Evidence for a multilayered internal structure of the chondritic acapulcoite-lodranite parent asteroid

Li, Shijie; Yin, Q. Z.; Bao, Huiming; Sanborn, M. E.; Irving, A. J.; Ziegler, K.; Agee, C. B.; Marti, K.; Miao, Bingkui; Li, Xiongyao; Li, Yang; Wang, Shijie

doi:10.1016/j.gca.2018.09.004

Cited by 33 publications

(24 citation statements)

References 84 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…By analogy with other meteorite groups such as the acapulcoites-lodranites and H-chondrites, which also exhibit diverse lithologies and were suggested to have a multilayered parent body (e.g., McCoy et al 1996;Benedix et al 2000;Trieloff et al 2003;Eugster and Lorenzetti 2005;Li et al 2018), our study and previous investigations (e.g., Benedix et al 2000) suggest that a four-layered structure is most likely to be formed through incomplete differentiation on winonaite-IAB parent asteroid (Fig. 7).…”

Section: The Layered Structure Model For Winonaite-iab Parent Asteroidsupporting

confidence: 79%

“…In addition, some silicate inclusions in IAB iron meteorites (e.g., Udei Station) contain the lithologies that formed as the residue of partial melting (Benedix et al 2000;Takeda et al 2000;Ruzicka and Hutson 2010). By analogy with the observations for acapulcoite-lodranite meteorites, the SAH 02029 and other partial melt residues are more similar to the lodranite meteorites that are thought to represent the partial melting residue from the deep region of acapulcoite-lodranite parent body (McCoy et al 1997a;Eugster and Lorenzetti 2005;Li et al 2018). These residues of silicate melting (e.g., SAH 02029 and Tierra Blanca) most likely represent the deep lithologies on winonaite-IAB parent asteroid.…”

Section: Deep Residue Of Partial Meltingmentioning

confidence: 84%

“…Most winonaites (e.g., NWA 6448, GRV 022890, GRV 021663, Pontlyfni, and Winona; Benedix et al 1998;Floss et al 2008; this study) have a mixture of fine-, medium-, and coarse-grained equigranular texture. These samples reached a peak temperature of < 1200 °C and experienced limited metamorphism, resulting in limited partial melting (Benedix et al 1998(Benedix et al , 2005Floss et al 2007Floss et al , 2008Hunt et al 2017;Li et al 2018). By comparing to the primitive achondrite group of acapulcoite-lodranite clans, these diverse winonaite lithologies share similar petrology and mineralogy (e.g., recrystallization texture, FeNi-FeS partial melting, and approximately chondritic mineralogy) with the acapulcoite meteorites which were thought to represent the outer layer of their parent body (Eugster and Lorenzetti 2005).…”

Section: Subsurface Layer Composed Of Diverse Lithologies That Experimentioning

confidence: 99%

See 2 more Smart Citations

The layered structure model for winonaite parent asteroid implicated by textural and mineralogical diversity

Zeng

Shang

et al. 2019

Earth Planets Space

Self Cite

View full text Add to dashboard Cite

The winonaites are primitive achondrites that are associated with IAB iron meteorites. They provide valuable insights into differentiation processes on asteroids in the early Solar System. However, there is still little understanding of the lithological diversity as well as the structure of the winonaite parent asteroid. In this work, we report the petrologic texture and mineralogy of a suite of winonaites (i.e., Northwest Africa (NWA) 725, NWA 6448, NWA 4024, Grove Mountains (GRV) 022890, GRV 021663, and Sahara (SAH) 02029) that exhibit a wide diversity of petrographic textures from primitive chondritic texture to coarse-grained equigranular texture. In particular, we recognized an unusual winonaite (SAH 02029) with a distinctive mineralogy and mineral chemistry (e.g., depleted in troilite, plagioclase contains melt inclusions, high plagioclase An values, and LREE-depleted clinopyroxene). The petrological and mineralogical features of SAH 02029 indicate that this meteorite has undergone silicate partial melting and may represent the residue of ~ 5-10 vol% partial melting. The textural and mineralogical diversity among winonaites suggests that the winonaite-IAB parent asteroid would have formed a four-layered structure during its evolution history: (1) surface layer consisting of precursor chondritic materials; (2) subsurface layer composed of diverse lithologies that experienced limited metamorphism and FeNi-FeS partial melting; (3) deep residues of silicate partial melting; and (4) interior layer consisting of incomplete differentiation metal pools. This conclusion enables us to establish constraints on the evolution history of winonaite-IAB parent body.

show abstract

Section: The Layered Structure Model For Winonaite-iab Parent Asteroidsupporting

confidence: 79%

Section: Deep Residue Of Partial Meltingmentioning

confidence: 84%

Section: Subsurface Layer Composed Of Diverse Lithologies That Experimentioning

confidence: 99%

See 1 more Smart Citation

The layered structure model for winonaite parent asteroid implicated by textural and mineralogical diversity

Zeng

Shang

et al. 2019

Earth Planets Space

Self Cite

View full text Add to dashboard Cite

show abstract

“…Literature data for ε 50 Ti and ε 54 Cr are from refs. 19 – 25 . ( C , D ) Literature Δ 17 Ο data are from refs.…”

Section: Resultsmentioning

confidence: 99%

Chondrules reveal large-scale outward transport of inner Solar System materials in the protoplanetary disk

Williams

Sanborn

Defouilloy

et al. 2020

Proc. Natl. Acad. Sci. U.S.A.

Self Cite

View full text Add to dashboard Cite

Dynamic models of the protoplanetary disk indicate there should be large-scale material transport in and out of the inner Solar System, but direct evidence for such transport is scarce. Here we show that the ε50Ti-ε54Cr-Δ17O systematics of large individual chondrules, which typically formed 2 to 3 My after the formation of the first solids in the Solar System, indicate certain meteorites (CV and CK chondrites) that formed in the outer Solar System accreted an assortment of both inner and outer Solar System materials, as well as material previously unidentified through the analysis of bulk meteorites. Mixing with primordial refractory components reveals a “missing reservoir” that bridges the gap between inner and outer Solar System materials. We also observe chondrules with positive ε50Ti and ε54Cr plot with a constant offset below the primitive chondrule mineral line (PCM), indicating that they are on the slope ∼1.0 in the oxygen three-isotope diagram. In contrast, chondrules with negative ε50Ti and ε54Cr increasingly deviate above from PCM line with increasing δ18O, suggesting that they are on a mixing trend with an ordinary chondrite-like isotope reservoir. Furthermore, the Δ17O-Mg# systematics of these chondrules indicate they formed in environments characterized by distinct abundances of dust and H2O ice. We posit that large-scale outward transport of nominally inner Solar System materials most likely occurred along the midplane associated with a viscously evolving disk and that CV and CK chondrules formed in local regions of enhanced gas pressure and dust density created by the formation of Jupiter.

show abstract

“…The ε 54 Cr value, which is the mass fractionation corrected deviation of the 54 Cr/ 52 Cr ratio from the terrestrial value in parts per 10,000, varies between bulk meteorite groups and reflects heterogeneous distribution of 54 Cr-rich supernova grains in the proto-solar molecular cloud material (Dauphas et al 2010;Qin et al 2011;Nittler et al 2018). This is expressed by higher ε 54 Cr values of carbonaceous chondrites (CC;Trinquier et al 2007;Qin et al 2010a;Yamashita et al 2010;Petitat et al 2011;Yamakawa & Yin 2014;Göpel et al 2015), compared to ordinary chondrites (OC) and some differentiated meteorites (e.g., Martian meteorites, angrites, howardite-eucrite-diogenite clan, mesosiderites, acapulcoitelodranite clan, winonaites, pallasites, and iron meteorites; Trinquier et al 2007;Qin et al 2010a;Li et al 2018;Pedersen et al 2019;Zhu et al 2019b), whereas the enstatite chondrites (EC), the Earth, the Moon, and the aubrites have intermediate values (Trinquier et al 2007;Qin et al 2010a;Mougel et al 2018).…”

Section: Introductionmentioning

confidence: 99%

Chromium Isotopic Constraints on the Origin of the Ureilite Parent Body

Zhu

Moynier

Schiller

et al. 2020

ApJ

View full text Add to dashboard Cite

We report on the mass-independent Cr isotope compositions of 11 main group ureilites and an ureilitic trachyandesite (ALM-A). The 54 Cr/ 52 Cr ratios for main group ureilites vary from −1.06±0.04 to −0.78±0.05 and averaged at −0.91±0.15 (2SD, N=18) including the data from literature. We argue that this variation reflects primitive mantle heterogeneities within the ureilite parent body (UPB). As such, this body did not experience a global-scale magma ocean, which is consistent with heterogeneous O isotope in ureilites. Furthermore, the ε 54 Cr values, Mn/Cr ratios, C isotope ratios, Mg#values, and Fe/Mn ratios in the olivine cores of ureilites are correlated with each other, which suggests the mixing of ureilite precursors from at least two reservoirs, rather than a smelting process or the oxidation from ice melting. All the ureilite samples (including the ALM-A) fall on a well-defined 53 Mn-53 Cr isochron corresponding to a 53 Mn/ 55 Mn ratio of (6.02 ± 1.59)×10 −6 , which translates to an age of 4566.7±1.5 Ma (within 2 Ma after calcium-aluminum-rich inclusions; CAIs) when anchored to the U-corrected Pb-Pb age for the D'Orbigny angrite. This old age indicates early partial melting on the UPB, consistent with the early accretion of the UPB (within 1 Ma after CAIs) predicted by thermal modeling. Furthermore, there is a 4∼5 Ma age difference between the external isochron in this study and internal isochron ages for the feldspathic clasts in polymict ureilites, which likely reflects an impact history during the early evolution of the UPB.

show abstract

Evidence for a multilayered internal structure of the chondritic acapulcoite-lodranite parent asteroid

Cited by 33 publications

References 84 publications

The layered structure model for winonaite parent asteroid implicated by textural and mineralogical diversity

The layered structure model for winonaite parent asteroid implicated by textural and mineralogical diversity

Chondrules reveal large-scale outward transport of inner Solar System materials in the protoplanetary disk

Chromium Isotopic Constraints on the Origin of the Ureilite Parent Body

Contact Info

Product

Resources

About