Highly siderophile element evidence for early solar system processes in components from ordinary chondrites

AbstractWe report I-Xe ages and other relevant xenon data for seven ordinary chondrites from H and L-groups of petrologic types 4-6, which were selected on the basis of minimum weathering and shock effects. Nevertheless, no chronological order with respect to the I-Xe ages exists among the different petrologic types. We demonstrate, however, that the degree to which the 1-Xe record is preserved in these chondrites, but not necessarily the age, is dependent on the thermal metamorphic history. In order to explain the lack of chronological order among the chondrites, spatiotemporal variations in the condensation-accretion process or inhomogeneities in the isotopic composition of iodine in the solar nebula is required.

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Petrology and oxygen isotopic composition of large igneous inclusions in ordinary chondrites: Early solar system igneous processes and oxygen reservoirs

Geochimica et Cosmochimica Acta ◽

10.1016/j.gca.2019.01.017 ◽

2019 ◽

Vol 266 ◽

pp. 497-528 ◽

Cited By ~ 7

Author(s):

Alex M. Ruzicka ◽

Richard C. Greenwood ◽

Katherine Armstrong ◽

Kristy L. Schepker ◽

Ian A. Franchi

Keyword(s):

Solar System ◽

Isotopic Composition ◽

Oxygen Isotopic Composition ◽

Ordinary Chondrites ◽

Early Solar System ◽

Oxygen Isotopic

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The iodine-xenon system in clasts and chondrules from ordinary chondrites: Implications for early solar system chronology

Meteoritics and Planetary Science ◽

10.1111/j.1945-5100.2000.tb01427.x ◽

2000 ◽

Vol 35 (3) ◽

pp. 445-455 ◽

Cited By ~ 24

Author(s):

J. D. GILMOUR ◽

J. A. WHITBY ◽

G. TURNER ◽

J. C. BRIDGES ◽

R. HUTCHISON

Keyword(s):

Solar System ◽

Ordinary Chondrites ◽

Early Solar System

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The magnetism of meteorites and early Solar System magnetic fields

Philosophical Transactions of the Royal Society of London Series A Physical and Engineering Sciences ◽

10.1098/rsta.1994.0124 ◽

1994 ◽

Vol 349 (1690) ◽

pp. 197-207 ◽

Cited By ~ 5

Keyword(s):

Solar System ◽

Remanent Magnetization ◽

Parent Body ◽

Primary Component ◽

Carbonaceous Chondrites ◽

Ordinary Chondrites ◽

Early Solar System ◽

History Of ◽

Magnetizing Field ◽

Feni Alloy

The characteristics of the remanent magnetization of chondrite, achondrite and shergottite, nakhlite and chassignite (SNC) meteorites are described, and interpretation in terms of magnetizing fields in the ancient Solar System discussed. The magnetism of ordinary chondrites is commonly scattered in direction within samples, implying magnetization of constituent fragments before accumulation. The magnetic history of these meteorites is uncertain because of lack of knowledge of the origin and properties of tetrataenite, an ordered FeNi alloy often carrying the bulk of the magnetization. Achondrites also often possess scattered magnetization, the primary component probably being acquired during cooling after differentiation of the parent body. A magnetizing field of internal origin is possible. Estimates of magnetizing field strength are in the approximate range 5-100 μ T, with carbonaceous chondrites showing the highest values. The SNC meteorites, probably originating on Mars, provide evidence for a weak, ancient Martian magnetic field of the order 1 μ T.

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Xenoliths in ordinary chondrites and ureilites: Implications for early solar system dynamics

Meteoritics and Planetary Science ◽

10.1111/maps.13738 ◽

2021 ◽

Author(s):

Cyrena Anne Goodrich ◽

David A. Kring ◽

Richard C. Greenwood ◽

Adrian Brearley

Keyword(s):

Solar System ◽

System Dynamics ◽

Ordinary Chondrites ◽

Early Solar System ◽

Solar System Dynamics

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Potassium isotope compositions of carbonaceous and ordinary chondrites: Implications on the origin of volatile depletion in the early solar system

Geochimica et Cosmochimica Acta ◽

10.1016/j.gca.2020.03.018 ◽

2020 ◽

Vol 277 ◽

pp. 111-131 ◽

Cited By ~ 5

Author(s):

Hannah Bloom ◽

Katharina Lodders ◽

Heng Chen ◽

Chen Zhao ◽

Zhen Tian ◽

...

Keyword(s):

Solar System ◽

Ordinary Chondrites ◽

Early Solar System

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Laboratory and in-situ analysis of comet dust

Proceedings, annual meeting, Electron Microscopy Society of America ◽

10.1017/s0424820100102122 ◽

1988 ◽

Vol 46 ◽

pp. 8-9

Author(s):

D.E. Brownlee ◽

A.L. Albee

Keyword(s):

Electron Microscopy ◽

Solar System ◽

Laboratory Study ◽

Isotopic Analysis ◽

Building Blocks ◽

Sem Analysis ◽

Early Solar System ◽

Cometary Material ◽

Comet Dust

Comets are primitive, kilometer-sized bodies that formed in the outer regions of the solar system. Composed of ice and dust, comets are generally believed to be relic building blocks of the outer solar system that have been preserved at cryogenic temperatures since the formation of the Sun and planets. The analysis of cometary material is particularly important because the properties of cometary material provide direct information on the processes and environments that formed and influenced solid matter both in the early solar system and in the interstellar environments that preceded it.The first direct analyses of proven comet dust were made during the Soviet and European spacecraft encounters with Comet Halley in 1986. These missions carried time-of-flight mass spectrometers that measured mass spectra of individual micron and smaller particles. The Halley measurements were semi-quantitative but they showed that comet dust is a complex fine-grained mixture of silicates and organic material. A full understanding of comet dust will require detailed morphological, mineralogical, elemental and isotopic analysis at the finest possible scale. Electron microscopy and related microbeam techniques will play key roles in the analysis. The present and future of electron microscopy of comet samples involves laboratory study of micrometeorites collected in the stratosphere, in-situ SEM analysis of particles collected at a comet and laboratory study of samples collected from a comet and returned to the Earth for detailed study.

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