Siderophile element systematics of IAB complex iron meteorites: New insights into the formation of an enigmatic group

Worsham, E. A.; Bermingham, K. R.; Walker, Richard J.

doi:10.1016/j.gca.2016.05.019

Cited by 28 publications

(53 citation statements)

References 82 publications

(156 reference statements)

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“…Previously reported siderophile element abundances of bulk pieces of Canyon Diablo are reported in Table 2. The abundances of Ir, Pt, Rh, Ni, As, Ga, and Ge determined in the average host metal kamacite are within 5% of the bulk meteorite abundances (Jochum et al 1980; Wasson and Kallemeyn 2002; Worsham et al 2016). Abundances of Re, Ru, Co, Pd, and Au are within 11% and abundances of Os, W, Mo, and Cu differ between 21% and 62%.…”

Section: Resultsmentioning

confidence: 99%

“… * Data are from Worsham et al (2016) (Re, Os, Ir, Ru, Pt, Pd), Jochum et al (1980) (Mo, Rh), and Wasson and Kallemeyn (2002) (other elements). …”

Section: Resultsmentioning

confidence: 99%

“…The IAB iron meteorites are a large group of non‐magmatic iron meteorites referred to as the IAB complex (Wasson and Kallemeyn 2002). Some meteorites within this complex have disparate chemical and isotopic compositions, which have led to the division of the complex into several, possibly unrelated, subgroups (Worsham et al 2016, 2017). Of these, the “main group” (IAB‐MG) is the largest with over 100 members.…”

Section: Introductionmentioning

confidence: 99%

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Origin and age of metal veins in Canyon Diablo graphite nodules

Hilton

Ash

Piccoli

et al. 2020

Meteorit & Planetary Scien

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Previous studies attributed the origin of metal veins penetrating graphite nodules in the Canyon Diablo IAB main group iron meteorite to condensation from vapor or melting of host metal. Abundances of 16 siderophile elements measured in kamacite within vein and host meteorite are most consistent with an origin by melting of the host metal followed by fractional crystallization of the liquid. The presence of the veins within graphite nodules may be explained by impact, as peak shock temperatures, and thus the most likely areas to undergo metal melting, are at metal-graphite interfaces. The origin of the veins is constrained by Re-Os chronometry to have occurred early (>4 Ga) in solar system history.

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Section: Resultsmentioning

confidence: 99%

“… * Data are from Worsham et al (2016) (Re, Os, Ir, Ru, Pt, Pd), Jochum et al (1980) (Mo, Rh), and Wasson and Kallemeyn (2002) (other elements). …”

Section: Resultsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Origin and age of metal veins in Canyon Diablo graphite nodules

Hilton

Ash

Piccoli

et al. 2020

Meteorit & Planetary Scien

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“…Crystallization processes of IAB iron meteorites have been proposed as crystal segregation (Wasson and Kallemeyn ) or a combination of crystal segregation and fractional crystallization (Worsham et al. ) and these authors suggested that each IAB subgroup has its own origin. IAB‐sLL has the smallest compositional variation among IAB subgroups (Fig.…”

Section: Discussionmentioning

confidence: 99%

“… and references therein; Worsham et al. ). Although the previous studies using model calculations of metallic partial melting mainly discussed behavior of highly siderophile elements (HSEs), behavior of other siderophile and chalcophile elements should also be considered.…”

Section: Introductionmentioning

confidence: 99%

Siderophile element characteristics of acapulcoite–lodranites and winonaites: Implications for the early differentiation processes of their parent bodies

Hidaka

Shirai

Yamaguchi

et al. 2019

Meteorit & Planetary Scien

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We have studied magnetic fractions of five acapulcoites, three lodranites, and two winonaites to investigate chemical compositions of their precursor materials and metallic partial melting processes occurring on their parent bodies. One winonaite metal is similar in composition to low Au, low Ni IAB iron subgroup, indicating genetic relationship between them. Magnetic fractions of chondrule-bearing acapulcoite and winonaite have intermediate chemical compositions of metals between H chondrites and EL chondrites. This fact indicates that the precursor materials of acapulcoite-lodranites and winonaites were similar to H and/or EL chondrites in chemical compositions. Magnetic fractions in acapulcoitelodranites have a large variety of chemical compositions. Most of them show enrichments of W, Re, Ir, Pt, Mo, and Rh, and one of them shows clear depletion in Re and Ir relative to those of chondrule-bearing acapulcoite. Chemical compositional variations among acapulcoite-lodranite metals cannot be explained by a single Fe-Ni-S partial melting event, but a two-step partial melting model can explain it.

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Water Reservoirs in Small Planetary Bodies: Meteorites, Asteroids, and Comets

Alexander¹,

McKeegan²,

Altwegg³

2018

Space Sciences Series of ISSI

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Asteroids and comets are the remnants of the swarm of planetesimals from which the planets ultimately formed, and they retain records of processes that operated prior to and during planet formation. They are also likely the sources of most of the water and other volatiles accreted by Earth. In this review, we discuss the nature and probable origins of asteroids and comets based on data from remote observations, in situ measurements by spacecraft, and laboratory analyses of meteorites derived from asteroids. The asteroidal parent bodies of meteorites formed ≤4 Ma after Solar System formation while there was still a gas disk present. It seems increasingly likely that the parent bodies of meteorites spectroscopically linked with the E-, S-, M-and V-type asteroids formed sunward of Jupiter's orbit, while those associated with C-and, possibly, D-type asteroids formed further out, beyond Jupiter but probably not beyond Saturn's orbit. Comets formed further from the Sun than any of the meteorite parent bodies, and retain much higher abundances of interstellar material. CI and CM group meteorites are probably related to the most common C-type asteroids, and based on isotopic evidence they, rather than comets, are the most likely sources of the H and N accreted by the terrestrial planets. However, comets may have been major sources of the noble gases accreted by Earth and Venus. Possible constraints that these observations can place on models of giant planet formation and migration are explored.

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Siderophile element systematics of IAB complex iron meteorites: New insights into the formation of an enigmatic group

Cited by 28 publications

References 82 publications

Origin and age of metal veins in Canyon Diablo graphite nodules

Origin and age of metal veins in Canyon Diablo graphite nodules

Siderophile element characteristics of acapulcoite–lodranites and winonaites: Implications for the early differentiation processes of their parent bodies

Water Reservoirs in Small Planetary Bodies: Meteorites, Asteroids, and Comets

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