26Al-26Mg deficit dating ultramafic meteorites and silicate planetesimal differentiation in the early Solar System?

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26Al-26Mg deficit dating ultramafic meteorites and silicate planetesimal differentiation in the early Solar System? / Baker, Joel A.; Schiller, Martin; Bizzarro, Martin.

In: Geochimica et Cosmochimica Acta, Vol. 77, 2012, p. 415-431.

Research output: Contribution to journal › Journal article › Research › peer-review

Harvard

Baker, JA, Schiller, M & Bizzarro, M 2012, '26Al-26Mg deficit dating ultramafic meteorites and silicate planetesimal differentiation in the early Solar System?', Geochimica et Cosmochimica Acta, vol. 77, pp. 415-431. https://doi.org/10.1016/j.gca.2011.10.030

APA

Baker, J. A., Schiller, M., & Bizzarro, M. (2012). 26Al-26Mg deficit dating ultramafic meteorites and silicate planetesimal differentiation in the early Solar System? Geochimica et Cosmochimica Acta, 77, 415-431. https://doi.org/10.1016/j.gca.2011.10.030

Vancouver

Baker JA, Schiller M, Bizzarro M. 26Al-26Mg deficit dating ultramafic meteorites and silicate planetesimal differentiation in the early Solar System? Geochimica et Cosmochimica Acta. 2012;77:415-431. https://doi.org/10.1016/j.gca.2011.10.030

Author

Baker, Joel A. ; Schiller, Martin ; Bizzarro, Martin. / 26Al-26Mg deficit dating ultramafic meteorites and silicate planetesimal differentiation in the early Solar System?. In: Geochimica et Cosmochimica Acta. 2012 ; Vol. 77. pp. 415-431.

Bibtex

@article{8ce56266781f4517941759f956607fc0,
title = "26Al-26Mg deficit dating ultramafic meteorites and silicate planetesimal differentiation in the early Solar System?",
abstract = "Meteorites with significantly sub-chondritic Al/Mg that formed in the first 2million years of the Solar System should be characterised by deficits in the abundance of Mg (d Mg ) due to the absence of in-growth of Mg from the decay of short-lived Al (t =0.73Myr). However, these Mg deficits will be small (d Mg >-0.037‰) even for material that formed at the same time as the Solar System's oldest solids - calcium-aluminium-rich inclusions - and thus measurement of these deficits is analytically challenging.Here, we report on a search for Mg deficits in three types of ultramafic meteorites (pallasites, ureilites and aubrites) by multiple-collector inductively coupled plasma mass spectrometry. A range of analytical tests were carried out including analysis of: (1) a range of synthetic Mg solution standards; (2) Mg gravimetrically doped with a high purity Mg spike; (3) Mg cuts collected sequentially from cation exchange separation columns with fractionated stable Mg isotope compositions; (4) Mg separated from samples that was bracketed by analyses of both DSM-3 and Mg separated from a natural olivine sample subjected to the same chemical processing as the samples. These tests confirm it is possible to resolve differences in d Mg from the terrestrial materials that are =0.005‰. However, if Mg yields from chemical separation are low or an inappropriate equilibrium-isotopically fractionated standard is used this will generate analytical artefacts on d Mg when this is calculated with the kinetic/exponential mass fractionation law as is the case when correcting for instrumental mass bias during mass spectrometric analysis.Olivine from four different main group pallasites and four bulk ureilites have small deficits in the abundance of Mg with d26MgDSM-3*=-0.0120±0.0018‰ and d26MgDSM-3*=-0.0062±0.0023‰, respectively, relative to terrestrial olivine (d26MgDSM-3*=+0.0029±0.0028‰). Six aubrites have d26MgDSM-3*=+0.0015±0.0020‰, which is identical to terrestrial olivine.Model ages from these deficits can be calculated by assuming that Al was homogeneously distributed in the planetesimal-forming regions of the proto-planetary disc at the same level as calcium-aluminium-rich inclusions (CAIs). The absence of Mg deficits in aubrites, means these can only be constrained to have formed relatively late >2.9Myr after CAI formation. Model ages calculated from pallasite olivine deficits would suggest that pallasite olivine crystallised and was diffusively isolated on its parent body 1.24-0.28+0.40Myr after formation of CAIs. Similarly, ureilites would have experienced silicate partial melting and lowering of their bulk Al/Mg ratios 1.9-0.7+2.2Myr after CAI formation. The model ages for silicate differentiation on the main group pallasite parent body are intermediate between those for metal-silicate fractionation for core formation obtained from magmatic iron meteorites and those for asteroidal silicate magmatism obtained from basaltic meteorites.",
author = "Baker, {Joel A.} and Martin Schiller and Martin Bizzarro",
year = "2012",
doi = "10.1016/j.gca.2011.10.030",
language = "English",
volume = "77",
pages = "415--431",
journal = "Geochimica et Cosmochimica Acta",
issn = "0016-7037",
publisher = "Pergamon Press",

}

RIS

TY - JOUR

T1 - 26Al-26Mg deficit dating ultramafic meteorites and silicate planetesimal differentiation in the early Solar System?

AU - Baker, Joel A.

AU - Schiller, Martin

AU - Bizzarro, Martin

PY - 2012

Y1 - 2012

N2 - Meteorites with significantly sub-chondritic Al/Mg that formed in the first 2million years of the Solar System should be characterised by deficits in the abundance of Mg (d Mg ) due to the absence of in-growth of Mg from the decay of short-lived Al (t =0.73Myr). However, these Mg deficits will be small (d Mg >-0.037‰) even for material that formed at the same time as the Solar System's oldest solids - calcium-aluminium-rich inclusions - and thus measurement of these deficits is analytically challenging.Here, we report on a search for Mg deficits in three types of ultramafic meteorites (pallasites, ureilites and aubrites) by multiple-collector inductively coupled plasma mass spectrometry. A range of analytical tests were carried out including analysis of: (1) a range of synthetic Mg solution standards; (2) Mg gravimetrically doped with a high purity Mg spike; (3) Mg cuts collected sequentially from cation exchange separation columns with fractionated stable Mg isotope compositions; (4) Mg separated from samples that was bracketed by analyses of both DSM-3 and Mg separated from a natural olivine sample subjected to the same chemical processing as the samples. These tests confirm it is possible to resolve differences in d Mg from the terrestrial materials that are =0.005‰. However, if Mg yields from chemical separation are low or an inappropriate equilibrium-isotopically fractionated standard is used this will generate analytical artefacts on d Mg when this is calculated with the kinetic/exponential mass fractionation law as is the case when correcting for instrumental mass bias during mass spectrometric analysis.Olivine from four different main group pallasites and four bulk ureilites have small deficits in the abundance of Mg with d26MgDSM-3*=-0.0120±0.0018‰ and d26MgDSM-3*=-0.0062±0.0023‰, respectively, relative to terrestrial olivine (d26MgDSM-3*=+0.0029±0.0028‰). Six aubrites have d26MgDSM-3*=+0.0015±0.0020‰, which is identical to terrestrial olivine.Model ages from these deficits can be calculated by assuming that Al was homogeneously distributed in the planetesimal-forming regions of the proto-planetary disc at the same level as calcium-aluminium-rich inclusions (CAIs). The absence of Mg deficits in aubrites, means these can only be constrained to have formed relatively late >2.9Myr after CAI formation. Model ages calculated from pallasite olivine deficits would suggest that pallasite olivine crystallised and was diffusively isolated on its parent body 1.24-0.28+0.40Myr after formation of CAIs. Similarly, ureilites would have experienced silicate partial melting and lowering of their bulk Al/Mg ratios 1.9-0.7+2.2Myr after CAI formation. The model ages for silicate differentiation on the main group pallasite parent body are intermediate between those for metal-silicate fractionation for core formation obtained from magmatic iron meteorites and those for asteroidal silicate magmatism obtained from basaltic meteorites.

AB - Meteorites with significantly sub-chondritic Al/Mg that formed in the first 2million years of the Solar System should be characterised by deficits in the abundance of Mg (d Mg ) due to the absence of in-growth of Mg from the decay of short-lived Al (t =0.73Myr). However, these Mg deficits will be small (d Mg >-0.037‰) even for material that formed at the same time as the Solar System's oldest solids - calcium-aluminium-rich inclusions - and thus measurement of these deficits is analytically challenging.Here, we report on a search for Mg deficits in three types of ultramafic meteorites (pallasites, ureilites and aubrites) by multiple-collector inductively coupled plasma mass spectrometry. A range of analytical tests were carried out including analysis of: (1) a range of synthetic Mg solution standards; (2) Mg gravimetrically doped with a high purity Mg spike; (3) Mg cuts collected sequentially from cation exchange separation columns with fractionated stable Mg isotope compositions; (4) Mg separated from samples that was bracketed by analyses of both DSM-3 and Mg separated from a natural olivine sample subjected to the same chemical processing as the samples. These tests confirm it is possible to resolve differences in d Mg from the terrestrial materials that are =0.005‰. However, if Mg yields from chemical separation are low or an inappropriate equilibrium-isotopically fractionated standard is used this will generate analytical artefacts on d Mg when this is calculated with the kinetic/exponential mass fractionation law as is the case when correcting for instrumental mass bias during mass spectrometric analysis.Olivine from four different main group pallasites and four bulk ureilites have small deficits in the abundance of Mg with d26MgDSM-3*=-0.0120±0.0018‰ and d26MgDSM-3*=-0.0062±0.0023‰, respectively, relative to terrestrial olivine (d26MgDSM-3*=+0.0029±0.0028‰). Six aubrites have d26MgDSM-3*=+0.0015±0.0020‰, which is identical to terrestrial olivine.Model ages from these deficits can be calculated by assuming that Al was homogeneously distributed in the planetesimal-forming regions of the proto-planetary disc at the same level as calcium-aluminium-rich inclusions (CAIs). The absence of Mg deficits in aubrites, means these can only be constrained to have formed relatively late >2.9Myr after CAI formation. Model ages calculated from pallasite olivine deficits would suggest that pallasite olivine crystallised and was diffusively isolated on its parent body 1.24-0.28+0.40Myr after formation of CAIs. Similarly, ureilites would have experienced silicate partial melting and lowering of their bulk Al/Mg ratios 1.9-0.7+2.2Myr after CAI formation. The model ages for silicate differentiation on the main group pallasite parent body are intermediate between those for metal-silicate fractionation for core formation obtained from magmatic iron meteorites and those for asteroidal silicate magmatism obtained from basaltic meteorites.

U2 - 10.1016/j.gca.2011.10.030

DO - 10.1016/j.gca.2011.10.030

M3 - Journal article

AN - SCOPUS:84855515857

VL - 77

SP - 415

EP - 431

JO - Geochimica et Cosmochimica Acta

JF - Geochimica et Cosmochimica Acta

SN - 0016-7037

ER -

ID: 45193418