Mass-independent and mass-dependent Cr isotopic composition of the Rumuruti (R) chondrites: Implications for their origin and planet formation

Ke Zhu (朱柯); Frédéric Moynier; Martin Schiller; Conel M.O.D. Alexander; Jean Alix Barrat; Addi Bischoff; Martin Bizzarro

doi:10.1016/j.gca.2020.10.007

Mass-independent and mass-dependent Cr isotopic composition of the Rumuruti (R) chondrites: Implications for their origin and planet formation

Ke Zhu (朱柯)^*, Frédéric Moynier, Martin Schiller, Conel M.O.D. Alexander, Jean Alix Barrat, Addi Bischoff, Martin Bizzarro

^*Corresponding author for this work

School of Earth Sciences

Research output: Contribution to journal › Article (Academic Journal) › peer-review

18 Citations (Scopus)

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.

Original language	English
Pages (from-to)	598-609
Number of pages	12
Journal	Geochimica et Cosmochimica Acta
Volume	293
Early online date	15 Oct 2020
DOIs	https://doi.org/10.1016/j.gca.2020.10.007
Publication status	Published - 15 Jan 2021

Bibliographical note

Funding Information:
Three anonymous reviewers, Associate Editor Prof. Yuri Amelin and Executive Editor Prof. Jeffrey G. Catalano are deeply thanked for constructive comments which greatly improved the quality of this paper. We thank the Meteorite Working Group (NASA), and the Museum für Naturkunde (Berlin; A. Greshake) for providing additional samples of Rumuruti chondrites. US Antarctic meteorite samples are recovered by the Antarctic search for Meteorites (ANSMET) program which has been funded by NSF and NASA, and characterized and curated in the Department of Mineral Sciences of the Smithsonian Institution and Astromaterials Curation Office at NASA Johnson Space Center. F. M. acknowledges funding from the European Research Council under the H2020 framework program/ERC grant agreement (ERC starting grant, #637503-PRISTINE) and financial support of the UnivEarthS Labex program at Université de Paris (#ANR-10-LABX-0023 and #ANR-11-IDEX-0005-02), and the IPGP platform PARI, and the Region Île-de-France Sesame grant no. 12015908. M. S. acknowledges funding from the Villum Fonden (#00025333). M. B. acknowledges funding from the Carlsberg Foundation (#CF18-1105), the Danish National Research Foundation (#DNRF97) and the European Research Council (ERC Advanced Grant Agreement, #833275-DEEPTIME). A. B. thanks the support by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation, #263649064) – TRR 170 (subproject B05). This is TRR170 Publication No. 116. K. Z. thanks the China Scholarship Council (CSC) for the PhD fellowship (#201706340161) and IPGP for the funding support of traveling, “Aide à la MOBILITE INTERNATIONALE des doctorants de l'IPGP” (2019), to visit Earth and Planetary Laboratory, Carnegie Institution for Science. Timothy Mock and Mary Horan are appreciated for their assistance in ICP-MS analysis and clean labs respectively.

Funding Information:
Three anonymous reviewers, Associate Editor Prof. Yuri Amelin and Executive Editor Prof. Jeffrey G. Catalano are deeply thanked for constructive comments which greatly improved the quality of this paper. We thank the Meteorite Working Group (NASA), and the Museum für Naturkunde (Berlin; A. Greshake) for providing additional samples of Rumuruti chondrites. US Antarctic meteorite samples are recovered by the Antarctic search for Meteorites (ANSMET) program which has been funded by NSF and NASA, and characterized and curated in the Department of Mineral Sciences of the Smithsonian Institution and Astromaterials Curation Office at NASA Johnson Space Center. F. M. acknowledges funding from the European Research Council under the H2020 framework program/ERC grant agreement (ERC starting grant, #637503-PRISTINE) and financial support of the UnivEarthS Labex program at Université de Paris (#ANR-10-LABX-0023 and #ANR-11-IDEX-0005-02), and the IPGP platform PARI, and the Region Île-de-France Sesame grant no. 12015908. M. S. acknowledges funding from the Villum Fonden (#00025333). M. B. acknowledges funding from the Carlsberg Foundation (#CF18-1105), the Danish National Research Foundation (#DNRF97) and the European Research Council (ERC Advanced Grant Agreement, #833275-DEEPTIME). A. B. thanks the support by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation, #263649064) – TRR 170 (subproject B05). This is TRR170 Publication No. 116. K. Z. thanks the China Scholarship Council (CSC) for the PhD fellowship (#201706340161) and IPGP for the funding support of traveling, “Aide à la MOBILITE INTERNATIONALE des doctorants de l’IPGP” (2019), to visit Earth and Planetary Laboratory, Carnegie Institution for Science. Timothy Mock and Mary Horan are appreciated for their assistance in ICP-MS analysis and clean labs respectively.

Publisher Copyright:
© 2020 Elsevier Ltd

Keywords

Mn-Cr chronometry
Cr nucleosynthetic anomalies
Chondritic clast
Cr stable isotopes
Rumuruti Chondrites

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@article{1f41d7ed153341f2a513bceeeee433ac,

title = "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.",

keywords = "Mn-Cr chronometry, Cr nucleosynthetic anomalies, Chondritic clast, Cr stable isotopes, Rumuruti Chondrites",

author = "{Zhu (朱柯)}, Ke and Fr{\'e}d{\'e}ric Moynier and Martin Schiller and Alexander, {Conel M.O.D.} and Barrat, {Jean Alix} and Addi Bischoff and Martin Bizzarro",

note = "Funding Information: Three anonymous reviewers, Associate Editor Prof. Yuri Amelin and Executive Editor Prof. Jeffrey G. Catalano are deeply thanked for constructive comments which greatly improved the quality of this paper. We thank the Meteorite Working Group (NASA), and the Museum f{\"u}r Naturkunde (Berlin; A. Greshake) for providing additional samples of Rumuruti chondrites. US Antarctic meteorite samples are recovered by the Antarctic search for Meteorites (ANSMET) program which has been funded by NSF and NASA, and characterized and curated in the Department of Mineral Sciences of the Smithsonian Institution and Astromaterials Curation Office at NASA Johnson Space Center. F. M. acknowledges funding from the European Research Council under the H2020 framework program/ERC grant agreement (ERC starting grant, #637503-PRISTINE) and financial support of the UnivEarthS Labex program at Universit{\'e} de Paris (#ANR-10-LABX-0023 and #ANR-11-IDEX-0005-02), and the IPGP platform PARI, and the Region {\^I}le-de-France Sesame grant no. 12015908. M. S. acknowledges funding from the Villum Fonden (#00025333). M. B. acknowledges funding from the Carlsberg Foundation (#CF18-1105), the Danish National Research Foundation (#DNRF97) and the European Research Council (ERC Advanced Grant Agreement, #833275-DEEPTIME). A. B. thanks the support by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation, #263649064) – TRR 170 (subproject B05). This is TRR170 Publication No. 116. K. Z. thanks the China Scholarship Council (CSC) for the PhD fellowship (#201706340161) and IPGP for the funding support of traveling, “Aide {\`a} la MOBILITE INTERNATIONALE des doctorants de l'IPGP” (2019), to visit Earth and Planetary Laboratory, Carnegie Institution for Science. Timothy Mock and Mary Horan are appreciated for their assistance in ICP-MS analysis and clean labs respectively. Funding Information: Three anonymous reviewers, Associate Editor Prof. Yuri Amelin and Executive Editor Prof. Jeffrey G. Catalano are deeply thanked for constructive comments which greatly improved the quality of this paper. We thank the Meteorite Working Group (NASA), and the Museum f{\"u}r Naturkunde (Berlin; A. Greshake) for providing additional samples of Rumuruti chondrites. US Antarctic meteorite samples are recovered by the Antarctic search for Meteorites (ANSMET) program which has been funded by NSF and NASA, and characterized and curated in the Department of Mineral Sciences of the Smithsonian Institution and Astromaterials Curation Office at NASA Johnson Space Center. F. M. acknowledges funding from the European Research Council under the H2020 framework program/ERC grant agreement (ERC starting grant, #637503-PRISTINE) and financial support of the UnivEarthS Labex program at Universit{\'e} de Paris (#ANR-10-LABX-0023 and #ANR-11-IDEX-0005-02), and the IPGP platform PARI, and the Region {\^I}le-de-France Sesame grant no. 12015908. M. S. acknowledges funding from the Villum Fonden (#00025333). M. B. acknowledges funding from the Carlsberg Foundation (#CF18-1105), the Danish National Research Foundation (#DNRF97) and the European Research Council (ERC Advanced Grant Agreement, #833275-DEEPTIME). A. B. thanks the support by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation, #263649064) – TRR 170 (subproject B05). This is TRR170 Publication No. 116. K. Z. thanks the China Scholarship Council (CSC) for the PhD fellowship (#201706340161) and IPGP for the funding support of traveling, “Aide {\`a} la MOBILITE INTERNATIONALE des doctorants de l{\textquoteright}IPGP” (2019), to visit Earth and Planetary Laboratory, Carnegie Institution for Science. Timothy Mock and Mary Horan are appreciated for their assistance in ICP-MS analysis and clean labs respectively. Publisher Copyright: {\textcopyright} 2020 Elsevier Ltd",

year = "2021",

month = jan,

day = "15",

doi = "10.1016/j.gca.2020.10.007",

language = "English",

volume = "293",

pages = "598--609",

journal = "Geochimica et Cosmochimica Acta",

issn = "0016-7037",

publisher = "Elsevier",

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TY - JOUR

T1 - Mass-independent and mass-dependent Cr isotopic composition of the Rumuruti (R) chondrites

T2 - Implications for their origin and planet formation

AU - Zhu (朱柯), Ke

AU - Moynier, Frédéric

AU - Schiller, Martin

AU - Alexander, Conel M.O.D.

AU - Barrat, Jean Alix

AU - Bischoff, Addi

AU - Bizzarro, Martin

N1 - Funding Information: Three anonymous reviewers, Associate Editor Prof. Yuri Amelin and Executive Editor Prof. Jeffrey G. Catalano are deeply thanked for constructive comments which greatly improved the quality of this paper. We thank the Meteorite Working Group (NASA), and the Museum für Naturkunde (Berlin; A. Greshake) for providing additional samples of Rumuruti chondrites. US Antarctic meteorite samples are recovered by the Antarctic search for Meteorites (ANSMET) program which has been funded by NSF and NASA, and characterized and curated in the Department of Mineral Sciences of the Smithsonian Institution and Astromaterials Curation Office at NASA Johnson Space Center. F. M. acknowledges funding from the European Research Council under the H2020 framework program/ERC grant agreement (ERC starting grant, #637503-PRISTINE) and financial support of the UnivEarthS Labex program at Université de Paris (#ANR-10-LABX-0023 and #ANR-11-IDEX-0005-02), and the IPGP platform PARI, and the Region Île-de-France Sesame grant no. 12015908. M. S. acknowledges funding from the Villum Fonden (#00025333). M. B. acknowledges funding from the Carlsberg Foundation (#CF18-1105), the Danish National Research Foundation (#DNRF97) and the European Research Council (ERC Advanced Grant Agreement, #833275-DEEPTIME). A. B. thanks the support by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation, #263649064) – TRR 170 (subproject B05). This is TRR170 Publication No. 116. K. Z. thanks the China Scholarship Council (CSC) for the PhD fellowship (#201706340161) and IPGP for the funding support of traveling, “Aide à la MOBILITE INTERNATIONALE des doctorants de l'IPGP” (2019), to visit Earth and Planetary Laboratory, Carnegie Institution for Science. Timothy Mock and Mary Horan are appreciated for their assistance in ICP-MS analysis and clean labs respectively. Funding Information: Three anonymous reviewers, Associate Editor Prof. Yuri Amelin and Executive Editor Prof. Jeffrey G. Catalano are deeply thanked for constructive comments which greatly improved the quality of this paper. We thank the Meteorite Working Group (NASA), and the Museum für Naturkunde (Berlin; A. Greshake) for providing additional samples of Rumuruti chondrites. US Antarctic meteorite samples are recovered by the Antarctic search for Meteorites (ANSMET) program which has been funded by NSF and NASA, and characterized and curated in the Department of Mineral Sciences of the Smithsonian Institution and Astromaterials Curation Office at NASA Johnson Space Center. F. M. acknowledges funding from the European Research Council under the H2020 framework program/ERC grant agreement (ERC starting grant, #637503-PRISTINE) and financial support of the UnivEarthS Labex program at Université de Paris (#ANR-10-LABX-0023 and #ANR-11-IDEX-0005-02), and the IPGP platform PARI, and the Region Île-de-France Sesame grant no. 12015908. M. S. acknowledges funding from the Villum Fonden (#00025333). M. B. acknowledges funding from the Carlsberg Foundation (#CF18-1105), the Danish National Research Foundation (#DNRF97) and the European Research Council (ERC Advanced Grant Agreement, #833275-DEEPTIME). A. B. thanks the support by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation, #263649064) – TRR 170 (subproject B05). This is TRR170 Publication No. 116. K. Z. thanks the China Scholarship Council (CSC) for the PhD fellowship (#201706340161) and IPGP for the funding support of traveling, “Aide à la MOBILITE INTERNATIONALE des doctorants de l’IPGP” (2019), to visit Earth and Planetary Laboratory, Carnegie Institution for Science. Timothy Mock and Mary Horan are appreciated for their assistance in ICP-MS analysis and clean labs respectively. Publisher Copyright: © 2020 Elsevier Ltd

PY - 2021/1/15

Y1 - 2021/1/15

N2 - 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.

AB - 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.

KW - Mn-Cr chronometry

KW - Cr nucleosynthetic anomalies

KW - Chondritic clast

KW - Cr stable isotopes

KW - Rumuruti Chondrites

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U2 - 10.1016/j.gca.2020.10.007

DO - 10.1016/j.gca.2020.10.007

M3 - Article (Academic Journal)

AN - SCOPUS:85094877611

SN - 0016-7037

VL - 293

SP - 598

EP - 609

JO - Geochimica et Cosmochimica Acta

JF - Geochimica et Cosmochimica Acta

ER -

Mass-independent and mass-dependent Cr isotopic composition of the Rumuruti (R) chondrites: Implications for their origin and planet formation

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