Accretionary dust mantles in CM chondrites: Evidence for solar nebula processes

Metzler, K.; Bischoff, A.; Stöffler, D.

doi:10.1016/0016-7037(92)90365-p

Cited by 348 publications

(506 citation statements)

References 33 publications

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“…A fascinating question is: whether primary accretionary rocks (PARs) are able to survive such a long period without substantial processing. Metzler et al (1992) coined the PAR term in order to describe very primitive (essentially unaltered ) CM chondrites. We use the same terminology in a general sense (to describe the first rocks that evolved to the present chondrites) although we disagree with Metzler's interpretation.…”

Section: Packing Densities and Tensile Strengths Of Primitive Meteoritesmentioning

confidence: 99%

“…We use the same terminology in a general sense (to describe the first rocks that evolved to the present chondrites) although we disagree with Metzler's interpretation. Basically, Metzler et al (1992) described the presence of fine-grained dust mantles around chondrules in CM chondrites and interpreted them as fine-dust material sticking to the chondrules, which have been preserved from the nebular accretionary stage. However, examined nine CM chondrites and concluded that these mantles can be produced by impact-induced shear of a porous precursor that later on suffered extensive aqueous alteration.…”

Section: Packing Densities and Tensile Strengths Of Primitive Meteoritesmentioning

confidence: 99%

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The Physics of Protoplanetesimal Dust Agglomerates. I. Mechanical Properties and Relations to Primitive Bodies in the Solar System

Blum

Schräpler

Davidsson

et al. 2006

ApJ

181

217

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We present laboratory experiments on the formation of macroscopic dust aggregates. The centimeter-sized highly porous bodies are produced by random ballistic deposition from individual micrometer-sized dust particles. We find packing densities between 0.07 and 0.15 for uncompressed samples, dependent on the shape and size distribution of the constituent dust grains. Impacts into these bodies are simulated by uniaxial compression experiments. We find that the maximum compression, equivalent to the highest protoplanetary impact velocities of $50 m s À1 , increases the packing density to 0.20-0.33. Tensile strength measurements with our laboratory samples yield values in the range 200-1100 Pa for slightly compressed samples. We review packing densities and tensile strengths found for primitive solar system bodies, e.g., for comets, primitive meteorites, and meteoroids. We find a consistency between packing densities and tensile strengths of our laboratory samples with those from cometary origin.

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Section: Packing Densities and Tensile Strengths Of Primitive Meteoritesmentioning

confidence: 99%

Section: Packing Densities and Tensile Strengths Of Primitive Meteoritesmentioning

confidence: 99%

The Physics of Protoplanetesimal Dust Agglomerates. I. Mechanical Properties and Relations to Primitive Bodies in the Solar System

Blum

Schräpler

Davidsson

et al. 2006

ApJ

181

217

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show abstract

“…As bare chondrules move through a dusty disk they would collect the dust. This dust is compressed to the observed rims, eventually (Bland et al 2011;Metzler et al 1992;Ormel et al 2008;Morfill et al 1998;Carballido 2011).…”

Section: Introductionmentioning

confidence: 96%

Thermal and photophoretic properties of dust mantled chondrules and sorting in the solar nebula

Loesche

Wurm

2012

A&A

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Many chondrules are found to be surrounded by a fine grained rim. Supposedly, these rims were acquired from dust accreted to the chondrules in a protoplanetary disk. In numerical simulations we study the heat transfer in illuminated bare and dust mantled chondrules. The calculations consider the chondrule size, the dust mantle size, and the thermal conductivities of both components as parameters. We calculate the photophoretic force and compare the numerical results to analytical approximations. We give an expression to quantify the photophoretic force on a spherical particle in the free molecular regime to better than 2%. We describe the influence of a dust mantle on the photophoretic strength by an effective thermal conductivity of the core-mantle particle. The effective thermal conductivity significantly depends on the size ratio between mantle and chondrule but not on the absolute sizes. It also strongly depends on the thermal conductivity of the mantle with minor influence of the thermal conductivity of the chondrule. The size ratio between rim and chondrule in meteorites is found to vary systematically with overall size by other authors. Based on this, our calculations show that a photophoretic size sorting can occur for dust mantled chondrules in optically thin disks or at the evolving inner edge of the solar nebula.

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“…A number of previous workers (e.g., Tomeoka and Buseck, 1985;Metzler et al, 1992;Browning et al, 1996;Bischoff, 1998;Hanowski and Brearley, 2001;Jones and Brearley, 2006;Chizmadia and Brearley, 2008) discussed the mechanism, condition and location of aqueous alteration in the CM chondrites. However, it is still controversial whether the aqueous alteration occurred in the solar nebula (e.g., Metzler et al, 1992;Bischoff, 1998) or on the meteorite parent bodies (e.g., Browning et al, 1996;Chizmadia and Brearley, 2008). Because progressive aqueous alteration on the parent bodies probably overwrote the earlier alteration history, it is desirable to investigate meteorites that have experienced aqueous alteration as little as possible to unravel the earliest alteration process.…”

Section: Introductionmentioning

confidence: 99%

Early aqueous alteration process in the QUE97990 and Y791198 CM carbonaceous chondrites

Maeda

Tomeoka

Seto

2009

Journal of Mineralogical and Petrological Sciences

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Queen Alexandra Range 97990 (QUE97990) and Yamato 791198 (Y791198) are among the least aqueously altered CM carbonaceous chondrites known to date. Our mineralogical and petrographic study reveals that chondrule mesostases in QUE97990 contain dense arrays of parallel, thin lath -shaped crystallites of diopside. The diopside crystallites are primary quenched products formed during chondrule formation. Thus their presence suggests that QUE97990 preserves a very early state of aqueous alteration. On the other hand, chondrule mesostases in Y791198 consist largely of serpentine without such quenched crystallites. In Y791198, quenched crystallites have probably been replaced by serpentine due to a higher degree of alteration than in QUE97990. Our study also reveals that chondrules in both QUE97990 and Y791198 show topographic depressions on their surfaces. The texture and mineralogy of the depressions suggest that they formed by replacing opaque nodules in their host chondrules during aqueous alteration. These imply that, in spite of the evidence of incipient alteration in the chondrule interiors, there was considerable alteration reaction between the chondrule margins and their surrounding rims in QUE97990. We suggest that the aqueous alteration in both meteorites occurred after the chondrules acquired their own rims on the meteorite parent bodies.

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Accretionary dust mantles in CM chondrites: Evidence for solar nebula processes

Cited by 348 publications

References 33 publications

The Physics of Protoplanetesimal Dust Agglomerates. I. Mechanical Properties and Relations to Primitive Bodies in the Solar System

The Physics of Protoplanetesimal Dust Agglomerates. I. Mechanical Properties and Relations to Primitive Bodies in the Solar System

Thermal and photophoretic properties of dust mantled chondrules and sorting in the solar nebula

Early aqueous alteration process in the QUE97990 and Y791198 CM carbonaceous chondrites

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