The Yamato-type (CY) carbonaceous chondrite group: Analogues for the surface of asteroid Ryugu?

King, A. J.; Bates, H. C.; Krietsch, Daniela; Busemann, H.; Clay, P. L.; Schofield, P. F.; Russell, S. S.

doi:10.1016/j.chemer.2019.08.003

Cited by 93 publications

(115 citation statements)

References 72 publications

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“…This average abundance matches that observed in petrographic observations of this group (Scott & Krot 2014). The most 18 O-and 17 O-rich material that falls close to or on this CO-CM line is the matrix of WIS 91600, Tagish Lake, the CI chondrites and heated CI-like (CY) chondrites (King et al 2019). The matrix of the CM and CO chondrites can, therefore, be expressed as a mixture of distal (matrix of WIS 91600, Tagish Lake, CI chondrites and CI-like -3.5 Myr after CAI formation; Kruahashi et al 2008;Fujiya et al 2012;Doyle et al 2015).…”

Section: Constraints On the Migration Of Micrometer-sized Materials Ansupporting

confidence: 85%

Constraints on the Distances and Timescales of Solid Migration in the Early Solar System from Meteorite Magnetism

Bryson

Weiss

Biersteker

et al. 2020

ApJ

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The migrations of solid objects throughout the solar system are thought to have played key roles in disk evolution and planet formation. However, our understanding of these migrations is limited by a lack of quantitative constraints on their timings and distances recovered from laboratory measurements of meteorites. The protoplanetary disk supported a magnetic field that decreased in intensity with heliocentric distance. As such, the formation distances of the parent asteroids of ancient meteorites can potentially be constrained by paleointensity measurements of these samples. Here, we find that the WIS 91600 ungrouped C2 chondrite experienced an ancient field intensity of 4.4 ± 2.8 µT. Combined with the thermal history of this meteorite, magnetohydrodynamical models suggest the disk field reached 4.4 µT at ∼9.8 AU, indicating that the WIS 91600 parent body formed in the distal solar system. Because WIS 91600 likely came to Earth from the asteroid belt, our recovered formation distance argues that this body previously travelled from ∼10 AU to 2-3 AU, supporting the migration of asteroid-sized bodies throughout the solar system. WIS 91600 also contains chondrules, calcium-aluminum-rich inclusions and amoeboid olivine aggregates, indicating that some primitive millimeter-sized solids that formed in the innermost solar system migrated outward to ∼10 AU within ∼3-4 Myr of solar system formation. Moreover, the oxygen isotopic compositions of proposed distal meteorites (WIS 91600, Experimental constraints on solid migration Tagish Lake and CI chondrites) argue that the CM, CO and CR chondrites contain micrometer-scale dust and ice that originated in the distal solar system.

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Section: Constraints On the Migration Of Micrometer-sized Materials Ansupporting

confidence: 85%

Constraints on the Distances and Timescales of Solid Migration in the Early Solar System from Meteorite Magnetism

Bryson

Weiss

Biersteker

et al. 2020

ApJ

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“…Changes in the sources of cosmic spherules with size complicate evaluating changes in isotopic composition owing to heating since both contribute to final distributions of isotopic composition. Apart from this, it should be noted that there are limitations with using the TFL above/below dichotomy to distinguish between ordinary and carbonaceous chondrite precursors as parent bodies of some hydrated carbonaceous chondrite groups plot on and above the TFL (e.g., the CI and CY chondrites, King et al, 2019).…”

Section: Discussionmentioning

confidence: 99%

The Oxygen Isotope Compositions of Large Numbers of Small Cosmic Spherules: Implications for Their Sources and the Isotopic Composition of the Upper Atmosphere

et al. 2020

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Cosmic spherules are micrometeorites that melt at high altitude as they enter Earth's atmosphere, and their oxygen isotope compositions are partially or completely inherited from the upper atmosphere, depending on the amount of heating experienced and the nature of their precursor materials. In this study, the three oxygen isotope compositions of 137 cosmic spherules are determined using 277 in situ analyses by ion probe. Our results indicate a possible correlation between increasing average δ 18 O compositions of silicate-dominated (S-type) spherules along the series scoriaceous < porphyritic < barred < cryptocrystalline < glass < CAT (calcium-aluminum-titanium) spherules (~12‰, 20‰, 22‰, 25‰, 26‰, and 50‰). This is consistent with the evolution of oxygen isotopes by mass fractionation owing to increased average entry heating and thus suggests mass fractionation dominates changes in isotopic composition, with atmospheric exchange being less significant. The Δ 17 O values of spherules, therefore, are mostly preserved and suggest that~80% of particles are samples of C-type asteroids. The genetic relationships between different S-types can also be determined with scoriaceous, barred, and cryptocrystalline spherules mostly having low Δ 17 O values (≤0‰) mainly derived from carbonaceous chondrite (CC)-like sources, while porphyritic spherules mostly have positive Δ 17 O (>0‰) and are largely derived from ordinary chondrite (OC)-like sources related to S (IV)-type asteroids. Glass and CAT spherules have variable Δ 17 O values indicating they formed by intense entry heating of both CC and OC-like materials. I-type cosmic spherules have a narrow range of δ 17 O (~20-25‰) and δ 18 O (~38-48‰) values, with Δ 17 O (~0‰) suggesting their oxygen is obtained entirely from the Earth's atmosphere, albeit with significant mass fractionation owing to evaporative heating. Finally, G-type cosmic spherules have unexpected isotopic compositions and demonstrate little mass fractionation from a CC-like source. The results of this study provide a vital assessment of the wider population of extraterrestrial dust arriving on Earth.

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“…First, the diversity among solar system materials is much larger than our contemporary (micro)meteorite inventory suggests (see also, e.g., Yada et al 2005;Gounelle et al 2009;Suavet et al 2010;Cordier and Folco 2014;Van Ginneken et al 2017;Goderis et al 2020;Suttle et al 2020). Second, the classical dichotomy (i.e., carbonaceous versus noncarbonaceous chondrites) observed in oxygen isotope space should be reconsidered as the oxygen isotope compositions of carbonaceous chondrites appear to be much more diverse (see also e.g., Goodrich et al 2019;Kebukawa et al 2019;King et al 2019;Kerraouch et al 2020;Suttle et al 2020). Micrometeorite WF1202A-001 may thus possibly serve as an example for the (hidden) diversity present among the carbonaceous chondrite class.…”

Section: Oxygen Isotopic Composition Of Micrometeorite Wf1202a-001: Amentioning

confidence: 98%

Evidence for the presence of chondrule‐ and CAI‐derived material in an isotopically anomalous Antarctic micrometeorite

Soens

Suttle

Maeda

et al. 2020

Meteorit & Planetary Scien

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We report the discovery of a unique, refractory phase‐bearing micrometeorite (WF1202A‐001) from the Sør Rondane Mountains, East Antarctica. A silicate‐rich cosmic spherule (~400 µm) displays a microporphyritic texture containing Ca‐Al‐rich inclusion (CAI)‐derived material (~5–10 area%), including high‐Mg forsterite (Fo98‐99) and enstatite (En98‐99, Wo0‐1). The micrometeorite also hosts a spherical inclusion (~209 µm), reminiscent of chondrules, displaying a barred olivine texture. Oxygen isotopic compositions of the micrometeorite groundmass (δ17O = –3.46‰, δ18O = 10.43‰, ∆17O = –1.96‰) are consistent with a carbonaceous chondrite precursor body. Yet, a relict forsterite grain is characterized by δ17O = –45.8‰, δ18O = –43.7‰, ∆17O = –23.1‰, compatible with CAIs. In contrast, a relict low‐Ca pyroxene grain (δ17O = –4.96‰, δ18O = –4.32‰, ∆17O = –2.71‰) presumably represents a first‐generation silicate grain that accreted 18O‐rich gas or dust in a transient melting scenario. The spherical inclusion displays anomalous oxygen isotope ratios (δ17O = –0.98‰, δ18O = –2.16‰, ∆17O = 0.15‰), comparable to anhydrous interplanetary dust particles (IDPs) and fragments from Comet 81P/Wild2. Based on its major element geochemistry, the chondrule size, and oxygen isotope systematics, micrometeorite WF1202A‐001 likely sampled a carbonaceous chondrite parent body similar to, but distinct from CM, CO, or CV chondrites. This observation may suggest that some carbonaceous chondrite bodies can be linked to comets. The reconstructed atmospheric entry parameters of micrometeorite WF1202A‐001 suggest that the precursor particle originated from a low‐inclination, low‐eccentricity source region, most likely either the main belt asteroids or Jupiter family comets (JFCs).

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The Yamato-type (CY) carbonaceous chondrite group: Analogues for the surface of asteroid Ryugu?

Cited by 93 publications

References 72 publications

Constraints on the Distances and Timescales of Solid Migration in the Early Solar System from Meteorite Magnetism

Constraints on the Distances and Timescales of Solid Migration in the Early Solar System from Meteorite Magnetism

The Oxygen Isotope Compositions of Large Numbers of Small Cosmic Spherules: Implications for Their Sources and the Isotopic Composition of the Upper Atmosphere

Evidence for the presence of chondrule‐ and CAI‐derived material in an isotopically anomalous Antarctic micrometeorite

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