10:15 AM - 10:30 AM
[PPS08-06] Anhydrous primary minerals in Ryugu, Ivuna, and Bennu
Keywords:Bennu, Ryugu, CI chondrite, SIMS
Samples returned from asteroid Ryugu are chemically and mineralogically similar to CI chondrites [e.g., 1–3]. Both are predominantly composed of low-temperature aqueously formed secondary minerals, whereas high-temperature anhydrous primary minerals, such as olivine, low-Ca pyroxene, spinel, and hibonite, are rarely present. Using secondary ion mass spectrometry (SIMS; Cameca ims-1280HR at Hokkaido University), we performed O [4] and Al–Mg [5] isotope measurements of anhydrous primary minerals in samples of Ryugu and the Ivuna CI chondrite to constrain their origin.
Anhydrous primary minerals in our samples of Ryugu (C0002-C1001) and Ivuna occur mostly as monomineralic isolated grains embedded in hydrated matrix, consistent with other Ryugu samples [2]. Their O-isotope compositions are distributed along the slope-1 line on the O three-isotope diagram and range from Δ17O ~ –23 to 0‰. Mg-Al spinel grains are 16O-rich (Δ17O ~ –23‰). Low-Ca pyroxene grains are 16O-poor (Δ17O ~ –5‰). Olivine grains show a bimodal distribution of O-isotope composition: 10 of 34 grains measured are 16O-rich (Δ17O ~ –23‰) and 24 grains are 16O-poor (Δ17O ~ –7 to 0‰).
We found refractory inclusions composed of Mg-Al spinel and hibonite, one from Ryugu and one from Ivuna. Also, in Ivuna, we found an amoeboid olivine aggregate (AOA) composed of olivine, diopside, anorthite, and Mg-Al spinel and an inclusion composed of olivine and Mg-Al spinel. The minerals in all of these inclusions are 16O-rich (Δ17O ~ –24‰).
The 16O-rich grains and inclusions are mineralogically and O-isotopically similar to calcium-aluminum–rich inclusions (CAIs) and AOAs reported in other carbonaceous chondrites [6, 7]. In addition, the initial 26Al/27Al ratios of the two spinel-hibonite inclusions are inferred as ~4.4 × 10–5, also similar to most CAIs in carbonaceous chondrites [6, 8]. The range of Δ17O values for the 16O-poor olivine and low-Ca pyroxene grains is consistent with that of these minerals in chondrules in most carbonaceous chondrites [9]. Moreover, the most frequent Δ17O value (–6‰) for Mg-rich (Mg# > 97) olivine grains is identical to those for chondrules. Although CI chondrites and Ryugu samples are devoid of chondrules, the 16O-poor grains most likely represent fragments of chondrule-like objects. The presence of both 16O-poor chondrule–like and 16O-rich refractory inclusion–like minerals in Ryugu and Ivuna suggests that some of their building blocks are similar to those of other carbonaceous chondrite groups. They both probably formed in the inner solar protoplanetary disk and were subsequently transported outward.
Preliminary data for petrography of asteroid Bennu samples and chemical and isotopic compositions of their anhydrous primary minerals will also be presented in the meeting.
References: [1] Yokoyama et al. (2023) Science 379, eabn7850. [2] Nakamura et al. (2023) Science 379, eabn8671. [3] Noguchi et al. (2023) Nat. Astron. 7, 170–181. [4] Kawasaki et al. (2022) Sci. Adv. 8 (50), eade2067. [5] Miyamoto et al. (2024) this meeting. [6] Ushikubo et al. (2017) GCA 201, 103–122. [7] Fukuda et al. (2021) GCA 293, 544–574. [8] Kawasaki et al. (2020) GCA 279, 1–15. [9] Tenner et al. (2018) In Chondrules, 196–246.
Anhydrous primary minerals in our samples of Ryugu (C0002-C1001) and Ivuna occur mostly as monomineralic isolated grains embedded in hydrated matrix, consistent with other Ryugu samples [2]. Their O-isotope compositions are distributed along the slope-1 line on the O three-isotope diagram and range from Δ17O ~ –23 to 0‰. Mg-Al spinel grains are 16O-rich (Δ17O ~ –23‰). Low-Ca pyroxene grains are 16O-poor (Δ17O ~ –5‰). Olivine grains show a bimodal distribution of O-isotope composition: 10 of 34 grains measured are 16O-rich (Δ17O ~ –23‰) and 24 grains are 16O-poor (Δ17O ~ –7 to 0‰).
We found refractory inclusions composed of Mg-Al spinel and hibonite, one from Ryugu and one from Ivuna. Also, in Ivuna, we found an amoeboid olivine aggregate (AOA) composed of olivine, diopside, anorthite, and Mg-Al spinel and an inclusion composed of olivine and Mg-Al spinel. The minerals in all of these inclusions are 16O-rich (Δ17O ~ –24‰).
The 16O-rich grains and inclusions are mineralogically and O-isotopically similar to calcium-aluminum–rich inclusions (CAIs) and AOAs reported in other carbonaceous chondrites [6, 7]. In addition, the initial 26Al/27Al ratios of the two spinel-hibonite inclusions are inferred as ~4.4 × 10–5, also similar to most CAIs in carbonaceous chondrites [6, 8]. The range of Δ17O values for the 16O-poor olivine and low-Ca pyroxene grains is consistent with that of these minerals in chondrules in most carbonaceous chondrites [9]. Moreover, the most frequent Δ17O value (–6‰) for Mg-rich (Mg# > 97) olivine grains is identical to those for chondrules. Although CI chondrites and Ryugu samples are devoid of chondrules, the 16O-poor grains most likely represent fragments of chondrule-like objects. The presence of both 16O-poor chondrule–like and 16O-rich refractory inclusion–like minerals in Ryugu and Ivuna suggests that some of their building blocks are similar to those of other carbonaceous chondrite groups. They both probably formed in the inner solar protoplanetary disk and were subsequently transported outward.
Preliminary data for petrography of asteroid Bennu samples and chemical and isotopic compositions of their anhydrous primary minerals will also be presented in the meeting.
References: [1] Yokoyama et al. (2023) Science 379, eabn7850. [2] Nakamura et al. (2023) Science 379, eabn8671. [3] Noguchi et al. (2023) Nat. Astron. 7, 170–181. [4] Kawasaki et al. (2022) Sci. Adv. 8 (50), eade2067. [5] Miyamoto et al. (2024) this meeting. [6] Ushikubo et al. (2017) GCA 201, 103–122. [7] Fukuda et al. (2021) GCA 293, 544–574. [8] Kawasaki et al. (2020) GCA 279, 1–15. [9] Tenner et al. (2018) In Chondrules, 196–246.