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Introduction: Two groups of carbonaceous chondrites, the CV and CK chondrites, have similar compositions and textures. The CV chondrites are characterized by a fine-grained matrix, abundant chondrules (≈45 vol%), and Fe-rich olivine [1-3]. However, the CK chondrites contain Ni-rich olivine and Cr-rich magnetite [4]. Both groups also experience different degrees of metamorphism; while CV chondrites are metamorphosed to types 3.0 - 3.6, CK chondrites are metamorphosed to types 3.7 - 6.0 [5-7]. [8-10] suggest that CV and CK chondrites originate from the same parent body, whereas [11] argue for separate parent bodies due to the two groups' distinct magnetite compositions. The single-parent-body model could be strengthened with evidence of transitional CV-CK material. In its original classification, Northwest Africa (NWA) 10588 (CK3) was described as potentially intermediate between CV and CK chondrites [12]. We investigated the mineralogy and texture of this sample to revisit the classification and determine if it is transitional. Methodology: Elemental mapping, Energy Dispersive Spectroscopy (EDS), and backscattered electron (BSE) imaging was completed at Bowdoin College using a Tescan Vega3 Scanning Electron Microscope (SEM). Mineral chemistry analyses were obtained using a JEOL JXA 8200 electron microprobe at Washington University in St. Louis, where we analyzed olivine, pyroxene, sulfides, and oxides present within chondrules, chondrule rims, veins, and matrix. We obtained 90 olivine analyses in 13 chondrules, as well as 35 pyroxene analyses in 10 chondrules. Microprobe operating conditions included a 15kV potential, 25.0nA beam current, and 2μm beam size. Results: The average fayalite (Fa) content of chondrules ranges between Fa11-Fa33; the average is Fa22 (n = 90). Olivine consistently contains NiO abundances <0.04 wt%, and average Cr2O3 is <0.10wt%. The average ferrosilite (Fs) value for pyroxene is Fs11.83 (n = 35). BSE images show that the matrix is fine-grained and not recrystallized. Shock veins and metal grains are present throughout the sample; multiple oxide veins show evidence of replacement by terrestrial limonite (FeO™nH2O). Minimally-altered magnetite grains in the matrix and chondrule rims contain average TiO2, Cr2O3, and NiO abundances of 0.0wt%, 0.02wt%, and 0.13wt%, respectively. Additionally, 2 troilite grains and one chromite grain were identified. Comparison with CV and CK Chondrites: Characteristics consistent with the CV chondrites include the primitive matrix, NiO content of chondrule olivine, chondrule abundance (65-70 vol%), and abundances of TiO2 and NiO in magnetite. However, the equilibrated nature of chondrule olivine suggests that the sample has experienced metamorphism consistent with Type 3.7 CK chondrites [13]. An anomalous characteristic that is not consistent with CV nor CK chondrites is the low (<0.1wt%) Cr in magnetite. Based on these results, we suggest that NWA 10588 is an anomalous CV chondrite. However, the equilibrated chondrule olivine indicates that it experienced a higher degree of metamorphism than recorded in other CV chondrites. In order to better understand the thermal history of the CV parent body, future work will focus on the search for similarly-equilibrated CV chondrites. [ABSTRACT FROM AUTHOR]

Five hundred and eighteen cosmic spherules were identified among the 672 spherules handpicked from deep sea sediments by using Scanning Electron Microscope-Energy Dispersive Spectrometry (SEM-EDS). One of the spherules is found to enclose a spherical chondrule-like object that can be distinguished from the rest of the spherule by its shape, texture and composition and whose petrographic features, size and chemical composition are similar to chondrules from a chondritic meteorite, probably of carbonaceous chondritic nature. The present finding suggests that a small fraction of the particulate extraterrestrial matter enters the earth as fragments of larger meteorites. [ABSTRACT FROM AUTHOR]

- We optically classified 5682 micrometeorites (MMs) from the 2000 South Pole collection into textural classes, imaged 2458 of these MMs with a scanning electron microscope, and made 200 elemental and eight isotopic measurements on those with unusual textures or relict phases. As textures provide information on both degree of heating and composition of MMs, we developed textural sequences that illustrate how fine-grained, coarse-grained, and single mineral MMs change with increased heating. We used this information to determine the percentage of matrix dominated to mineral dominated precursor materials (precursors) that produced the MMs. We find that at least 75% of the MMs in the collection derived from fine-grained precursors with compositions similar to CI and CM meteorites and consistent with dynamical models that indicate 85% of the mass influx of small particles to Earth comes from Jupiter family comets. A lower limit for ordinary chondrites is estimated at 2-8% based on MMs that contain Na-bearing plagioclase relicts. Less than 1% of the MMs have achondritic compositions, CAI components, or recognizable chondrules. Single mineral MMs often have magnetite zones around their peripheries. We measured their isotopic compositions to determine if the magnetite zones demarcate the volume affected by atmospheric exchange during entry heating. Because we see little gradient in isotopic composition in the olivines, we conclude that the magnetites are a visual marker that allows us to select and analyze areas not affected by atmospheric exchange. Similar magnetite zones are seen in some olivine and pyroxene relict grains contained within MMs. [ABSTRACT FROM AUTHOR]