = −0.11 ± 0.05‰) that is consistent (within error) with it being an R chondrite-like clast. |
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| title_short |
Mass-independent and mass-dependent Cr isotopic composition of the Rumuruti (R) chondrites: Implications for their origin and planet formation |
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Moynier, Frédéric Schiller, Martin Alexander, Conel M.O'D. Barrat, Jean-Alix Bischoff, Addi Bizzarro, Martin |
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Moynier, Frédéric Schiller, Martin Alexander, Conel M.O'D. Barrat, Jean-Alix Bischoff, Addi Bizzarro, Martin |
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| doi_str |
10.1016/j.gca.2020.10.007 |
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2024-07-06T17:15:24.437Z |
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