Introduction: We recently reported the discovery of E-MNHN-002, a compound Ca-Al-rich Inclusion (CAI)-chondrule object from the reduced CV3 chondrite Efremovka, composed of an amoeboid olivine aggregate (AOA) core surrounded by a type I chondrule mantle [1]. Its petrographic study indicates that a Ca-Al-rich AOA accreted an olivine + metal mantle akin to the precursors of type I chondrules and ...

Elephant Moraine (EET) 96029 is a CM carbonaceous chondrite regolith breccia with evidence for unusually mild aqueous alteration, a later phase of heating and terrestrial weathering. The presence of phyllosilicates and carbonates within chondrules and the fine-grained matrix indicates that this meteorite was aqueously altered in its parent body. Features showing that water-mediated processing w...

[1] Textural and compositional analyses using Chemistry Camera (ChemCam) remote microimager and laser-induced breakdown spectroscopy (LIBS) have been performed on five float rocks and coarse gravels along the first 100 m of the Curiosity traverse at Bradbury Rise. ChemCam, the first LIBS instrument sent to another planet, offers the opportunity to assess mineralogic diversity at grain-size scal...

Many asteroids in the main belt have spectra like those of Mighei-type CM chondrites, but some Near Earth Objects (NEO) resemble less well known types C2 chondrite. Northwest Africa (NWA) 12563, a new find with affinities to could help us understand differences between observations CM2 chondrites and bodies that are currently being studied by Hayabusa2 OSIRIS-REx space missions. NWA 12563 conta...

Lunar meteorite EET 96008 is a fragmental breccia that predominantly consists of basaltic mineral clasts (0.5–2 mm), along with minor lithic fragments and breccia clasts. The matrix consists mainly of smaller mineral fragments ( 0.5 mm), bound by glassy cement, the majority of which are pyroxene and plagioclase. The pyroxene possesses extensive exsolution lamellae. These lamellae, up to 1 m in ...

Introduction: The A16 (Apollo16) site in the lunar nearside highlands is 220 km from the nearest mare. Thus it is no surprise that mare basalt samples are uncommon at the site. Here, we present the petrography and geochemistry of 5 new mare basalt samples found at the A16 site. We also discuss possible provenances of all A16 mare basalt samples using high-resolution global data for the distribu...

Introduction: It has been proposed that chondrules behaved as chemically closed system with respect to Na [1-5]. This implies that Na did not evaporate from the chondrule melt after onset of olivine crystallization. High temperatures, low pressure and low fO 2 during chondrule formation, however, should lead to rapid loss (minutes) of Na [e.g., 6]. This is not observed. Understanding the relati...

Introduction: MIL 03346 is a newly discovered clinopyroxenite belonging to the nakhlite class of SNC (martian) meteorites [1]. Although the petrographic and geochemical characteristics of MIL 03346 are broadly similar to those of previously known nakhlites, there are also some differences. In particular, it has the highest abundance of glassy mesostasis among the nakhlites, possibly indicative ...

Introduction: Previous trace element and isotopic analyses of the Apollo 14 high-Al basalts, suggest that these samples represent the earliest stages of basaltic volcanism on the Moon and that they are not random samples from the lunar regolith [1,2,3,4,5,6,7]. One of the primary goals of this work is to determine if these small, fragmented samples are the result of igneous or impact processes....