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Instruments / Technical Area	Publication Details	Published
E01-JEM ARM 200CF E02-JEM ARM 300CF I14-Hard X-ray Nanoprobe I18-Microfocus Spectroscopy	Fe‐redox changes in Itokawa space‐weathered rims L. J. Hicks , J. C. Bridges , T. Noguchi , A. Miyake , J. D. Piercy , S. H. Baker Meteoritics & Planetary Science 312 DOI: 10.1111/maps.13611 Diamond Proposal Number(s): [19641, 23232, 26303] Open Access Show Abstract ▼ Abstract: Synchrotron Fe‐K X‐ray absorption spectroscopy and transmission electron microscopy have been used to investigate the mineralogy and Fe‐redox variations in the space‐weathered (SW) rims of asteroidal samples. This study focuses on the FIB lift‐out sections from five Itokawa grains, returned by the Hayabusa spacecraft, including samples RB‐QD04‐0063, RB‐QD04‐0080, RB‐CV‐0011, RB‐CV‐0089, and RB‐CV‐0148. Each of the samples featured partially amorphized SW rims, caused by irradiation damage from implanted low mass solar wind ions, and the impacting of micrometeorites. Using bright‐field and HAADF‐STEM imaging, vesicular blistering and nanophase Fe metal (npFe0) particles were observed within grain rims, and solar flare tracks were observed in the substrate host grain, confirming the presence of SW zones. We use Fe‐K XANES mapping to investigate Fe‐redox changes between the host mineral and the SW zones. All SW zones measured show some increases in the ferric‐ferrous ratio (Fe3+/ΣFe) relative to their respective host grains, likely the result of the implanted solar wind H+ ions reacting with the segregated ferrous Fe in the surface material.	Jan 2021
B22-Multimode InfraRed imaging And Microspectroscopy	The alteration history of the Jbilet Winselwan CM carbonaceous chondrite: An analog for C‐type asteroid sample return A. J. King , S. S. Russell , P. F. Schofield , E. R. Humphreys‐williams , S. Strekopytov , F. A. J. Abernethy , A. B. Verchovsky , M. M. Grady Meteoritics & Planetary Science 49 DOI: 10.1111/maps.13224 Diamond Proposal Number(s): [9614] Open Access Show Abstract ▼ Abstract: Jbilet Winselwan is one of the largest CM carbonaceous chondrites available for study. Its light, major, and trace elemental compositions are within the range of other CM chondrites. Chondrules are surrounded by dusty rims and set within a matrix of phyllosilicates, oxides, and sulfides. Calcium‐ and aluminum‐rich inclusions (CAIs) are present at ≤1 vol% and at least one contains melilite. Jbilet Winselwan is a breccia containing diverse lithologies that experienced varying degrees of aqueous alteration. In most lithologies, the chondrules and CAIs are partially altered and the metal abundance is low (<1 vol%), consistent with petrologic subtypes 2.7–2.4 on the Rubin et al. (2007) scale. However, chondrules and CAIs in some lithologies are completely altered suggesting more extensive hydration to petrologic subtypes ≤2.3. Following hydration, some lithologies suffered thermal metamorphism at 400–500 °C. Bulk X‐ray diffraction shows that Jbilet Winselwan consists of a highly disordered and/or very fine‐grained phase (73 vol%), which we infer was originally phyllosilicates prior to dehydration during a thermal metamorphic event(s). Some aliquots of Jbilet Winselwan also show significant depletions in volatile elements such as He and Cd. The heating was probably short‐lived and caused by impacts. Jbilet Winselwan samples a mixture of hydrated and dehydrated materials from a primitive water‐rich asteroid. It may therefore be a good analog for the types of materials that will be encountered by the Hayabusa‐2 and OSIRIS‐REx asteroid sample‐return missions.	Dec 2018
I18-Microfocus Spectroscopy	Magnetite in comet Wild 2: evidence for parent body aqueous alteration Leon Hicks , J. L. Macarthur , J. C. Bridges , M. C. Price , J. E. Wickham-Eade , M. J. Burchell , G. M. Hansford , A. L. Butterworth , S. J. Gurman , S. H. Baker Meteoritics & Planetary Science 53 DOI: 10.1111/maps.12909 Diamond Proposal Number(s): [1833, 7487, 9418, 10328, 13690] Open Access Show Abstract ▼ Abstract: The mineralogy of comet 81P/Wild 2 particles, collected in aerogel by the Stardust mission, has been determined using synchrotron Fe-K X-ray absorption spectroscopy with in situ transmission XRD and X-ray fluorescence, plus complementary microRaman analyses. Our investigation focuses on the terminal grains of eight Stardust tracks: C2112,4,170,0,0; C2045,2,176,0,0; C2045,3,177,0,0; C2045,4,178,0,0; C2065,4,187,0,0; C2098,4,188,0,0; C2119,4,189,0,0; and C2119,5,190,0,0. Three terminal grains have been identified as near pure magnetite Fe3O4. The presence of magnetite shows affinities between the Wild 2 mineral assemblage and carbonaceous chondrites, and probably resulted from hydrothermal alteration of the coexisting FeNi and ferromagnesian silicates in the cometary parent body. In order to further explore this hypothesis, powdered material from a CR2 meteorite (NWA 10256) was shot into the aerogel at 6.1 km s−1, using a light-gas gun, and keystones were then prepared in the same way as the Stardust keystones. Using similar analysis techniques to the eight Stardust tracks, a CR2 magnetite terminal grain establishes the likelihood of preserving magnetite during capture in silica aerogel.	Jul 2017
I11-High Resolution Powder Diffraction I12-JEEP: Joint Engineering, Environmental and Processing	Thermal processing and crystallization of amorphous Mg-Ca silicates Sarah J. Day , Stephen P. Thompson , Aneurin Evans , Julia Parker , Leigh Connor , Chiu Tang Meteoritics & Planetary Science 48 (8), 1459-–1471 DOI: 10.1111/maps.12162 Diamond Proposal Number(s): [6515, 7124] Show Abstract ▼ Abstract: The structural evolution of sol–gel-produced amorphous Mg(x)Ca(1–x)SiO3 silicates is investigated. Mid-IR Fourier transform infrared spectroscopy and synchrotron X-ray diffraction are used to confirm the amorphous nature of the as-prepared silicates, while subsequent in situ synchrotron X-ray powder diffraction measurements are used to study the evolution of crystalline mineral phases as a function of annealing temperature. Multiple silicate phases, including diopside, enstatite, forsterite, and SiO2, are identified, while Rietveld (i.e., structure) refinement of the diffraction data is used to quantify phase change relationships. Investigated as possible analogs for the refractory dust grain materials likely to have been present in the early solar nebula, the likely relevance of these investigations to the observed silicate compositions of chondritic meteorites and cometary bodies and the processing of their precursor materials is discussed.	Jul 2013
I18-Microfocus Spectroscopy	Iron oxides in comet 81P/Wild 2 John C. Bridges , Mark J. Burchell , Hitesh C. Changela , Nick J. Foster , J. Alan Creighton , James D. Carpenter , Steve J. Gurman , Ian A. Franchi , Henner Busemann Meteoritics & Planetary Science 45 (1), 55 - 72 DOI: 10.1111/j.1945-5100.2009.01005.x Show Abstract ▼ Abstract: We have used synchrotron Fe-XANES, XRS, microRaman, and SEM-TEM analyses of Stardust track 41 slice and track 121 terminal area slices to identify Fe oxide (magnetite-hematite and amorphous oxide), Fe-Ti oxide, and V-rich chromite (Fe-Cr-V-Ti-Mn oxide) grains ranging in size from 200 nm to ∼10 μm. They co-exist with relict FeNi metal. Both Fe-XANES and microRaman analyses suggest that the FeNi metal and magnetite (Fe2O3FeO) also contain some hematite (Fe2O3). The FeNi has been partially oxidized (probably during capture), but on the basis of our experimental work with a light-gas gun and microRaman analyses, we believe that some of the magnetite-hematite mixtures may have originated on Wild 2. The terminal samples from track 121 also contain traces of sulfide and Mg-rich silicate minerals. Our results show an unequilibrated mixture of reduced and oxidized Fe-bearing minerals in the Wild 2 samples in an analogous way to mineral assemblages seen in carbonaceous chondrites and interplanetary dust particles. The samples contain some evidence for terrestrial contamination, for example, occasional Zn-bearing grains and amorphous Fe oxide in track 121 for which evidence of a cometary origin is lacking.	Feb 2010

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