Mineralogical Criteria for the Parent Asteroid of the “Carbonaceous” Achondrite NWA 6704

McGraw, A. M.; Reddy, V.; Izawa, M. R. M.; Sanchez, Juan A.; Corre, Lucille Le; Cloutis, E. A.; Applin, D. M.; Pearson, N.

doi:10.3847/1538-3881/ab5fe7

Cited by 4 publications

(3 citation statements)

References 74 publications

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“…Given overall burial depths of 2.55 − 3.25 km derived, both grouplets would be intrusive rocks and, in fact, NWA 011 has a cumulate-eucrite-like REE pattern, 51 while NWA 6704 spectrum showed a close similarity to the basaltic and cumulate eucrites. 54 The asteroid (34698) 2001 OD22 suggested as parent body of NWA 6704 55 does not fulfill the size requirements we derived and, if related, should be a piece of a fractured parent asteroid. A partially differentiated parent body with a radius of ≈ 200 km has been proposed previously as parent body of CR1-3 and NWA 011 6,7,8 .…”

Section: Meteoritementioning

confidence: 91%

Temporally distributed parent body accretion in the C reservoir of the solar system

Neumann¹,

Ma²,

Bouvier³

et al. 2023

Preprint

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Accretion processes in protoplanetary disks produce a diversity of small bodies that played a crucial role in potentially multiple reshuffling events throughout the solar system and in both early and late accretion of planets. Application of thermo-chronometers to meteorites provides precise dating of the formation age of various mineralogical components. Nucleosynthetic isotopic anomalies that indicate a dichotomy between noncarbonaceous (NC) and carbonaceous (C) meteorites and precise parent body chronology can be combined with planetesimal thermal evolution models to constrain the timescale of accretion and dynamical processes in the early solar system. Achondrite parent bodies are considered to have accreted early and mostly in the NC region. By contrast, late accretion in the C region produced mostly undifferentiated parent bodies, such as the parent body of CR chondrites that formed as late as 4 Ma after solar system formation 25 . However, presence of more evolved CR-related meteorites suggests also an earlier accretion timing. We present modeling evidence for a temporally distributed accretion of parent bodies of CR-related meteorite groups that originate from a C reservoir and range from aqueously altered chondrites to highly equilibrated chondrites and partially differentiated primitive achondrites. The parent body formation times derived range from < 1 Ma to ≈ 4 Ma after solar system formation,

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Section: Meteoritementioning

confidence: 91%

Temporally distributed parent body accretion in the C reservoir of the solar system

Neumann¹,

Ma²,

Bouvier³

et al. 2023

Preprint

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show abstract

“…An integration time of 0.136 s was used with 7000 total scans for the samples and white reference (952 s total integration time), while 100 scans were used for darks (1.36 s total integration time). The near-infrared to mid-infrared range (1.5-14.2 μm) was measured using a Thermofisher Nicolet FTIR spectrometer at a spectral resolution of 4 cm −1 (wavenumber) with a mercury cadmium telluride detector, potassium bromide beam splitter, and a silicon nitride globar light source (McGraw et al 2020). Light was directed onto and collected from the sample using a SpecAc diffuse reflectance goniometer with an incidence at 0°and emission at 30°.…”

Section: Methodsmentioning

confidence: 99%

Laboratory Spectral Characterization of Ribbeck Aubrite: Meteorite Sample of Earth-impacting Near-Earth Asteroid 2024 BX1

Cantillo,

Ridenhour,

Battle

et al. 2024

Planet. Sci. J.

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Characterization of near-Earth objects (NEOs) is critical for Earth-impact hazard assessment. Particularly crucial to our physical understanding of NEOs are laboratory spectral measurements of meteorites as they are the best and most widely available analog materials, barring sample return missions. However, most meteorites do not have direct orbital links to specific asteroids, making it challenging to identify their source body in the NEO or main-belt asteroid populations. Near-Earth asteroid (NEA) 2024 BX1 was discovered on 2024 January 20 at 21:48 UTC from MPC code K88, impacting the Earth (west of Berlin, Germany) 165 minutes later. The incoming bolide was observed by multiple meteor cameras, which enabled successful reconstruction of its exo-atmospheric orbit and quick recovery. We present results from laboratory spectral characterization of the Ribbeck meteorite in the UV–mid-infrared wavelengths (0.2–14.2 μm) over seven grain size bins (<45 μm–slab). Our results suggest that Ribbeck has spectral properties consistent with enstatite achondrite (aubrite) meteorites. Our grain-size spectral analysis shows that albedo and spectral slope decrease as grain size increases. In addition, increasing grain size also shifts the taxonomic type in the Bus–DeMeo system from Xn to B types, suggesting the limitations of taxonomy in classifying small, regolith-free NEAs. We also present results of our comparison between Ribbeck data and spectra of E types in the main-belt and NEA populations. Principal component analysis of our Ribbeck samples shows variations parallel to the α line, which can be confused with space weathering in PC space.

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“…These meteorites include NWA 6693 (Warren et al, 2013), NWA 6704 (Hibiya et al, 2019), NWA 6926 (Ruzicka et al, 2014), and NWA 10132 (Sanborn et al, 2018). NWA 6704 was found by McGraw et al (2020) to have a visible and near-infrared reflectance spectrum that would classify it as a V-type. However, NWA 6693 (Warren et al, 2013) and NWA 6704 (Hibiya et al, 2019) have siderophile (iron-loving) element abundances that are nearly chondritic, which implies that their parent bodies did not undergo differentiation.…”

Section: Isotopic Chemical and Petrologic Evidencementioning

confidence: 99%

How many Vesta‐like bodies existed in the asteroid belt?

Burbine,

Greenwood,

Zhang

et al. 2024

Meteorit & Planetary Scien

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Asteroid 4 Vesta is typically thought to be the parent body of the HED (howardite, eucrite, and diogenite) meteorites due to spectral similarities. The discovery of asteroids far from Vesta with HED‐like spectra like (1459) Magnya and HED‐like meteorites (e.g., NWA 011) with anomalous oxygen isotopic values compared to typical HEDs is evidence that other Vesta‐like bodies formed. We broadly define a Vesta‐like body as a differentiated object with a crust composed primarily of low‐Ca pyroxene and plagioclase feldspar. We estimate the number of Vesta‐like bodies that did form by looking at the astronomical evidence; the oxygen isotopic, chemical, and petrologic evidence; and the iron meteorite evidence. Assuming that fragments of Vesta were scattered from Vesta by giant planet migration, we conservatively estimate that at least two Vesta‐like bodies (Vesta and the Magnya parent bodies) existed. From the oxygen isotopic, chemical, and petrologic evidence, we also conservatively estimate that seven Vesta‐like bodies formed. Analyses of iron meteorites indicate that there may be as many as 23 Vesta‐like bodies (Vesta, 10 magmatic iron groups, South Byron trio, Emsland/Mbosi duo, 10 ungrouped irons). This estimate from iron meteorites is most certainly an overestimation due to the existence of a number of non‐HED crustal/mantle fragments that potentially originated from bodies with magmatic iron cores. Using our three estimates as a guide, we predict that there were ~10 Vesta‐like bodies (including Vesta) that formed in the early solar system. Only Vesta remains intact with the others being disrupted early in solar system history.

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Mineralogical Criteria for the Parent Asteroid of the “Carbonaceous” Achondrite NWA 6704

Cited by 4 publications

References 74 publications

Temporally distributed parent body accretion in the C reservoir of the solar system

Temporally distributed parent body accretion in the C reservoir of the solar system

Laboratory Spectral Characterization of Ribbeck Aubrite: Meteorite Sample of Earth-impacting Near-Earth Asteroid 2024 BX1

How many Vesta‐like bodies existed in the asteroid belt?

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