<sup>53</sup>Mn‐<sup>53</sup>Cr ages of Kaidun carbonates

Petitat, M.; Marrocchi, Yves; McKeegan, Kevin D.; Mostefaoui, S.; Meibom, Anders; Zolensky, M. E.; Gounelle, M.

doi:10.1111/j.1945-5100.2010.01150.x

Cited by 32 publications

(22 citation statements)

References 23 publications

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“…olivine or diopside) used in the present study and by previous workers (e.g. Hoppe et al, 2007;de Leuw et al, 2009b;Petitat et al, 2011). With the caveat that ages obtained using the different standards are not directly comparable, Fujiya et al (2012) found that carbonates from the four meteorites have an identical age of 4563.4 +0.4 -0.5 Ma (i.e.…”

Section: Carbonate Agesmentioning

confidence: 63%

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Extended chronologies of aqueous alteration in the CM2 carbonaceous chondrites: Evidence from carbonates in Queen Alexandra Range 93005

Lee

Lindgren

Sofe

et al. 2012

Geochimica et Cosmochimica Acta

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The Antarctic CM2 carbonaceous chondrite QUE 93005 contains four compositionally distinct carbonates, namely breunnerite, calcite, dolomite and a Ca-poor dolomite. These carbonates can form monomineralic grains, or may be intergrown as bimineralic grains consisting of dolomite plus breunnerite and dolomite plus calcite, or polymineralic grains containing an intergrowth of breunnerite, Ca-poor dolomite and calcite. Carbonates in all grain types have inclusions of Fe,Ni sulphides and/or Mg-Fe phyllosilicates. In the bimineralic grains dolomite crystallised first to be overgrown by breunnerite or partially replaced by calcite. Polymineralic grains are concentrically layered, with breunnerite crystallising first on pore margins to be later etched, then overgrown and partially replaced by Ca-poor dolomite that was itself partly dissolved prior to being overgrown by calcite. Calcite and dolomite have also cemented fractures that cross-cut the fine-grained rims to aqueously altered chondrules and were formed by expansion of the chondrules during their hydration. Overall, the sequence of mineralisation in QUE 93005 was: (1) dolomite, (2) breunnerite, (3) Ca-poor dolomite then (4) calcite. This secular change in carbonate composition and mineralogy reflects changing solution composition and probably also provenance. Mg-Fe phyllosilicates replaced dolomite, breunnerite and Ca-poor dolomite prior to calcite crystallisation and most or all of the sulphides formed after both the phyllosilicates and calcite. Following sulphide crystallisation the edges of carbonate grains were abraded, either by impact 'gardening' or as a consequence of fluidisation of the matrix during rapid loss of gas or vapour. Determination of the crystallisation age of dolomite via the Mn−Cr system indicates that aqueous alteration of QUE 93005 began on or before 3.93 ± 0.23 Ma after the formation of the solar system. Overall, the water/rock ratio and fO 2 during alteration of QUE 93005 was similar to that of the CM1s and CR1s, but the lower degree of alteration of QUE 93005 overall suggests that alteration timescales were shorter, possibly due to loss of intergranular liquid water during fluidisation.2

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Section: Carbonate Agesmentioning

confidence: 63%

“…Endress et al, 1996;Brearley et al, 2001;de Leuw et al, 2009a, b;Tyra et al, 2010a;Petitat et al, 2011;Fujiya et al, 2012). Naturally occurring Mn has one stable isotope, 55 Mn, and eighteen radioisotopes.…”

Section: Mn−cr Systematicsmentioning

confidence: 99%

Extended chronologies of aqueous alteration in the CM2 carbonaceous chondrites: Evidence from carbonates in Queen Alexandra Range 93005

Lee

Lindgren

Sofe

et al. 2012

Geochimica et Cosmochimica Acta

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“…The former indicate that alteration began soon after CAI formation and lasted <10 My Fujiya et al, 2013;Petitat et al, 2009Petitat et al, , 2011. Oxygen isotopic compositions of carbonates provide model-dependent temperatures under 50 C (see McSween et al, 2002).…”

Section: Thermal History and Modelingmentioning

confidence: 97%

Chondrites and Their Components

Scott

Krot

2014

Treatise on Geochemistry

153

101

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“…On the other hand, the W isotopic compositions of iron meteorites suggest their formation within 1.5 Myr after CAI formation 2 . If the carbonate ages of CI chondrites reported so far also have systematic errors, like those of the CM chondrites, they would become comparable with or younger than the carbonate ages of the CM chondrites 8,[10][11][12] . In any case, the early formation of hydrous asteroids suggested by old carbonates in CM chondrites is no longer well founded, and we conclude that hydrous asteroids accreted later than differentiated and metamorphosed asteroids.…”

Section: − +mentioning

confidence: 99%

“…5 and references therein), with ages comparable to the oldest solids in the Solar System (that is, calcium-aluminium-rich inclusions (CAIs); 4,568.2 million years ago (Myr ago) 6 ). Although the ages of the secondary minerals in CI chondrites (named for their type specimen of the Ivuna meteorite) may not be as old (4,567 to 4,554 Myr ago [7][8][9][10][11][12] ), one must conclude that at least some hydrous asteroids, such as the CM chondrite parent body, accreted very rapidly because the accretion time should be constrained by the oldest alteration product.…”

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confidence: 99%

Evidence for the late formation of hydrous asteroids from young meteoritic carbonates

et al. 2012

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The accretion of small bodies in the solar system is a fundamental process that was followed by planet formation. Chronological information of meteorites can constrain when asteroids formed. secondary carbonates show extremely old 53 mn-53 Cr radiometric ages, indicating that some hydrous asteroids accreted rapidly. However, previous studies have failed to define accurate mn/Cr ratios; hence, these old ages could be artefacts. Here we develop a new method for accurate mn/Cr determination, and report a reliable age of 4,563.4+0.4/-0.5 million years ago for carbonates in carbonaceous chondrites. We find that these carbonates have identical ages, which are younger than those previously estimated. This result suggests the late onset of aqueous activities in the solar system. The young carbonate age cannot be explained if the parent asteroid accreted within 3 million years after the birth of the solar system. Thus, we conclude that hydrous asteroids accreted later than differentiated and metamorphosed asteroids.

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⁵³Mn‐⁵³Cr ages of Kaidun carbonates

Abstract: Abstract-We report the 53 Mn-53

Cited by 32 publications

References 23 publications

Extended chronologies of aqueous alteration in the CM2 carbonaceous chondrites: Evidence from carbonates in Queen Alexandra Range 93005

Extended chronologies of aqueous alteration in the CM2 carbonaceous chondrites: Evidence from carbonates in Queen Alexandra Range 93005

Chondrites and Their Components

Evidence for the late formation of hydrous asteroids from young meteoritic carbonates

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53Mn‐53Cr ages of Kaidun carbonates

Abstract: Abstract-We report the 53 Mn-53

Cited by 32 publications

References 23 publications

Extended chronologies of aqueous alteration in the CM2 carbonaceous chondrites: Evidence from carbonates in Queen Alexandra Range 93005

Extended chronologies of aqueous alteration in the CM2 carbonaceous chondrites: Evidence from carbonates in Queen Alexandra Range 93005

Chondrites and Their Components

Evidence for the late formation of hydrous asteroids from young meteoritic carbonates

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Product

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⁵³Mn‐⁵³Cr ages of Kaidun carbonates