The initial solar system abundance of 60Fe and early core formation of the first asteroids
High-precision Ni isotope analyses of the differentiated andesitic meteorite Erg Chech 002 (EC 002), the oldest known crustal fragment of a planetesimal, show that short-lived 60Fe was present in the early solar system with an initial 60Fe/56Fe ratio of (7.71 ± 0.47) × 10-9, which is five times more...
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| description | High-precision Ni isotope analyses of the differentiated andesitic meteorite Erg Chech 002 (EC 002), the oldest known crustal fragment of a planetesimal, show that short-lived 60Fe was present in the early solar system with an initial 60Fe/56Fe ratio of (7.71 ± 0.47) × 10-9, which is five times more precise than previous estimates and is proposed to be the reference value for further studies. Using this ratio, the Ni isotopic composition of EC 002 implies that metal segregation in the source of the EC 002 parental melts took place [Formula: see text] million years (Myr) after solar system formation, and similar very early metal-silicate differentiation ages are obtained for 4-Vesta ([Formula: see text] Myr) and the angrite parent body ([Formula: see text] Myr). Such an early age dictates a specific accretion and differentiation history for the EC 002 parent body, with metal segregation occurring at relatively low temperatures (1000° to 1200°C), followed by a high-temperature silicate melting event.High-precision Ni isotope analyses of the differentiated andesitic meteorite Erg Chech 002 (EC 002), the oldest known crustal fragment of a planetesimal, show that short-lived 60Fe was present in the early solar system with an initial 60Fe/56Fe ratio of (7.71 ± 0.47) × 10-9, which is five times more precise than previous estimates and is proposed to be the reference value for further studies. Using this ratio, the Ni isotopic composition of EC 002 implies that metal segregation in the source of the EC 002 parental melts took place [Formula: see text] million years (Myr) after solar system formation, and similar very early metal-silicate differentiation ages are obtained for 4-Vesta ([Formula: see text] Myr) and the angrite parent body ([Formula: see text] Myr). Such an early age dictates a specific accretion and differentiation history for the EC 002 parent body, with metal segregation occurring at relatively low temperatures (1000° to 1200°C), followed by a high-temperature silicate melting event. |
| doi_str_mv | 10.1126/sciadv.adp9381 |
| format | Article |
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Using this ratio, the Ni isotopic composition of EC 002 implies that metal segregation in the source of the EC 002 parental melts took place [Formula: see text] million years (Myr) after solar system formation, and similar very early metal-silicate differentiation ages are obtained for 4-Vesta ([Formula: see text] Myr) and the angrite parent body ([Formula: see text] Myr). Such an early age dictates a specific accretion and differentiation history for the EC 002 parent body, with metal segregation occurring at relatively low temperatures (1000° to 1200°C), followed by a high-temperature silicate melting event.High-precision Ni isotope analyses of the differentiated andesitic meteorite Erg Chech 002 (EC 002), the oldest known crustal fragment of a planetesimal, show that short-lived 60Fe was present in the early solar system with an initial 60Fe/56Fe ratio of (7.71 ± 0.47) × 10-9, which is five times more precise than previous estimates and is proposed to be the reference value for further studies. Using this ratio, the Ni isotopic composition of EC 002 implies that metal segregation in the source of the EC 002 parental melts took place [Formula: see text] million years (Myr) after solar system formation, and similar very early metal-silicate differentiation ages are obtained for 4-Vesta ([Formula: see text] Myr) and the angrite parent body ([Formula: see text] Myr). Such an early age dictates a specific accretion and differentiation history for the EC 002 parent body, with metal segregation occurring at relatively low temperatures (1000° to 1200°C), followed by a high-temperature silicate melting event.</description><identifier>ISSN: 2375-2548</identifier><identifier>EISSN: 2375-2548</identifier><identifier>DOI: 10.1126/sciadv.adp9381</identifier><identifier>PMID: 39772667</identifier><language>eng</language><publisher>American Association for the Advancement of Science</publisher><subject>Earth, Environmental, Ecological, and Space Sciences ; SciAdv r-articles ; Space Sciences</subject><ispartof>Science advances, 2025-01, Vol.11 (2), p.eadp9381</ispartof><rights>Copyright © 2025 The Authors, some rights reserved; exclusive licensee American Association for the Advancement of Science. No claim to original U.S. Government Works. 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Using this ratio, the Ni isotopic composition of EC 002 implies that metal segregation in the source of the EC 002 parental melts took place [Formula: see text] million years (Myr) after solar system formation, and similar very early metal-silicate differentiation ages are obtained for 4-Vesta ([Formula: see text] Myr) and the angrite parent body ([Formula: see text] Myr). Such an early age dictates a specific accretion and differentiation history for the EC 002 parent body, with metal segregation occurring at relatively low temperatures (1000° to 1200°C), followed by a high-temperature silicate melting event.High-precision Ni isotope analyses of the differentiated andesitic meteorite Erg Chech 002 (EC 002), the oldest known crustal fragment of a planetesimal, show that short-lived 60Fe was present in the early solar system with an initial 60Fe/56Fe ratio of (7.71 ± 0.47) × 10-9, which is five times more precise than previous estimates and is proposed to be the reference value for further studies. Using this ratio, the Ni isotopic composition of EC 002 implies that metal segregation in the source of the EC 002 parental melts took place [Formula: see text] million years (Myr) after solar system formation, and similar very early metal-silicate differentiation ages are obtained for 4-Vesta ([Formula: see text] Myr) and the angrite parent body ([Formula: see text] Myr). Such an early age dictates a specific accretion and differentiation history for the EC 002 parent body, with metal segregation occurring at relatively low temperatures (1000° to 1200°C), followed by a high-temperature silicate melting event.</description><subject>Earth, Environmental, Ecological, and Space Sciences</subject><subject>SciAdv r-articles</subject><subject>Space Sciences</subject><issn>2375-2548</issn><issn>2375-2548</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2025</creationdate><recordtype>article</recordtype><recordid>eNpVjj1PwzAYhC0EohV0ZfbIkuKv-GNCqKKAVImlLCzR2-Q1NUriYKeV-u8pogNMd9LdPTpCbjibcy70Xa4DNPs5NIOTlp-RqZCmLESp7PkfPyGznD8ZY1xpXXJ3SSbSGSO0NlPyvt4iDX0YA7Q0xxYSzYc8Ykdhs-sb6Guk0VPNlkihbyhCag-0jgmpj6mDMcT-pzAeMT6kPFI4rlMMTb4mFx7ajLOTXpG35eN68VysXp9eFg-rYuBGjcXxi0cnPAJablE66wyTstl4AZoJ4ZQwTDlde21FLZVSHmvjGuatAqWNvCL3v9xht-mwqbEfE7TVkEIH6VBFCNX_pA_b6iPuK84Ns9bII-H2REjxa4d5rLqQa2xb6DHuciV5Ka3hrtTyG4AhcOk</recordid><startdate>20250108</startdate><enddate>20250108</enddate><creator>Fang, Linru</creator><creator>Moynier, Frédéric</creator><creator>Chaussidon, Marc</creator><creator>Limare, Angela</creator><creator>Makhatadze, Georgy V</creator><creator>Villeneuve, Johan</creator><general>American Association for the Advancement of Science</general><scope>7X8</scope><scope>5PM</scope></search><sort><creationdate>20250108</creationdate><title>The initial solar system abundance of 60Fe and early core formation of the first asteroids</title><author>Fang, Linru ; Moynier, Frédéric ; Chaussidon, Marc ; Limare, Angela ; Makhatadze, Georgy V ; Villeneuve, Johan</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-p174t-397fe92feae818e39897033dbf2a602294270496cf682c3444fec79d0f84a4673</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2025</creationdate><topic>Earth, Environmental, Ecological, and Space Sciences</topic><topic>SciAdv r-articles</topic><topic>Space Sciences</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Fang, Linru</creatorcontrib><creatorcontrib>Moynier, Frédéric</creatorcontrib><creatorcontrib>Chaussidon, Marc</creatorcontrib><creatorcontrib>Limare, Angela</creatorcontrib><creatorcontrib>Makhatadze, Georgy V</creatorcontrib><creatorcontrib>Villeneuve, Johan</creatorcontrib><collection>MEDLINE - Academic</collection><collection>PubMed Central (Full Participant titles)</collection><jtitle>Science advances</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Fang, Linru</au><au>Moynier, Frédéric</au><au>Chaussidon, Marc</au><au>Limare, Angela</au><au>Makhatadze, Georgy V</au><au>Villeneuve, Johan</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>The initial solar system abundance of 60Fe and early core formation of the first asteroids</atitle><jtitle>Science advances</jtitle><date>2025-01-08</date><risdate>2025</risdate><volume>11</volume><issue>2</issue><spage>eadp9381</spage><pages>eadp9381-</pages><issn>2375-2548</issn><eissn>2375-2548</eissn><abstract>High-precision Ni isotope analyses of the differentiated andesitic meteorite Erg Chech 002 (EC 002), the oldest known crustal fragment of a planetesimal, show that short-lived 60Fe was present in the early solar system with an initial 60Fe/56Fe ratio of (7.71 ± 0.47) × 10-9, which is five times more precise than previous estimates and is proposed to be the reference value for further studies. Using this ratio, the Ni isotopic composition of EC 002 implies that metal segregation in the source of the EC 002 parental melts took place [Formula: see text] million years (Myr) after solar system formation, and similar very early metal-silicate differentiation ages are obtained for 4-Vesta ([Formula: see text] Myr) and the angrite parent body ([Formula: see text] Myr). Such an early age dictates a specific accretion and differentiation history for the EC 002 parent body, with metal segregation occurring at relatively low temperatures (1000° to 1200°C), followed by a high-temperature silicate melting event.High-precision Ni isotope analyses of the differentiated andesitic meteorite Erg Chech 002 (EC 002), the oldest known crustal fragment of a planetesimal, show that short-lived 60Fe was present in the early solar system with an initial 60Fe/56Fe ratio of (7.71 ± 0.47) × 10-9, which is five times more precise than previous estimates and is proposed to be the reference value for further studies. Using this ratio, the Ni isotopic composition of EC 002 implies that metal segregation in the source of the EC 002 parental melts took place [Formula: see text] million years (Myr) after solar system formation, and similar very early metal-silicate differentiation ages are obtained for 4-Vesta ([Formula: see text] Myr) and the angrite parent body ([Formula: see text] Myr). Such an early age dictates a specific accretion and differentiation history for the EC 002 parent body, with metal segregation occurring at relatively low temperatures (1000° to 1200°C), followed by a high-temperature silicate melting event.</abstract><pub>American Association for the Advancement of Science</pub><pmid>39772667</pmid><doi>10.1126/sciadv.adp9381</doi><oa>free_for_read</oa></addata></record> |
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| title | The initial solar system abundance of 60Fe and early core formation of the first asteroids |
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