Early aqueous activity on primitive meteorite parent bodies

Endress, M.; Zinner, E.; Bischoff, A.

doi:10.1038/379701a0

Cited by 163 publications

(109 citation statements)

References 10 publications

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“…CI meteorite Orgueil shows signs of extensive aqueous alteration being devoid of chondrules that are most probably destroyed during this process. The most abundant mineral phases in Orgueil are magnetites and carbonates with the latter formed in the very early stages of aqueous alteration on the CI parent body (Endress et al 1996). These carbonates are believed to have precipitated from aqueous solution circulating on the CI parent body (Endress & Bischoff 1995).…”

Section: Discussionmentioning

confidence: 99%

Near infra-red spectroscopy of the asteroid 21 Lutetia

Nedelcu

Birlan²,

Vernazza³

et al. 2007

A&A

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Aims. In the framework of the ground-based science campaign dedicated to the encounter with the Rosetta spacecraft, the mineralogy of the asteroid (21) Lutetia was investigated. Methods. Near-infrared (NIR) spectra of the asteroid in the 0.8−2.5 µm spectral range were obtained with SpeX/IRTF in remote observing mode from Meudon, France in March and April 2006. We analysed these data together with previously acquired spectra -March 2003, August 2004. I-band relative photometric data obtained on 20 January 2006 using the 105 cm telescope from Pic du Midi, France has been used to build the ephemeris for physical observations. A χ 2 test using meteorite spectra from the RELAB database was performed in order to find the best fit of complete visible + infrared (VNIR) spectra of Lutetia. Results. The new spectra reveal no absorption features. We find a clear spectral variation (slope), and a good correspondence between spectral variations and rotational phase. Two of the most different spectra correspond to two opposite sides of the asteroid (sub-Earth longitude difference around 180 • ). For the neutral spectra a carbonaceous chondrite spectrum yields the best fit, while for those with a slightly positive slope the enstatitic chondrite spectra are the best analog. Based on the chosen subset of the meteorite samples, our analysis suggests a primitive, chondritic nature for (21) Lutetia. Differences in spectra are interpreted in terms of the coexistence of several lithologies on the surface where the aqueous alteration played an important role.

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Section: Discussionmentioning

confidence: 99%

Near infra-red spectroscopy of the asteroid 21 Lutetia

Nedelcu

Birlan²,

Vernazza³

et al. 2007

A&A

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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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“…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 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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Early aqueous activity on primitive meteorite parent bodies

Cited by 163 publications

References 10 publications

Near infra-red spectroscopy of the asteroid 21 Lutetia

Near infra-red spectroscopy of the asteroid 21 Lutetia

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

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

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