U‐Pb and Hf‐W dating of young zircon in mesosiderite Asuka 882023

Koike, Masao; Sugiura, N.; Takahata, Naoto; Ishida, Akizumi; Sano, Yuji

doi:10.1002/2016gl071609

Cited by 10 publications

(8 citation statements)

References 41 publications

(71 reference statements)

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“…The 207 Pb- 206 Pb dates of analysed zircons show two distinct populations (Fig. 1, Supplementary In previous studies, the younger ages were proposed to record either the timing of the metal-silicate mixing 14 or later local impacts 14,15 .…”

Section: High-precision 207 Pb-206 Pb Dates For Mesosiderite Zirconsmentioning

confidence: 90%

“…In situ 207 Pb- 206 Pb and Hf-W dates from a total of five zircons reveal a complex history with crystallization ages ranging from 4,563 Myr (ref. 13) to ~4,520 Myr (refs 14,15). The older dates were interpreted to correspond to the time of crust formation on the silicate parent body.…”

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confidence: 99%

“…Zircon [ZrSiO4] is a rare mineral in asteroidal meteorites, but was identified in mesosiderites [13][14][15] . In situ 207 Pb- 206 Pb and Hf-W dates from a total of five zircons reveal a complex history with crystallization ages ranging from 4,563 Myr (ref.…”

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confidence: 99%

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Mesosiderite formation on asteroid 4 Vesta by a hit-and-run collision

et al. 2019

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Collision and disruption processes of proto-planetary bodies in the early solar system are key to understanding the genesis of diverse types of main-belt asteroids. Mesosiderites are stony-iron meteorites that formed by mixing of howardite-eucrite-diogenite-like crust and molten core materials and provide unique insights into the catastrophic break-up of differentiated asteroids. However, the enigmatic formation process and the poorly constrained timing of metal-silicate mixing complicate the assignment to potential parent bodies. Here we report high-precision uranium-lead dating of mesosiderite zircons by isotope dilution thermal ionization mass spectrometry, revealing initial crust formation 4,558.5 ± 2.1 million years ago and metal-silicate mixing at 4,525.39 ± 0.85 million years.The two distinct ages coincide with the timing of crust formation and a large-scale reheating event on the eucrite parent body, likely the asteroid Vesta. This chronological coincidence corroborates that Vesta is the parent body of mesosiderite silicates.Mesosiderite formation on Vesta can be explained by a hit-and-run collision 4,525.4 million years ago that caused the thick crust observed by NASA's Dawn mission and explains the missing olivine in mesosiderites, howardite-eucrite-diogenite meteorites, and vestoids.

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Section: High-precision 207 Pb-206 Pb Dates For Mesosiderite Zirconsmentioning

confidence: 90%

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confidence: 99%

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Mesosiderite formation on asteroid 4 Vesta by a hit-and-run collision

et al. 2019

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“…However, below 500°C, they cooled much more slowly, 0.2-0.5°C Myr À1 , than any iron meteorites (Goldstein et al 2014). The timing of this reheating event is probably within~50 Ma of the parent body formation (Haba et al 2017;Koike et al 2017).…”

Section: Introductionmentioning

confidence: 90%

The most primitive mesosiderite Northwest Africa 1878, subgroup 0

Kimura

Sugiura

Yamaguchi

et al. 2020

Meteorit & Planetary Scien

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All mesosiderites previously reported were subjected to thermal metamorphism and/or partial melting on the parent body. Therefore, their primordial features have been mostly lost. Here, we report detailed petrological and mineralogical features on a mesosiderite, Northwest Africa (NWA) 1878. This meteorite comprises silicate lithology and aggregates of small spheroidal Fe-Ni metal grains. Silicate lithology typically shows igneous texture without recrystallization features, and mainly consists of low-Ca pyroxene and plagioclase. Pyroxenes often show normal zoning. Exsolution lamella of augite is rarely noticed and very thin in width, compared with other mesosiderites. A few magnesian olivine grains are encountered without typical corona texture around them. They are not equilibrated with pyroxene on a large scale. Plagioclase shows a wide compositional range. These results show that NWA 1878 hardly experienced thermal metamorphism, distinguished from mesosiderites of subgroups 1-4. Therefore, we propose that this is classified as subgroup 0 mesosiderite. Nevertheless, NWA 1878 was locally subjected to secondary reactions, such as weak reduction of pyroxene and Fe-Mg diffusion between olivine and pyroxene, on the parent body.

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“…In the giant impact scenario, measurements of highly siderophile element (HSE) concentrations would be interesting. Since the abundances of HSEs in the terrestrial and Martian mantles are similar and about 200 times lower than the chondritic abundances, the proportion of the impactor (chondritic) materials consisting of Phobos might be evaluated from HSE concentrations (Walker, 2009 An isotopic dichotomy between CCs and NCs is also clearly demonstrated by Mo isotopic ratios in ε 95 Mo versus ε 94 Mo space (ε 95 Mo versus ε 94 Mo denote parts per 10,000 deviations of 94 Pringle and Moynier, 2017). However, while the isotopic measurement of Zn has been actively optimized to utilize a minimum amount of material, those of other MVE have not, leaving the opportunity for improvements in the future and possibly in time for analysis of MMX material.…”

Section: Inorganic Analysesmentioning

confidence: 99%

Analytical Protocols for Phobos Regolith Samples Returned by the Martian Moons Exploration (MMX) Mission

Fujiya

Furukawa

Sugahara

et al. 2020

Preprint

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Japan Aerospace Exploration Agency (JAXA) will launch a spacecraft in 2024 for a sample return mission from Phobos (Martian Moons eXploration: MMX). Touchdown operations are planned to be performed twice at different landing sites on the Phobos surface to collect >10 g of the Phobos surface materials with coring and pneumatic sampling systems on board. The Sample Analysis Working Team (SAWT) of MMX is now designing analytical protocols of the returned Phobos samples to shed light on the origin of the Martian moons as well as the evolution of the Mars-moon system. Observations of petrology and mineralogy, and measurements of bulk chemical compositions and stable isotopic ratios of, e.g., O, Cr, and Ti can provide crucial information about the origin of Phobos. If Phobos is a captured asteroid composed of primitive chondritic materials, as inferred from its reflectance spectra, the nature of organic matter as well as bulk H, N, and Zn isotopic compositions characterize the volatile materials in the samples and constrain the type of the captured asteroid. Cosmogenic and solar wind components, most pronounced in noble gas isotopic compositions, can reveal surface processes on Phobos. Long- and short-lived radionuclide chronometry such as 53Mn-53Cr and 87Rb-87Sr systematics can date pivotal events like impacts, thermal metamorphism, and aqueous alteration on Phobos. It should be noted that the Phobos regolith is expected to contain a small amount of materials delivered from Mars, which may be physically and chemically different from any Martian meteorites in our collection and thus are particularly precious. The analysis plan will be designed to detect such Martian materials, if any, from the returned samples dominated by the Phobos building blocks in curation procedures at JAXA before they are processed for further analyses.

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U‐Pb and Hf‐W dating of young zircon in mesosiderite Asuka 882023

Cited by 10 publications

References 41 publications

Mesosiderite formation on asteroid 4 Vesta by a hit-and-run collision

Mesosiderite formation on asteroid 4 Vesta by a hit-and-run collision

The most primitive mesosiderite Northwest Africa 1878, subgroup 0

Analytical Protocols for Phobos Regolith Samples Returned by the Martian Moons Exploration (MMX) Mission

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