Isotopic evidence for primordial molecular cloud material in metal-rich carbonaceous chondrites

Elishevah M. M. E. van Kooten; Daniel Kim Peel Wielandt; Martin Schiller; Kazuhide Nagashima; Aurélien Thomen; Kirsten Kolbjørn Larsen; Mia Bjørg Stolberg Olsen; Åke Nordlund; Alexander N. Krot; Martin Bizzarro

doi:10.1073/pnas.1518183113

Isotopic evidence for primordial molecular cloud material in metal-rich carbonaceous chondrites

Elishevah M. M. E. van Kooten, Daniel Kim Peel Wielandt, Martin Schiller, Kazuhide Nagashima, Aurélien Thomen, Kirsten Kolbjørn Larsen, Mia Bjørg Stolberg Olsen, Åke Nordlund, Alexander N. Krot, Martin Bizzarro

Astrophysics and Planetary Science

90 Citations (Scopus)

Abstract

The short-lived (26)Al radionuclide is thought to have been admixed into the initially (26)Al-poor protosolar molecular cloud before or contemporaneously with its collapse. Bulk inner Solar System reservoirs record positively correlated variability in mass-independent (54)Cr and (26)Mg*, the decay product of (26)Al. This correlation is interpreted as reflecting progressive thermal processing of in-falling (26)Al-rich molecular cloud material in the inner Solar System. The thermally unprocessed molecular cloud matter reflecting the nucleosynthetic makeup of the molecular cloud before the last addition of stellar-derived (26)Al has not been identified yet but may be preserved in planetesimals that accreted in the outer Solar System. We show that metal-rich carbonaceous chondrites and their components have a unique isotopic signature extending from an inner Solar System composition toward a (26)Mg*-depleted and (54)Cr-enriched component. This composition is consistent with that expected for thermally unprocessed primordial molecular cloud material before its pollution by stellar-derived (26)Al. The (26)Mg* and (54)Cr compositions of bulk metal-rich chondrites require significant amounts (25-50%) of primordial molecular cloud matter in their precursor material. Given that such high fractions of primordial molecular cloud material are expected to survive only in the outer Solar System, we infer that, similarly to cometary bodies, metal-rich carbonaceous chondrites are samples of planetesimals that accreted beyond the orbits of the gas giants. The lack of evidence for this material in other chondrite groups requires isolation from the outer Solar System, possibly by the opening of disk gaps from the early formation of gas giants.

Original language	English
Journal	National Academy of Sciences. Proceedings
Volume	113
Issue number	8
Pages (from-to)	2011-2016
Number of pages	6
ISSN	0027-8424
DOIs	https://doi.org/10.1073/pnas.1518183113
Publication status	Published - 23 Feb 2016

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@article{d20823f55f0743999f5a5f80254a225b,

title = "Isotopic evidence for primordial molecular cloud material in metal-rich carbonaceous chondrites",

abstract = "The short-lived (26)Al radionuclide is thought to have been admixed into the initially (26)Al-poor protosolar molecular cloud before or contemporaneously with its collapse. Bulk inner Solar System reservoirs record positively correlated variability in mass-independent (54)Cr and (26)Mg*, the decay product of (26)Al. This correlation is interpreted as reflecting progressive thermal processing of in-falling (26)Al-rich molecular cloud material in the inner Solar System. The thermally unprocessed molecular cloud matter reflecting the nucleosynthetic makeup of the molecular cloud before the last addition of stellar-derived (26)Al has not been identified yet but may be preserved in planetesimals that accreted in the outer Solar System. We show that metal-rich carbonaceous chondrites and their components have a unique isotopic signature extending from an inner Solar System composition toward a (26)Mg*-depleted and (54)Cr-enriched component. This composition is consistent with that expected for thermally unprocessed primordial molecular cloud material before its pollution by stellar-derived (26)Al. The (26)Mg* and (54)Cr compositions of bulk metal-rich chondrites require significant amounts (25-50%) of primordial molecular cloud matter in their precursor material. Given that such high fractions of primordial molecular cloud material are expected to survive only in the outer Solar System, we infer that, similarly to cometary bodies, metal-rich carbonaceous chondrites are samples of planetesimals that accreted beyond the orbits of the gas giants. The lack of evidence for this material in other chondrite groups requires isolation from the outer Solar System, possibly by the opening of disk gaps from the early formation of gas giants.",

author = "{van Kooten}, {Elishevah M. M. E.} and Wielandt, {Daniel Kim Peel} and Martin Schiller and Kazuhide Nagashima and Aur{\'e}lien Thomen and Larsen, {Kirsten Kolbj{\o}rn} and Olsen, {Mia Bj{\o}rg Stolberg} and {\AA}ke Nordlund and Krot, {Alexander N.} and Martin Bizzarro",

year = "2016",

month = feb,

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doi = "10.1073/pnas.1518183113",

language = "English",

volume = "113",

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T1 - Isotopic evidence for primordial molecular cloud material in metal-rich carbonaceous chondrites

AU - van Kooten, Elishevah M. M. E.

AU - Wielandt, Daniel Kim Peel

AU - Schiller, Martin

AU - Nagashima, Kazuhide

AU - Thomen, Aurélien

AU - Larsen, Kirsten Kolbjørn

AU - Olsen, Mia Bjørg Stolberg

AU - Nordlund, Åke

AU - Krot, Alexander N.

AU - Bizzarro, Martin

PY - 2016/2/23

Y1 - 2016/2/23

N2 - The short-lived (26)Al radionuclide is thought to have been admixed into the initially (26)Al-poor protosolar molecular cloud before or contemporaneously with its collapse. Bulk inner Solar System reservoirs record positively correlated variability in mass-independent (54)Cr and (26)Mg*, the decay product of (26)Al. This correlation is interpreted as reflecting progressive thermal processing of in-falling (26)Al-rich molecular cloud material in the inner Solar System. The thermally unprocessed molecular cloud matter reflecting the nucleosynthetic makeup of the molecular cloud before the last addition of stellar-derived (26)Al has not been identified yet but may be preserved in planetesimals that accreted in the outer Solar System. We show that metal-rich carbonaceous chondrites and their components have a unique isotopic signature extending from an inner Solar System composition toward a (26)Mg*-depleted and (54)Cr-enriched component. This composition is consistent with that expected for thermally unprocessed primordial molecular cloud material before its pollution by stellar-derived (26)Al. The (26)Mg* and (54)Cr compositions of bulk metal-rich chondrites require significant amounts (25-50%) of primordial molecular cloud matter in their precursor material. Given that such high fractions of primordial molecular cloud material are expected to survive only in the outer Solar System, we infer that, similarly to cometary bodies, metal-rich carbonaceous chondrites are samples of planetesimals that accreted beyond the orbits of the gas giants. The lack of evidence for this material in other chondrite groups requires isolation from the outer Solar System, possibly by the opening of disk gaps from the early formation of gas giants.

AB - The short-lived (26)Al radionuclide is thought to have been admixed into the initially (26)Al-poor protosolar molecular cloud before or contemporaneously with its collapse. Bulk inner Solar System reservoirs record positively correlated variability in mass-independent (54)Cr and (26)Mg*, the decay product of (26)Al. This correlation is interpreted as reflecting progressive thermal processing of in-falling (26)Al-rich molecular cloud material in the inner Solar System. The thermally unprocessed molecular cloud matter reflecting the nucleosynthetic makeup of the molecular cloud before the last addition of stellar-derived (26)Al has not been identified yet but may be preserved in planetesimals that accreted in the outer Solar System. We show that metal-rich carbonaceous chondrites and their components have a unique isotopic signature extending from an inner Solar System composition toward a (26)Mg*-depleted and (54)Cr-enriched component. This composition is consistent with that expected for thermally unprocessed primordial molecular cloud material before its pollution by stellar-derived (26)Al. The (26)Mg* and (54)Cr compositions of bulk metal-rich chondrites require significant amounts (25-50%) of primordial molecular cloud matter in their precursor material. Given that such high fractions of primordial molecular cloud material are expected to survive only in the outer Solar System, we infer that, similarly to cometary bodies, metal-rich carbonaceous chondrites are samples of planetesimals that accreted beyond the orbits of the gas giants. The lack of evidence for this material in other chondrite groups requires isolation from the outer Solar System, possibly by the opening of disk gaps from the early formation of gas giants.

U2 - 10.1073/pnas.1518183113

DO - 10.1073/pnas.1518183113

M3 - Journal article

C2 - 26858438

SN - 0027-8424

VL - 113

SP - 2011

EP - 2016

JO - National Academy of Sciences. Proceedings

JF - National Academy of Sciences. Proceedings

IS - 8

ER -

Isotopic evidence for primordial molecular cloud material in metal-rich carbonaceous chondrites

Abstract

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