The origin of inner Solar System water
Of the potential volatile sources for the terrestrial planets, the CI and CM carbonaceous chondrites are closest to the planets' bulk H and N isotopic compositions. For the Earth, the addition of approximately 2–4 wt% of CI/CM material to a volatile-depleted proto-Earth can explain the abundanc...
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ftpubmed:oai:pubmedcentral.nih.gov:5394251 2023-05-15T18:30:05+02:00 The origin of inner Solar System water Alexander, Conel M. O'D. 2017-05-28 http://www.ncbi.nlm.nih.gov/pmc/articles/PMC5394251/ http://www.ncbi.nlm.nih.gov/pubmed/28416723 https://doi.org/10.1098/rsta.2015.0384 en eng The Royal Society Publishing http://www.ncbi.nlm.nih.gov/pmc/articles/PMC5394251/ http://www.ncbi.nlm.nih.gov/pubmed/28416723 http://dx.doi.org/10.1098/rsta.2015.0384 © 2017 The Author(s) http://royalsocietypublishing.org/licence Published by the Royal Society. All rights reserved. Articles Text 2017 ftpubmed https://doi.org/10.1098/rsta.2015.0384 2018-06-03T00:06:40Z Of the potential volatile sources for the terrestrial planets, the CI and CM carbonaceous chondrites are closest to the planets' bulk H and N isotopic compositions. For the Earth, the addition of approximately 2–4 wt% of CI/CM material to a volatile-depleted proto-Earth can explain the abundances of many of the most volatile elements, although some solar-like material is also required. Two dynamical models of terrestrial planet formation predict that the carbonaceous chondrites formed either in the asteroid belt (‘classical’ model) or in the outer Solar System (5–15 AU in the Grand Tack model). To test these models, at present the H isotopes of water are the most promising indicators of formation location because they should have become increasingly D-rich with distance from the Sun. The estimated initial H isotopic compositions of water accreted by the CI, CM, CR and Tagish Lake carbonaceous chondrites were much more D-poor than measured outer Solar System objects. A similar pattern is seen for N isotopes. The D-poor compositions reflect incomplete re-equilibration with H2 in the inner Solar System, which is also consistent with the O isotopes of chondritic water. On balance, it seems that the carbonaceous chondrites and their water did not form very far out in the disc, almost certainly not beyond the orbit of Saturn when its moons formed (approx. 3–7 AU in the Grand Tack model) and possibly close to where they are found today. Text Tagish PubMed Central (PMC) Tagish ENVELOPE(-134.272,-134.272,60.313,60.313) Tagish Lake ENVELOPE(-134.233,-134.233,59.717,59.717) Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences 375 2094 20150384 |
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Articles Alexander, Conel M. O'D. The origin of inner Solar System water |
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Of the potential volatile sources for the terrestrial planets, the CI and CM carbonaceous chondrites are closest to the planets' bulk H and N isotopic compositions. For the Earth, the addition of approximately 2–4 wt% of CI/CM material to a volatile-depleted proto-Earth can explain the abundances of many of the most volatile elements, although some solar-like material is also required. Two dynamical models of terrestrial planet formation predict that the carbonaceous chondrites formed either in the asteroid belt (‘classical’ model) or in the outer Solar System (5–15 AU in the Grand Tack model). To test these models, at present the H isotopes of water are the most promising indicators of formation location because they should have become increasingly D-rich with distance from the Sun. The estimated initial H isotopic compositions of water accreted by the CI, CM, CR and Tagish Lake carbonaceous chondrites were much more D-poor than measured outer Solar System objects. A similar pattern is seen for N isotopes. The D-poor compositions reflect incomplete re-equilibration with H2 in the inner Solar System, which is also consistent with the O isotopes of chondritic water. On balance, it seems that the carbonaceous chondrites and their water did not form very far out in the disc, almost certainly not beyond the orbit of Saturn when its moons formed (approx. 3–7 AU in the Grand Tack model) and possibly close to where they are found today. |
format |
Text |
author |
Alexander, Conel M. O'D. |
author_facet |
Alexander, Conel M. O'D. |
author_sort |
Alexander, Conel M. O'D. |
title |
The origin of inner Solar System water |
title_short |
The origin of inner Solar System water |
title_full |
The origin of inner Solar System water |
title_fullStr |
The origin of inner Solar System water |
title_full_unstemmed |
The origin of inner Solar System water |
title_sort |
origin of inner solar system water |
publisher |
The Royal Society Publishing |
publishDate |
2017 |
url |
http://www.ncbi.nlm.nih.gov/pmc/articles/PMC5394251/ http://www.ncbi.nlm.nih.gov/pubmed/28416723 https://doi.org/10.1098/rsta.2015.0384 |
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ENVELOPE(-134.272,-134.272,60.313,60.313) ENVELOPE(-134.233,-134.233,59.717,59.717) |
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Tagish Tagish Lake |
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Tagish Tagish Lake |
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Tagish |
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Tagish |
op_relation |
http://www.ncbi.nlm.nih.gov/pmc/articles/PMC5394251/ http://www.ncbi.nlm.nih.gov/pubmed/28416723 http://dx.doi.org/10.1098/rsta.2015.0384 |
op_rights |
© 2017 The Author(s) http://royalsocietypublishing.org/licence Published by the Royal Society. All rights reserved. |
op_doi |
https://doi.org/10.1098/rsta.2015.0384 |
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Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences |
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375 |
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2094 |
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20150384 |
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1766213569210220544 |