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1. The Metal-Silicate Partitioning of Carbon During Earth's Accretion and its Distribution in the Early Solar System

Author

Blanchard, I., Rubie, D. C., Jennings, E. S., Franchi, I. A., Zhao, X., Petitgirard, S., Miyajima, N., Jacobson, S. A., and Morbidelli, A.

Subjects
Astrophysics - Earth and Planetary Astrophysics, Physics - Geophysics
Abstract

Carbon is an essential element for the existence and evolution of life on Earth. Its abundance in Earth's crust and mantle (the Bulk Silicate Earth, BSE) is surprisingly high given that carbon is strongly siderophile (metal-loving) at low pressures and temperatures, and hence should have segregated almost completely into Earth's core during accretion. Estimates of the concentration of carbon in the BSE lie in the range 100-260 ppm and are much higher than expected based on simple models of core-mantle differentiation. Here we show through experiments at the putative conditions of Earth's core formation (49-71 GPa and 3600-4000 K) that carbon is significantly less siderophile at these conditions than at the low pressures ($\leq$13 GPa) and temperatures ($\leq$2500 K) of previous large volume press studies, but at least an order of magnitude more siderophile than proposed recently based on an experimental approach that is similar to ours. Using our new data along with previously published results, we derive a new parameterization of the pressure-temperature dependence of the metal-silicate partitioning of carbon. We apply this parameterization in a model that combines planet formation and core-mantle differentiation that is based on astrophysical N-body accretion simulations. Because differentiated planetesimals were almost completely depleted in carbon due to sublimation at high temperatures, almost all carbon in the BSE was added by the accretion of fully-oxidized carbonaceous chondrite material from the outer solar system. Carbon is added to the mantle continuously throughout accretion and its concentration reaches values within the BSE range (e.g. 140$\pm$40 ppm) at the end of accretion. The corresponding final core and bulk Earth carbon concentrations are 1270$\pm$300 ppm and 495$\pm$125 ppm respectively., Comment: Supplementary material included in pdf

Published
2022
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3. OSIRIS-REx Contamination Control Strategy and Implementation

Author

Dworkin, J. P., Adelman, L. A., Ajluni, T., Andronikov, A. V., Aponte, J. C., Bartels, A. E., Beshore, E., Bierhaus, E. B., Brucato, J. R., Bryan, B. H., Burton, A. S., Callahan, M. P., Castro-Wallace, S. L., Clark, B. C., Clemett, S. J., Connolly Jr., H. C., Cutlip, W. E., Daly, S. M., Elliott, V. E., Elsila, J. E., Enos, H. L., Everett, D. F., Franchi, I. A., Glavin, D. P., Graham, H. V., Hendershot, J. E., Harris, J. W., Hill, S. L., Hildebrand, A. R., Jayne, G. O., Jenkens Jr., R. W., Johnson, K. S., Kirsch, J. S., Lauretta, D. S., Lewis, A. S., Loiacono, J. J., Lorentson, C. C., Marshall, J. R., Martin, M. G., Matthias, L. L., McLain, H. L., Messenger, S. R., Mink, R. G., Moore, J. L., Nakamura-Messenger, K., Nuth III, J. A., Owens, C. V., Parish, C. L., Perkins, B. D., Pryzby, M. S., Reigle, C. A., Righter, K., Rizk, B., Russell, J. F., Sandford, S. A., Schepis, J. P., Songer, J., Sovinski, M. F., Stahl, S. E., Thomas-Keprta, K., Vellinga, J. M., and Walker, M. S.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

OSIRIS-REx will return pristine samples of carbonaceous asteroid Bennu. This article describes how pristine was defined based on expectations of Bennu and on a realistic understanding of what is achievable with a constrained schedule and budget, and how that definition flowed to requirements and implementation. To return a pristine sample, the OSIRIS- REx spacecraft sampling hardware was maintained at level 100 A/2 and <180 ng/cm2 of amino acids and hydrazine on the sampler head through precision cleaning, control of materials, and vigilance. Contamination is further characterized via witness material exposed to the spacecraft assembly and testing environment as well as in space. This characterization provided knowledge of the expected background and will be used in conjunction with archived spacecraft components for comparison with the samples when they are delivered to Earth for analysis. Most of all, the cleanliness of the OSIRIS-REx spacecraft was achieved through communication among scientists, engineers, managers, and technicians., Comment: 75 pages, 28 figures, 2 supplements, accepted for publication in Space Science Reviews

Published
2017
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6. The formation and aqueous alteration of CM2 chondrites and their relationship to CO3 chondrites: A fresh isotopic (O, Cd, Cr, Si, Te, Ti, and Zn) perspective from the Winchcombe CM2 fall.

Author

Greenwood, R. C., Findlay, R., Martins, R., Steele, R. C. J., Shaw, K. M. M., Morton, E., Savage, P. S., Murphy, M. E., Rehkämper, M., Franchi, I. A., Elliott, T., Suttle, M. D., King, A. J., Anand, M., Malley, J., Howard, K. T., Zhao, X., Johnson, D., Liu, M.‐C., and McCain, K. A.

Subjects
CHONDRITES, OXYGEN isotopes, PROTOPLANETARY disks, ISOTOPIC analysis, METEORITES, SIDEROPHILE elements
Abstract

As part of an integrated consortium study, we have undertaken O, Cd, Cr, Si, Te, Ti, and Zn whole rock isotopic measurements of the Winchcombe CM2 meteorite. δ66Zn values determined for two Winchcombe aliquots are +0.29 ± 0.05‰ (2SD) and +0.45 ± 0.05‰ (2SD). The difference between these analyses likely reflects sample heterogeneity. Zn isotope compositions for Winchcombe show excellent agreement with published CM2 data. δ114Cd for a single Winchcombe aliquot is +0.29 ± 0.04‰ (2SD), which is close to a previous result for Murchison. δ130Te values for three aliquots gave indistinguishable results, with a mean value of +0.62 ± 0.01‰ (2SD) and are essentially identical to published values for CM2s. ε53Cr and ε54Cr for Winchcombe are 0.319 ± 0.029 (2SE) and 0.775 ± 0.067 (2SE), respectively. Based on its Cr isotopic composition, Winchcombe plots close to other CM2 chondrites. ε50Ti and ε46Ti values for Winchcombe are 3.21 ± 0.09 (2SE) and 0.46 ± 0.08 (2SE), respectively, and are in line with recently published data for CM2s. The δ30Si composition of Winchcombe is −0.50 ± 0.06‰ (2SD, n = 11) and is essentially indistinguishable from measurements obtained on other CM2 chondrites. In conformity with petrographic observations, oxygen isotope analyses of both bulk and micromilled fractions from Winchcombe clearly demonstrate that its parent body experienced extensive aqueous alteration. The style of alteration exhibited by Winchcombe is consistent with relatively closed system processes. Analysis of different fractions within Winchcombe broadly support the view that, while different lithologies within an individual CM2 meteorite can be highly variable, each meteorite is characterized by a predominant alteration type. Mixing of different lithologies within a regolith environment to form cataclastic matrix is supported by oxygen isotope analysis of micromilled fractions from Winchcombe. Previously unpublished bulk oxygen isotope data for 12 CM2 chondrites, when combined with published data, define a well‐constrained regression line with a slope of 0.77. Winchcombe analyses define a more limited linear trend at the isotopically heavy, more aqueously altered, end of the slope 0.77 CM2 array. The CM2 slope 0.77 array intersects the oxygen isotope field of CO3 falls, indicating that the unaltered precursor material to the CMs was essentially identical in oxygen isotope composition to the CO3 falls. Our data are consistent with earlier suggestions that the main differences between the CO3s and CM2s reflect differing amounts of water ice that co‐accreted into their respective parent bodies, being high in the case of CM2s and low in the case of CO3s. The small difference in Si isotope compositions between the CM and CO meteorites can be explained by different proportions of matrix versus refractory silicates. CMs and COs may also be indistinguishable with respect to Ti and Cr isotopes; however, further analysis is required to test this possibility. The close relationship between CO3 and CM2 chondrites revealed by our data supports the emerging view that the snow line within protoplanetary disks marks an important zone of planetesimal accretion. [ABSTRACT FROM AUTHOR]

Published
2024
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7. Quantitative evolved gas analysis: Winchcombe in comparison with other CM2 meteorites.

Author

Verchovsky, A. В., Abernethy, F. A. J., Anand, M., Barber, S. J., Findlay, R., Franchi, I. A., Greenwood, R. C., and Grady, M. M.

Subjects
GAS analysis, METEORITES, CHEMICAL weathering, WEATHERING, MASS spectrometers, CARBON dioxide, PHYLLOSILICATES
Abstract

Two bulk Winchcombe along with six other CM2 meteorite samples were subjected to quantitative evolved gas analysis. The observed release patterns for almost all volatile species demonstrate close similarity for all the samples and especially between those for Winchcombe. This can be considered as a fingerprint for this petrological type of meteorites. We identified several gases including H2, H2O, O2, CO, CO2, and SO2 released in different temperature ranges. The sources and mechanisms of their release were also established. Some of the gases, H2, CO, and CO2, are released as a result of oxidation of macromolecular organic material from oxygen derived from oxygen‐bearing minerals (a part of CO2 is also released as a result of decomposition of carbonates). The others, O2 and H2O, are associated with the phase transformation/decomposition of phyllosilicates and (oxy)hydrates, while a high‐temperature release of SO2 is associated mostly with the decomposition of sulfides and in few cases also with sulfates. A low‐temperature release of SO2 is due to evaporation and oxidation of elemental sulfur from the meteoritic matrix and organic material. The total concentrations of H (mostly represented by H2O), C, and S, calculated according to calibration of the quadrupole mass spectrometer with reference gases and decomposition of solid samples (CaSO4·2H2O and NaHCO3) are in reasonable agreement with those determined by independent methods. Variations in the ratio of the carbon amounts released as CO2 and CO (CCO2/CCO) between the samples could be an indicator of their terrestrial weathering. [ABSTRACT FROM AUTHOR]

Published
2024
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10. The impact history and prolonged magmatism of the angrite parent body.

Author

Rider‐Stokes, B. G., Anand, M., White, L. F., Darling, J. R., Tartèse, R., Whitehouse, M. J., Franchi, I., Greenwood, R. C., and Degli‐Alessandrini, G.

Subjects
MAGMATISM, OXYGEN isotopes, METEORITES, SOLAR system, TRACE elements, OLIVINE
Abstract

As some of the oldest differentiated materials in our solar system, angrite meteorites can provide unique insights into the earliest stages of planetary evolution. However, the timing of planetary mixing, as evidenced by oxygen isotope variations in the quenched angrites, and the extent of magmatism on the angrite parent body (APB) remain poorly understood. Here, we report on microstructurally guided in situ geochemical and Pb–Pb isotopic measurements on angrites aimed at better understanding of the timing and nature of magmatic processes, as well as impact events, on the APB. The quenched angrite Northwest Africa (NWA) 12320 yielded a Pb–Pb date of 4571.2 ± 9.4 Ma, which we interpret as corresponding to the timing of planetary mixing. The only known shocked quenched angrite, NWA 7203, also yielded an ancient Pb–Pb date of 4562.9 ± 9.3 Ma, which is identical to the Pb–Pb date of 4563.6 ± 7.9 Ma obtained for the texturally intermediate angrite NWA 10463. Pb–Pb analyses in phosphates in the dunitic angrite NWA 8535 yielded a much younger date of 4514 ± 30 Ma, representing the youngest Pb–Pb date ever recorded for an angrite. Based on the evidence from the lack of shock deformation, olivine major and trace element compositions, and no apparent contamination in the oxygen isotope composition of NWA 8535, our findings are consistent with prolonged magmatism on the APB. This finding is consistent with a large size for the APB. [ABSTRACT FROM AUTHOR]

Published
2024
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12. The formation and aqueous alteration of CM2 chondrites and their relationship to CO3 chondrites: A fresh isotopic (O, Cd, Cr, Si, Te, Ti, and Zn) perspective from the Winchcombe CM2 fall

Author

Greenwood, R. C., primary, Findlay, R., additional, Martins, R., additional, Steele, R. C. J., additional, Shaw, K. M. M., additional, Morton, E., additional, Savage, P. S., additional, Murphy, M. E., additional, Rehkämper, M., additional, Franchi, I. A., additional, Elliott, T., additional, Suttle, M. D., additional, King, A. J., additional, Anand, M., additional, Malley, J., additional, Howard, K. T., additional, Zhao, X., additional, Johnson, D., additional, Liu, M.‐C., additional, McCain, K. A., additional, and Stephen, N. R., additional

Published
2023
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14. The grain size distribution of matrix in primitive chondrites

Author

Vaccaro, E., Wozniakiewicz, Penelope J., Franchi, I. A., Starkey, N., Russell, S. S., Vaccaro, E., Wozniakiewicz, Penelope J., Franchi, I. A., Starkey, N., and Russell, S. S.

Abstract

The matrix of primitive chondrites is composed of submicron crystals embedded in amorphous silicates. These grains are thought to be the remains of relatively unprocessed dust from the inner regions of the protoplanetary disk. The matrix of primitive meteorites is often compared to chondritic porous interplanetary dust particles (CP‐IDPs) which are believed to be of cometary origin, having accreted in the outermost regions of the solar nebula. Crystalline grains in CP‐IDPs show evidence of a size–density relationship between the silicates and sulfides suggesting that these components experienced sorting prior to accretion. Here, we investigate whether such evidence of sorting is also present in the matrix constituents of primitive chondrites. We report findings from our study of grain size distributions of discrete silicate and opaque (sulfide and metal) grains within the matrix of the primitive meteorites Acfer 094 (C2‐ung.), ALHA77307 (CO3), MIL 07687 (C3‐ung.), and QUE 99177 (CR2). Mean radii of matrix silicate grains range from 103 nm in QUE 99177 to 2018 nm in MIL 07687. The opaque grains show a wider variation, with average radii ranging from 15 nm in QUE 99177 to 219 nm in MIL07687. Our results indicate that, in contrast to CP‐IDPs, the size distribution of matrix components of these primitive meteorites cannot be explained by aerodynamic sorting that took place prior to accretion. We conclude that any evidence of sorting is likely to have been lost due to a greater variety and degree of processing experienced on these primitive chondrites than on cometary parent bodies.

Published
2023

15. Properties of Rubble-Pile Asteroid (101955) Bennu from OSIRIS-REx Imaging and Thermal Analysis

Author

DellaGiustina, D. N, Emery, J. P, Golish, D. R, Rozitis, B, Bennett, C. A, Burke, K. N, Ballouz, R.-L, Becker, K. J, Christensen, P. R, Drouet d’Aubigny, C. Y, Hamilton, V. E, Reuter, D. C, Rizk, B, Simon, A. A, Asphaug, E, Bandfield, J. L, Barnouin, O. S, Barucci, M. A, Binzel, R. P, Bottke, W. F, Bowles, N. E, Campins, H, Clark, B. C, Clark, B. E, Connolly, H. C., Jr, Daly, M. G, de Leon, J, Delbo, M, Deshapriya, J. D. P, Fornasier, S, Hergenrother, C. W, Jawin, E. R, Howell, E. S, Kaplan, H. H, Kareta, T. R, Corre, L. Le, Li, J.-Y, Licandro, J, Lim, L. F, Michel, P, Molaro, J, Nolan, M. C, Popescu, M, Rizos Garcia, J. L, Ryan, A, Schwartz, S. R, Shultz, N, Siegler, M. A, Smith, P. H, Tatsumi, E, Thomas, C. A, Walsh, K. J, Wolner, C. W. V, Zou, X.-D, Lauretta, D. S, Highsmith, D. E, Small, J, Vokrouhlick, D, Brown, E, Hanna, K. L. Donaldson, Warren, T, Brunet, C, Chicoine, R. A, Desjardins, S, Gaudreau, D, Haltigin, T, Millington-Veloza, S, Rubi, A, Aponte, J, Gorius, N, Lunsford, A, Allen, B, Grindlay, J, Guevel, D, Hoak, D, Hong, J, Schrader, D. L, Bayron, J, Golubov, O, Sánchez, P, Stromberg, J, Hirabayashi, M, Hartzell, C. M, Oliver, S, Rascon, M, Harch, A, Joseph, J, Squyres, S, Richardson, D, McGraw, L, Ghent, R, Al Asad, M. M, Johnson, C. L, Philpott, L, Susorney, H. C. M, Cloutis, E. A, Hanna, R. D, Ciceri, F, Hildebrand, A. R, Ibrahim, E.-M, Breitenfeld, L, Glotch, T, Rogers, A. D, Ferrone, S, Fernandez, Y, Chang, W, Cheuvront, A, Trang, D, Tachibana, S, Yurimoto, H, Brucato, J. R, Poggiali, G, Pajola, M, Dotto, E, Mazzotta Epifani, E, Crombie, M. K, Lantz, C, Izawa, M. R. M, Leon, J. de, Clemett, S, Thomas-Keprta, K, Van wal, S, Yoshikawa, M, Bellerose, J, Bhaskaran, S, Boyles, C, Chesley, S. R, Elder, C. M, Farnocchia, D, Harbison, A, Kennedy, B, Knight, A, Martinez-Vlasoff, N, Mastrodemos, N, McElrath, T, Owen, W, Park, R, Rush, B, Swanson, L, Takahashi, Y, Velez, D, Yetter, K, Thayer, C, Adam, C, Antreasian, P, Bauman, J, Bryan, C, Carcich, B, Corvin, M, Geeraert, J, Hoffman, J, Leonard, J. M, Lessac-Chenen, E, Levine, A, McAdams, J, McCarthy, L, Nelson, D, Page, B, Pelgrift, B, Sahr, E, Stakkestad, K, Stanbridge, D, Wibben, D, Williams, B, Williams, K, Wolff, P, Hayne, P, Kubitschek, D, Fulchignoni, M, Hasselmann, P, Merlin, F, Praet, A, Bierhaus, E. B, Billett, O, Boggs, A, Buck, B, Carlson-Kelly, S, Cerna, J, Chaffin, K, Church, E, Coltrin, M, Daly, J, Deguzman, A, Dubisher, R, Eckart, D, Ellis, D, Falkenstern, P, Fisher, A, Fisher, M. E, Fleming, P, Fortney, K, Francis, S, Freund, S, Gonzales, S, Haas, P, Hasten, A, Hauf, D, Hilbert, A, Howell, D, Jaen, F, Jayakody, N, Jenkins, M, Johnson, K, Lefevre, M, Ma, H, Mario, C, Martin, K, May, C, McGee, M, Miller, B, Miller, C, Miller, G, Mirfakhrai, A, Muhl, E, Norman, C, Olds, R, Parish, C, Ryle, M, Schmitzer, M, Sherman, P, Skeen, M, Susak, M, Sutter, B, Tran, Q, Welch, C, Witherspoon, R, Wood, J, Zareski, J, Arvizu-Jakubicki, M, Audi, E, Bandrowski, R, Becker, T. L, Bendall, S, Bloomenthal, H, Blum, D, Boynton, W. V, Brodbeck, J, Chojnacki, M, Colpo, A, Contreras, J, Cutts, J, Dean, D, Diallo, B, Drinnon, D, Drozd, K, Enos, H. L, Enos, R, Fellows, C, Ferro, T, Fisher, M. R, Fitzgibbon, G, Fitzgibbon, M, Forelli, J, Forrester, T, Galinsky, I, Garcia, R, Gardner, A, Habib, N, Hamara, D, Hammond, D, Hanley, K, Harshman, K, Herzog, K, Hill, D, Hoekenga, C, Hooven, S, Huettner, E, Janakus, A, Jones, J, Kidd, J, Kingsbury, K, Balram-Knutson, S. S, Koelbel, L, Kreiner, J, Lambert, D, Lewin, C, Lovelace, B, Loveridge, M, Lujan, M, Maleszewski, C. K, Malhotra, R, Marchese, K, McDonough, E, Mogk, N, Morrison, V, Morton, E, Munoz, R, Nelson, J, Padilla, J, Pennington, R, Polit, A, Ramos, N, Reddy, V, Riehl, M, Roper, H. L, Salazar, S, Selznick, S, Stewart, S, Sutton, S, Swindle, T, Tang, Y. H, Westermann, M, Worden, D, Zega, T, Zeszut, Z, Bjurstrom, A, Bloomquist, L, Dickinson, C, Keates, E, Liang, J, Nifo, V, Taylor, A, Teti, F, Caplinger, M, Bowles, H, Carter, S, Dickenshied, S, Doerres, D, Fisher, T, Hagee, W, Hill, J, Miner, M, Noss, D, Piacentine, N, Smith, M, Toland, A, Wren, P, Bernacki, M, Pino Munoz, D, Watanabe, S.-I, Sandford, S. A, Aqueche, A, Ashman, B, Barker, M, Bartels, A, Berry, K, Bos, B, Burns, R, Calloway, A, Carpenter, R, Castro, N, Cosentino, R, Donaldson, J, Dworkin, J. P, Cook, J. Elsila, Emr, C, Everett, D, Fennell, D, Fleshman, K, Folta, D, Gallagher, D, Garvin, J, Getzandanner, K, Glavin, D, Hull, S, Hyde, K, Ido, H, Ingegneri, A, Jones, N, Kaotira, P, Liounis, A, Lorentson, C, Lorenz, D, Lyzhoft, J, Mazarico, E. M, Mink, R, Moore, W, Moreau, M, Mullen, S, Nagy, J, Neumann, G, Nuth, J, Poland, D, Rhoads, L, Rieger, S, Rowlands, D, Sallitt, D, Scroggins, A, Shaw, G, Swenson, J, Vasudeva, P, Wasser, M, Zellar, R, Grossman, J, Johnston, G, Morris, M, Wendel, J, Burton, A, Keller, L. P, McNamara, L, Messenger, S, Nakamura-Messenger, K, Nguyen, A, Righter, K, Queen, E, Bellamy, K, Dill, K, Gardner, S, Giuntini, M, Key, B, Kissell, J, Patterson, D, Vaughan, D, Wright, B, Gaskell, R. W, Le Corre, L, Molaro, J. L, Palmer, E. E, Tricarico, P, Weirich, J. R, Ireland, T, Tait, K, Bland, P, Anwar, S, Bojorquez-Murphy, N, Haberle, C. W, Mehall, G, Rios, K, Franchi, I, Beddingfield, C. B, Marshall, J, Brack, D. N, French, A. S, McMahon, J. W, Scheeres, D. J, McCoy, T. J, Russell, S, Killgore, M, Chodas, M, Lambert, M, Masterson, R. A, Freemantle, J, Seabrook, J. A, Craft, K, Daly, R. T, Ernst, C, Espiritu, R. C, Holdridge, M, Jones, M, Nair, A. H, Nguyen, L, Peachey, J, Perry, M. E, Plescia, J, Roberts, J. H, Steele, R, Turner, R, Backer, J, Edmundson, K, Mapel, J, Milazzo, M, Sides, S, Manzoni, C, May, B, Libourel, G, Thuillet, F, and Marty, B

Subjects
Lunar And Planetary Science And Exploration
Abstract

Establishing the abundance and physical properties of regolith and boulders on asteroids is crucial for understanding the formation and degradation mechanisms at work on their surfaces. Using images and thermal data from NASA's Origins, Spectral Interpretation, Resource Identification, and Security-Regolith Explorer (OSIRIS-REx) spacecraft, we show that asteroid (101955) Bennu's surface is globally rough, dense with boulders, and low in albedo. The number of boulders is surprising given Bennu's moderate thermal inertia, suggesting that simple models linking thermal inertia to particle size do not adequately capture the complexity relating these properties. At the same time, we find evidence for a wide range of particle sizes with distinct albedo characteristics. Our findings imply that ages of Bennu's surface particles span from the disruption of the asteroid's parent body (boulders) to recent in situ production (micrometre-scale particles).

Published
2019
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17. The Winchcombe meteorite—A regolith breccia from a rubble pile CM chondrite asteroid

Author

Suttle, M. D., primary, Daly, L., additional, Jones, R. H., additional, Jenkins, L., additional, Van Ginneken, M., additional, Mitchell, J. T., additional, Bridges, J. C., additional, Hicks, L. J., additional, Johnson, D., additional, Rollinson, G., additional, Taylor, R., additional, Genge, M. J., additional, Schröder, C., additional, Trimby, P., additional, Mansour, H., additional, Piazolo, S., additional, Bonsall, E., additional, Salge, T., additional, Heard, R., additional, Findlay, R., additional, King, A. J., additional, Bates, H. C., additional, Lee, M. R., additional, Stephen, N. R., additional, Willcocks, F. M., additional, Greenwood, R. C., additional, Franchi, I. A., additional, Russell, S. S., additional, Harrison, C. S., additional, Schofield, P. F., additional, Almeida, N. V., additional, Floyd, C., additional, Martin, P.‐E., additional, Joy, K. H., additional, Wozniakiewicz, P. J., additional, Hallatt, D., additional, Burchell, M. J., additional, Alesbrook, L. S., additional, Spathis, V., additional, Cornwell, L. T., additional, and Dignam, A., additional

Published
2022
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18. The Significance of Slope 1 Variation in Early Solar System Solids

Author

Greenwood, R. C, Franchi, I. A, Alexander, C. M. O'D, Zolensky, M. E, and Buchanan, P. C

Subjects
Astrophysics
Abstract

As originally demonstrated by Clayton and co-workers, primitive meteorites and their components commonly display mass-independent oxygen isotopic variation. As a tool to understand this behaviour, a number of reference lines have been defined, with slopes of approximately 1. The Carbonaceous Chondrite Anhydrous Mineral (CCAM) line, derived predominantly from analyses of components in the Allende (CV3) meteorite, is the most widely used reference and has a slope of 0.94 plus or minus 0.01 (2 sigma). However, the fundamental significance of the CCAM line has been questioned. Based on the results of a UV laser ablation study of an Allende CAI (calcium-aluminum–rich inclusion), it was suggested that a line of exactly slope 1 (Y&R line - Young and Russell line) was of more fundamental significance. SIMS (Secondary Ion Mass Spectrometry) analysis of chondrules from primitive CRs and related chondrites define a third, distinct slope 1 line, known as the Primitive Chondrule Minerals (PCM) line. Here we discuss the results of bulk oxygen isotope analysis of CO, CV and CR chondrites and various separated components, with the aim of better understanding the origin of slope 1 behaviour in early Solar System materials.

Published
2018

19. Primitive Oxygen-, Nitrogen-, and Organic-Rich Vein Preserved in a Xenolith Hosted in the Metamorphosed Carancas Meteorite

Author

Chan, Q. H. S, Zolensky, M. E, Kebukawa, Y, Franchi, I, Wright, I, Zhao, I, Rahman, Z, and Utas, J

Subjects
Lunar And Planetary Science And Exploration
Abstract

Primitive xenolithic CI-like carbonaceous (C) clasts are sometimes hosted within meteorites of a different origin (ordinary chondrite, ureilite, howardite, and eucrite). These xenoliths contain aggregates of macromolecular carbon (MMC), which are often present as discrete grains and exhibit a wide range of structural order and chemical compositions. The Carancas meteorite is a H4-5 that impacted south of Lake Titicaca, Peru in 2007. While the meteorite exhibits extensive recrystallization of the matrix indicating metamorphism, it contains dark, CI-like clasts that show no evidence of heating. Similar to other xenolithic clasts, the examined C clast of Carancas contains MMC, which however exists in the form of a vein-like structure dissimilar to the typical occurrence of MMC in meteorites. We investigated the organic and isotopic compositions of the organic-rich vein with C,N,O-X-ray absorption near-edge structure (XANES), Raman spectroscopy, and NanoSIMS, in order to constrain its possible origin.

Published
2018

20. The Genesis Solar-Wind Collector Materials

Author

Jurewicz, A. J. G., Burnett, D. S., Wiens, R. C., Friedmann, T. A., Hays, C. C., Hohlfelder, R. J., Nishiizumi, K., Stone, J. A., Woolum, D. S., Becker, R., Butterworth, A. L., Campbell, A. J., Ebihara, M., Franchi, I. A., Heber, V., Hohenberg, C. M., Humayun, M., McKeegan, K. D., McNamara, K., Meshik, A., Pepin, R. O., Schlutter, D., Wieler, R., and Russell, Christopher T., editor

Published
2003
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22. OSIRIS-REx Contamination Control Strategy and Implementation

Author

Dworkin, J. P, Adelman, L. A, Ajluni, T, Andronikov, A. V, Aponte, J. C, Bartels, A. E, Beshore, E, Bierhaus, E. B, Brucato, J. R, Bryan, B. H, Burton, A. S, Castro-Wallace, S. L, Clark, B. C, Clemett, S. J, Connolly, H. C., Jr, Cutlip, W. E, Daly, S. M, Elliott, V. E, Elsila, J. E, Enos, H. L, Everett, D. F, Franchi, I. A, Glavin, D. P, Graham, H. V, Hendershot, J. E, Harris, J. W, Hill, S. L, Hildebrand, A. R, Jayne, G. O, Jenkens, R. W., Jr, Johnson, K. S, Kirsch, J. S, Lauretta, D. S, Lewis, A. S, Loiacono, J. J, Lorentson, C. C, Marshall, J. R, Martin, M. G, Matthias, L. L, McLain, H. L, Messenger, S. R, Mink, R. GT, Moore, J. L, Nakamura, Messenger, K, Nuth, J. A., III, Owens, C. V, Parish, C. L, Perkins, B. D, Pryzby, M. S, Reigle, C. A, Righter, K, Rizk, B, Russell, J. F, Sandford, S. A, Schepis, J. P, Songer, J, Sovinski, M. F, Stahl, S. E, Thomas-Keprta, K, Vellinga, J. M, and Walker, M. S

Subjects
Lunar And Planetary Science And Exploration
Abstract

OSIRIS-REx will return pristine samples of carbonaceous asteroid Bennu. This manuscript describes how pristine was defined based on expectations of Bennu and on a realistic understanding of what is achievable with a constrained schedule and budget, and how that definition flowed to requirements and implementation. To return a pristine sample, the OSIRIS-REx spacecraft sampling hardware was maintained at Level 100 A/2 and less than 180 nanograms per square centimeter of amino acids and hydrazine on the sampler head through precision cleaning, control of materials, and vigilance. Contamination is further characterized via witness material exposed to the spacecraft assembly and testing environment as well as in space. This characterization provided knowledge of the expected background and will be used in conjunction with archived spacecraft components for comparison with the samples when they are delivered to Earth for analysis. Most of all, the cleanliness of the OSIRIS-REx spacecraft was achieved through communication between scientists, engineers, managers, and technicians.

Published
2017

23. Chlorine in Lunar Basalts

Author

Barnes, J. J, Anand, M, and Franchi, I. A

Subjects
Lunar And Planetary Science And Exploration
Abstract

In the context of the lunar magma ocean (LMO) model, it is anticipated that chlorine (and other volatiles) should have been concentrated in the late-stage LMO residual melts (i.e., the dregs enriched in incompatible elements such as K, REEs, and P, collectively called KREEP, and in its primitive form - urKREEP, [1]), given its incompatibility in mafic minerals like olivine and pyroxene, which were the dominant phases that crystallized early in the cumulate pile of the LMO (e.g., [2]). When compared to chondritic meteorites and terrestrial rocks (e.g., [3-4]), lunar samples often display heavy chlorine isotope compositions [5-9]. Boyce et al. [8] found a correlation between delta Cl-37 (sub Ap) and bulk-rock incompatible trace elements (ITEs) in lunar basalts, and used this to propose that early degassing of Cl (likely as metal chlorides) from the LMO led to progressive enrichment in remaining LMO melt in Cl-37over Cl-35- the early degassing model. Barnes et al. [9] suggested that relatively late degassing of chlorine from urKREEP (to yield delta Cl-37 (sub urKREEP greater than +25 per mille) followed by variable mixing between KREEPy melts and mantle cumulates (characterized by delta Cl-37~0 per mille) could explain the majority of Cl isotope data from igneous lunar samples. In order to better understand the processes involved in giving rise to the heavy chlorine isotope compositions of lunar samples, we have performed an in situ study of chlorine isotopes and abundances of volatiles in lunar apatite from a diverse suite of lunar basalts spanning a range of geochemical types.

Published
2017

26. Tissemouminites: A new group of primitive achondrites spanning the transition between acapulcoites and winonaites.

Author

Stephant, A., Carli, C., Anand, M., Néri, A., Davidson, J., Pratesi, G., Cuppone, T., Greenwood, R. C., and Franchi, I. A.

Subjects
ACHONDRITES, NATIVE element minerals, OXYGEN isotopes, ISOTOPIC analysis, PLAGIOCLASE, MARTIAN meteorites, ISOTOPIC signatures
Abstract

The Northwest Africa (NWA) 090 meteorite, initially classified as an acapulcoite, presents petrological, chemical, and isotopic characteristics comparable to a group of seven primitive winonaites: Dhofar 1222, NWA 725, NWA 1052, NWA 1054, NWA 1058, NWA 1463, and NWA 8614. Five of these samples were previously classified as acapulcoites or ungrouped achondrites before being reclassified as winonaites based on their oxygen isotopic compositions. These misclassifications are indicative of the particular compositional nature of these primitive achondrites. All contain relict chondrules and a lower closure temperature of metamorphism of 820 ± 20 °C compared to other typical winonaites, as well as mineral elemental compositions similar to those of acapulcoites. The oxygen isotopic signature of these samples, δ17O of 1.18 ± 0.17‰, δ18O of 3.18 ± 0.30‰, and Δ17O of −0.47 ± 0.02, is in fact resolvable from both acapulcoites and winonaites. We investigate the relationship between these eight primitive achondrites, typical winonaites, and acapulcoites, to redefine petrological, mineralogical, and geochemical criteria of primitive achondrite classification. Distinguishing between winonaites, acapulcoites, and this group of eight primitive achondrites can be unambiguously done using a combination of several mineralogical and chemical criteria. A combination of olivine fayalite content and FeO/MnO ratio, as well as plagioclase potassium content allow us to separate these three groups without the absolute necessity of oxygen isotope analyses. NWA 090 as well as the other seven primitive achondrites, although related to winonaites, are most likely derived from a parent body distinct from winonaites and acapulcoites–lodranites, and define a new group of primitive achondrites that can be referred to as tissemouminites. [ABSTRACT FROM AUTHOR]

Published
2023
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28. H-Isotopic Composition of Apatite in Northwest Africa 7034

Author

McCubbin, F. M, Barnes, J. J, Santos, A. R, Boyce, J. W, Anand, M, Franchi, I. A, and Agee, C. B

Subjects
Lunar And Planetary Science And Exploration
Abstract

Northwest Africa (NWA) 7034 and its pairings comprise a regolith breccia with a basaltic bulk composition [1] that yields a better match than any other martian meteorite to estimates of Mars' bulk crust composition [1]. Given the similarities between NWA 7034 and the martian crust, NWA 7034 may represent an important sample for constraining the crustal composition of components that cannot be measured directly by remote sensing. In the present study, we seek to constrain the H isotopic composition of the martian crust using Cl-rich apatite in NWA 7034.

Published
2016

29. The Chlorine Isotopic Composition Of Lunar UrKREEP

Author

Barnes, J. J, Tartese, R, Anand, M, McCubbin, F. M, Neal, C. R, and Franchi, I. A

Subjects
Lunar And Planetary Science And Exploration, Geophysics
Abstract

Since the long standing paradigm of an anhydrous Moon was challenged there has been a renewed focus on investigating volatiles in a variety of lunar samples. However, the current models for the Moon’s formation have yet to fully account for its thermal evolution in the presence of H2O and other volatiles. When compared to chondritic meteorites and terrestrial rocks, lunar samples have exotic chlorine isotope compositions, which are difficult to explain in light of the abundance and isotopic composition of other volatile species, especially H, and the current estimates for chlorine and H2O in the bulk silicate Moon. In order to better understand the processes involved in giving rise to the heavy chlorine isotope compositions of lunar samples, we have performed a comprehensive in situ high precision study of chlorine isotopes, using NanoSIMS (Nanoscale Secondary Ion Mass Spectrometry) of lunar apatite from a suite of Apollo samples covering a range of geochemical characteristics and petrologic types.

Published
2016

30. The Origin and Significance of the CCAM Line: Evidence from Chondrules and Dark Inclusions in Allende (CV3)

Author

Greenwood, R. C, Franchi, I. A, Zolensky, M. E, and Buchanan, P. C

Subjects
Astrophysics, Lunar And Planetary Science And Exploration
Abstract

The process responsible for the mass independent oxygen isotope variation observed in Solar System materials remains poorly understood. While self-shielding of CO, either in the early solar nebula, or precursor molecular cloud, appears to be a viable mechanism, alternative models have also been proposed.

Published
2016

31. Hydrogen Isotopic Composition of Apatite in Northwest Africa 7034: A Record of the 'Intermediate' H-Isotopic Reservoir in the Martian Crust?

Author

McCubbin, F. M, Barnes, J. J, Santos, A. R, Boyce, J. W, Anand, M, Franchi, I. A, and Agee, C. B

Subjects
Lunar And Planetary Science And Exploration
Abstract

Northwest Africa (NWA) 7034 and its pairings comprise a regolith breccia with a basaltic bulk composition [1] that yields a better match than any other martian meteorite to visible-infrared reflectance spectra of the martian surface measured from orbit [2]. The composition of the fine-grained matrix within NWA 7034 bears a striking resemblance to the major element composition estimated for the martian crust, with several exceptions. The NWA 7034 matrix is depleted in Fe, Ti, and Cr and enriched in Al, Na, and P [3]. The differences in Al and Fe are the most substantial, but the Fe content of NWA 7034 matrix falls within the range reported for the southern highlands crust [6]. It was previously suggested by [4] that NWA 7034 was sourced from the southern highlands based on the ancient 4.4 Ga ages recorded in NWA 7034/7533 zircons [4, 5]. In addition, the NWA 7034 matrix material is enriched in incompatible trace elements by a factor of 1.2-1.5 [7] relative to estimates of the bulk martian crust. The La/Yb ratio of the bulk martian crust is estimated to be approximately 3 [7], and the La/Yb of the NWA 7034 matrix materials ranges from approximately 3.9 to 4.4 [3, 8], indicating a higher degree of LREE enrichment in the NWA 7034 matrix materials. This elevated La/Yb ratio and enrichment in incompatible lithophile trace elements is consistent with NWA 7034 representing a more geochemically enriched crustal terrain than is represented by the bulk martian crust, which would be expected if NWA 7034 represents the bulk crust from the southern highlands. Given the similarities between NWA 7034 and the martian crust, NWA 7034 may represent an important sample for constraining the composition of the martian crust, particularly the ancient highlands. In the present study, we seek to constrain the H isotopic composition of the martian crust using Cl-rich apatite in NWA 7034. Usui et al., [9] recently proposed that a H isotopic reservoir exists within the martian crust that has a H-isotopic composition that is intermediate (δD of 1000-2000per mille) between an isotopically light mantle (Delta D is less than 275per mille [10]) and an isotopically heavy atmosphere (δD of 2500-6100per mille [11, 12]). Apatites in NWA 7034 occur in a number of lithologic domains, however apatites across all lithologic domains have been affected by a Pb-loss event at about 1.5 Ga before present [5], so they are unlikely to have retained a primary composition and are more likely to have equilibrated with fluids within the martian crust that may or may not have exchanged with the martian atmosphere. Equilibration of apatite with crustal fluids is further supported by the chlorine-rich compositions exhibited by apatites in NWA 7034 in comparison to apatites from other martian meteorites (Figure 1; [13]). Cl is more hydrophilic than F, which promotes formation of Cl-rich apatite compositions in fluid-rich systems [e.g., 14, 15-17].

Published
2016

32. Craters, boulders and regolith of (101955) Bennu indicative of an old and dynamic surface

Author

Walsh, KJ, Jawin, ER, Ballouz, R-L, Barnouin, OS, Bierhaus, EB, Jr, CHC, Molaro, JL, McCoy, TJ, Delbo', M, Hartzell, CM, Pajola, M, Schwartz, SR, Trang, D, Asphaug, E, Becker, KJ, Beddingfield, CB, Bennett, CA, Bottke, WF, Burke, KN, Clark, BC, Daly, MG, Dellagiustina, DN, Dworkin, JP, Elder, CM, Golish, DR, Hildebrand, AR, Malhotra, R, Marshall, J, Michel, P, Nolan, MC, Perry, ME, Rizk, B, Ryan, A, Sandford, SA, Scheeres, DJ, Susorney, HCM, Thuillet, F, Lauretta, DS, Highsmith, DE, Small, J, Vokrouhlicky, D, Bowles, NE, Brown, E, Hanna, KLD, Warren, T, Brunet, C, Chicoine, RA, Desjardins, S, Gaudreau, D, Haltigin, T, Millington-Veloza, S, Rubi, A, Aponte, J, Gorius, N, Lunsford, A, Allen, B, Grindlay, J, Guevel, D, Hoak, D, Hong, J, Schrader, DL, Bayron, J, Golubov, O, Sanchez, P, Stromberg, J, Hirabayashi, M, Oliver, S, Rascon, M, Harch, A, Joseph, J, Squyres, S, Richardson, D, Emery, JP, McGraw, L, Ghent, R, Binzel, RP, Asad, MM, Johnson, CL, Philpott, L, Cloutis, EA, Hanna, RD, Ciceri, F, Ibrahim, E-M, Breitenfeld, L, Glotch, T, Rogers, AD, Clark, BE, Ferrone, S, Thomas, CA, Campins, H, Fernandez, Y, Chang, W, Cheuvront, A, Tachibana, S, Yurimoto, H, Brucato, JR, Poggiali, G, Dotto, E, Epifani, EM, Crombie, MK, Lantz, C, Izawa, MRM, De Leon, J, Licandro, J, Garcia, JLR, Clemett, S, Thomas-Keprta, K, Van Wal, S, Yoshikawa, M, Bellerose, J, Bhaskaran, S, Boyles, C, Chesley, SR, Farnocchia, D, Harbison, A, Kennedy, B, Knight, A, Martinez-Vlasoff, N, Mastrodemos, N, McElrath, T, Owen, W, Park, R, Rush, B, Swanson, L, Takahashi, Y, Velez, D, Yetter, K, Thayer, C, Adam, C, Antreasian, P, Bauman, J, Bryan, C, Carcich, B, Corvin, M, Geeraert, J, Hoffman, J, Leonard, JM, Lessac-Chenen, E, Levine, A, McAdams, J, McCarthy, L, Nelson, D, Page, B, Pelgrift, J, Sahr, E, Stakkestad, K, Stanbridge, D, Wibben, D, Williams, B, Williams, K, Wolff, P, Hayne, P, Kubitschek, D, Barucci, MA, Deshapriya, JDP, Fornasier, S, Fulchignoni, M, Hasselmann, P, Merlin, F, Praet, A, Billett, O, Boggs, A, Buck, B, Carlson-Kelly, S, Cerna, J, Chaffin, K, Church, E, Coltrin, M, Daly, J, Deguzman, A, Dubisher, R, Eckart, D, Ellis, D, Falkenstern, P, Fisher, A, Fisher, ME, Fleming, P, Fortney, K, Francis, S, Freund, S, Gonzales, S, Haas, P, Hasten, A, Hauf, D, Hilbert, A, Howell, D, Jaen, F, Jayakody, N, Jenkins, M, Johnson, K, Lefevre, M, Ma, H, Mario, C, Martin, K, May, C, McGee, M, Miller, B, Miller, C, Miller, G, Mirfakhrai, A, Muhle, E, Norman, C, Olds, R, Parish, C, Ryle, M, Schmitzer, M, Sherman, P, Skeen, M, Susak, M, Sutter, B, Tran, Q, Welch, C, Witherspoon, R, Wood, J, Zareski, J, Arvizu-Jakubicki, M, Audi, E, Bandrowski, R, Becker, TL, Bendall, S, Bloomenthal, H, Blum, D, Boynton, WV, Brodbeck, J, Chojnacki, M, Colpo, A, Contreras, J, Cutts, J, D'Aubigny, CYD, Dean, D, Diallo, B, Drinnon, D, Drozd, K, Enos, HL, Enos, R, Fellows, C, Ferro, T, Fisher, MR, Fitzgibbon, G, Fitzgibbon, M, Forelli, J, Forrester, T, Galinsky, I, Garcia, R, Gardner, A, Habib, N, Hamara, D, Hammond, D, Hanley, K, Harshman, K, Hergenrother, CW, Herzog, K, Hill, D, Hoekenga, C, Hooven, S, Howell, ES, Huettner, E, Janakus, A, Jones, J, Kareta, TR, Kidd, J, Kingsbury, K, Balram-Knutson, SS, Koelbel, L, Kreiner, J, Lambert, D, Lewin, C, Lovelace, B, Loveridge, M, Lujan, M, Maleszewski, CK, Marchese, K, McDonough, E, Mogk, N, Morrison, V, Morton, E, Munoz, R, Nelson, J, Padilla, J, Pennington, R, Polit, A, Ramos, N, Reddy, V, Riehl, M, Roper, HL, Salazar, S, Selznick, S, Shultz, N, Smith, PH, Stewart, S, Sutton, S, Swindle, T, Tang, YH, Westermann, M, Wolner, CWV, Worden, D, Zega, T, Zeszut, Z, Bjurstrom, A, Bloomquist, L, Dickinson, C, Keates, E, Liang, J, Nifo, V, Taylor, A, Teti, F, Caplinger, M, Bowles, H, Carter, S, Dickenshied, S, Doerres, D, Fisher, T, Hagee, W, Hill, J, Miner, M, Noss, D, Piacentine, N, Smith, M, Toland, A, Wren, P, Bernacki, M, Munoz, DP, Watanabe, S-I, Aqueche, A, Ashman, B, Barker, M, Bartels, A, Berry, K, Bos, B, Burns, R, Calloway, A, Carpenter, R, Castro, N, Cosentino, R, Donaldson, J, Cook, JE, Emr, C, Everett, D, Fennell, D, Fleshman, K, Folta, D, Gallagher, D, Garvin, J, Getzandanner, K, Glavin, D, Hull, S, Hyde, K, Ido, H, Ingegneri, A, Jones, N, Kaotira, P, Lim, LF, Liounis, A, Lorentson, C, Lorenz, D, Lyzhoft, J, Mazarico, EM, Mink, R, Moore, W, Moreau, M, Mullen, S, Nagy, J, Neumann, G, Nuth, J, Poland, D, Reuter, DC, Rhoads, L, Rieger, S, Rowlands, D, Sallitt, D, Scroggins, A, Shaw, G, Simon, AA, Swenson, J, Vasudeva, P, Wasser, M, Zellar, R, Grossman, J, Johnston, G, Morris, M, Wendel, J, Burton, A, Keller, LP, McNamara, L, Messenger, S, Nakamura-Messenger, K, Nguyen, A, Righter, K, Queen, E, Bellamy, K, Dill, K, Gardner, S, Giuntini, M, Key, B, Kissell, J, Patterson, D, Vaughan, D, Wright, B, Gaskell, RW, Le Corre, L, Li, J-Y, Palmer, EE, Siegler, MA, Tricarico, P, Weirich, JR, Zou, X-D, Ireland, T, Tait, K, Bland, P, Anwar, S, Bojorquez-Murphy, N, Christensen, PR, Haberle, CW, Mehall, G, Rios, K, Franchi, I, Rozitis, B, Brack, DN, French, AS, McMahon, JW, Russell, S, Killgore, M, Hamilton, VE, Kaplan, HH, Bandfield, JL, Chodas, M, Lambert, M, Masterson, RA, Freemantle, J, Seabrook, JA, Craft, K, Daly, RT, Ernst, C, Espiritu, RC, Holdridge, M, Jones, M, Nair, AH, Nguyen, L, Peachey, J, Plescia, J, Roberts, JH, Steele, R, Turner, R, Backer, J, Edmundson, K, Mapel, J, Milazzo, M, Sides, S, Manzoni, C, May, B, Delbo, M, Libourel, G, Marty, B, Team, O-R, Centro di Ateneo di Studi e Attività Spaziali 'Giuseppe Colombo' (CISAS), Universita degli Studi di Padova, Laboratoire de Géophysique Interne et Tectonophysique (LGIT), Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Laboratoire Central des Ponts et Chaussées (LCPC)-Institut des Sciences de la Terre (ISTerre), Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-PRES Université de Grenoble-Institut de recherche pour le développement [IRD] : UR219-Institut national des sciences de l'Univers (INSU - CNRS)-Institut Français des Sciences et Technologies des Transports, de l'Aménagement et des Réseaux (IFSTTAR)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS)-PRES Université de Grenoble-Institut de recherche pour le développement [IRD] : UR219-Institut Français des Sciences et Technologies des Transports, de l'Aménagement et des Réseaux (IFSTTAR), ASU School of Earth and Space Exploration (SESE), Arizona State University [Tempe] (ASU), IHU-LIRYC, Université Bordeaux Segalen - Bordeaux 2-CHU Bordeaux [Bordeaux], NASA Goddard Space Flight Center (GSFC), National Dairy Research Institute, SETI Institute, Institute of Northern Engineering, 455 Duckering Bldg, Lunar and Planetary Laboratory [Tucson] (LPL), University of Arizona, Centre de Mise en Forme des Matériaux (CEMEF), Centre National de la Recherche Scientifique (CNRS)-PSL Research University (PSL)-MINES ParisTech - École nationale supérieure des mines de Paris, Institut des Sciences de la Terre (ISTerre), Institut Français des Sciences et Technologies des Transports, de l'Aménagement et des Réseaux (IFSTTAR)-Institut national des sciences de l'Univers (INSU - CNRS)-Institut de recherche pour le développement [IRD] : UR219-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), MINES ParisTech - École nationale supérieure des mines de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), and ANR-15-IDEX-0001,UCA JEDI,Idex UCA JEDI(2015)

Subjects
Near-Earth object, 010504 meteorology & atmospheric sciences, Mass movement, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Geomorphology, 010502 geochemistry & geophysics, 01 natural sciences, Billion years, Regolith, Astrobiology, [SPI]Engineering Sciences [physics], Asteroids comets and Kuiper belt, Impact crater, Asteroid, General Earth and Planetary Sciences, Asteroid belt, Early solar system, Geology, 0105 earth and related environmental sciences
Abstract

著者人数: 38名ほか (The OSIRIS-REx Team: 所属. 宇宙航空研究開発機構宇宙科学研究所(JAXA)(ISAS): Van wal, S; 吉川, 真; 渡邊, 誠一郎), Number of authors: 38 and The OSIRIS-REx Team (Affiliation. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency(JAXA)(ISAS): Van wal, S; Yoshikawa, Makoto; Watanabe, Sei-icihro), Accepted: 2019-02-11, 資料番号: SA1190038000

Published
2019
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34. The OSIRIS-REx Contamination Control and Witness Strategy

Author

Dworkin, J. P, Adelman, L, Ajluni, T. M, Andronikov, A. V, Ballou, D. M, Bartels, A. E, Beshore, E, Bierhaus, E. B, Boynton, W. V, Brucato, J. R, Callahan, M. P, Benton, B. C, Connolly, H. C., Jr, Enos, H. L, Elsila, J. E, Everett, D. F, Franchi, I. A, Fust, J. S, Glavin, D. P, Hendershot, J. E, Harris, J. W, Hildebrand, A. R, Jayne, G, Jenkins, R. W, Kretsch, W. E, Kuhns, R. M, Lauretta, D. S, Ladewig, J. V, Lorentson, C. C, Marshall, J. R, Matthias, L. L, McLain, H. L, Messenger, S. R, Mink, R. G, Moore, J, Nakamura-Messenger, K, Nuth, J. A, Righter, K, Roher, W. D, Sandford, S. A, Schepis, J. P, Sovinski, M. F, and Walker, M. S

Subjects
Lunar And Planetary Science And Exploration, Life Sciences (General)
Abstract

The OSIRIS-REx mission (Origins, Spectral Interpretation, Resource Identification, and Security Regolith Explorer) is the third NASA New Frontiers mission. It is scheduled for launch in 2016. The primary objective of the mission is to return at least 60 g of "pristine" material from the B-type near- Earth asteroid (101955) Bennu, which is spectrally similar to organic-rich CI or CM meteorites [1]. The study of these samples will advance our understanding of materials available for the origin of life on Earth or elsewhere. The spacecraft will rendezvous with Bennu in 2018 and spend at least a year characterizing the asteroid before executing a maneuver to recover a sample of regolith in the touch-and-go sample acquisition mechanism (TAGSAM). The TAGSAM and sample is stowed in the sample return capsule (SRC) and returned to Earth in 2023.

Published
2015

35. The Oxygen Isotope Composition of Dark Inclusions in HEDs, Ordinary and Carbonaceous Chondrites

Author

Greenwood, R. C, Zolensky, M. E, Buchanan, P. C, and Franchi, I. A

Subjects
Lunar And Planetary Science And Exploration
Abstract

Dark inclusions (DIs) are lithic fragments that form a volumetrically small, but important, component in carbonaceous chondrites. Carbonaceous clasts similar to DIs are also found in some ordinary chondrites and HEDs. DIs are of particular interest because they provide a record of nebular and planetary processes distinct from that of their host meteorite. DIs may be representative of the material that delivered water and other volatiles to early Earth as a late veneer. Here we focus on the oxygen isotopic composition of DIs in a variety of settings with the aim of understanding their formational history and relationship to the enclosing host meteorite.

Published
2015

36. The Mineralogy and Petrology of Anomalous Eucrite Emmaville

Author

Barrett, T. J, Mittlefehldt, D. W, Ross, D. K, Greenwood, R. C, Anand, M, Franchi, I. A, Grady, M. M, and Charlier, B. L. A

Subjects
Lunar And Planetary Science And Exploration
Abstract

It has long been known that certain basaltic achondrites share similarities with eucrites. These eucrite-like achondrites have distinct isotopic compositions and petrologic characteristics indicative of formation on a separate parent body from the howardite-eucrite-diogenite (HED) clan (e.g., Ibitira, Northwest Africa (NWA) 011). Others show smaller isotopic variations but are otherwise petrologically and compositionally indistinguishable from basaltic eucrites (e.g., Pasamonte, Pecora Escarpment (PCA) 91007). The Emmaville eucrite has a delta O-17 value of -0.137 plus or minus 0.024 per mille (1 sigma), which is substantially different from the eucrite mean of -0.246 plus or minus 0.014 per mille (2 sigma), but similar to those of A-881394 and Bunburra Rockhole (BR). Currently little data exist for Emmaville in terms of petrology or bulk composition. Studying anomalous eucrites allows us to more completely understand the numbers of asteroids represented by eucrite- like basalts and thus constrain the heterogeneity of the HED suite. In this study, we present our preliminary petrological and mineral composition results for Emmaville.

Published
2015

37. MarcoPolo-R near earth asteroid sample return mission

Author

Barucci, Maria Antonietta, Cheng, A. F., Michel, P., Benner, L. A. M., Binzel, R. P., Bland, P. A., Böhnhardt, H., Brucato, J. R., Campo Bagatin, A., Cerroni, P., Dotto, E., Fitzsimmons, A., Franchi, I. A., Green, S. F., Lara, L.-M., Licandro, J., Marty, B., Muinonen, K., Nathues, A., Oberst, J., Rivkin, A. S., Robert, F., Saladino, R., Trigo-Rodriguez, J. M., Ulamec, S., and Zolensky, M.

Published
2012
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39. Kronos: exploring the depths of Saturn with probes and remote sensing through an international mission

Author

Marty, B., Guillot, T., Coustenis, A., Achilleos, N., Alibert, Y., Asmar, S., Atkinson, D., Atreya, S., Babasides, G., Baines, K., Balint, T., Banfield, D., Barber, S., Bézard, B., Bjoraker, G. L., Blanc, M., Bolton, S., Chanover, N., Charnoz, S., Chassefière, E., Colwell, J. E., Deangelis, E., Dougherty, M., Drossart, P., Flasar, F. M., Fouchet, T., Frampton, R., Franchi, I., Gautier, D., Gurvits, L., Hueso, R., Kazeminejad, B., Krimigis, T., Jambon, A., Jones, G., Langevin, Y., Leese, M., Lellouch, E., Lunine, J., Milillo, A., Mahaffy, P., Mauk, B., Morse, A., Moreira, M., Moussas, X., Murray, C., Mueller-Wodarg, I., Owen, T. C., Pogrebenko, S., Prangé, R., Read, P., Sanchez-Lavega, A., Sarda, P., Stam, D., Tinetti, G., Zarka, P., Zarnecki, J., and the Kronos consortium

Published
2009
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41. Sierra Gorda 009: A New Member of the Metal-Rich G Chondrites Grouplet

Author

Ivanova, M. A., Lorenz, C. A., Humayun, M., Corrigan, C. M., Ludwig, T., Trieloff, M., Righter, K., Franchi, I. A., Verchovsky, A. B., Korochantseva, E. V., Kozlov, V. V., Teplyakova, S. N., Korochantsev, A. V., and Grokhovsky, V. I.

Abstract

We investigated the metal-rich chondrite Sierra Gorda (SG) 009, a member of the new G chondrite grouplet (also including NWA 5492, GRO 95551). G chondrites contain 23% metal, very reduced silicates, and rare oxidized mineral phases (Mg-chromite, FeO-rich pyroxene). G chondrites are not related to CH-CB chondrites, based on bulk O, C, and N isotopic compositions, mineralogy, and geochemistry. G chondrites have no fine-grained matrix or matrix lumps enclosing hydrated material typical for CH-CB chondrites. G chondrites’ average metal compositions are similar to H chondrites. Siderophile and lithophile geochemistry indicates sulfidization and fractionation of the SG 009 metal and silicates, unlike NWA 5492 and GRO 95551. The G chondrites have average O isotopic compositions Δ17O'0‰ ranging between bulk enstatite (E) and ordinary (O) chondrites. An Al-rich chondrule from SG 009 has Δ17O'0‰ indicating some heterogeneity in oxygen isotopic composition of G chondrite components. SG 009’s bulk carbon and nitrogen isotopic compositions correspond to E and O chondrites. Neon isotopic composition reflects a mixture of cosmogenic and solar components, and cosmic ray exposure age of SG 009 is typical for O, E, and R chondrites. G chondrites are closely related to O, E, and R chondrites and may represent a unique metal-rich parent asteroid containing primitive and fractionated material from the inner solar system. Oxidizing and reducing conditions during SG 009 formation may be connected with a chemical microenvironment and possibly could indicate that G chondrites may have formed by a planetesimal collision resulting in the lack of matrix. © The Meteoritical Society, 2020. We thank M. Weisberg, H. Downes, an anonymous reviewer, and Associate Editor C. Goodrich, for their thoughtful reviews which helped to improve this paper. The authors thank Sasha Krot for very fruitful discussions. This work was supported by the Russian Fond of Basic Research no. 20-05-00117A, by Klaus Tschira Stiftung gGmbH, by the NASA Emerging Worlds program (80NSSC18K0595, MH), and we thank the National High Magnetic Field Laboratory, which is supported by National Science Foundation Cooperative Agreement No. DMR-1644779* and the State of Florida. This work was also supported?by the Project No. FEUZ-2020-0059 of the Ministry of Science and Higher Education of the Russian Federation. This study was a partial contribution to research theme no. 0137-2019-0002.

Published
2020

42. First Identification of Indigenous Organic Matter Alongside Water in Itokawa Particle Returned by the Hayabusa Mission

Author

Chan, Q. H. S., Brunetto, R., Kebukawa, Y., Noguchi, T., Stephant, A., Franchi, I. A., Zhao, X., Johnson, D., Starkey, N. A., Anand, M., Russell, S. S., Schofield, P., Price, M. C., McDermott, K. H., BRADLEY, R., Gilmour, J. D., Lyon, I., Withers, P. J., Lee, M., Sano, Y., Grady, M. M., Institut d'astrophysique spatiale (IAS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), and Brunetto, Rosario

Subjects
[SDU] Sciences of the Universe [physics], [SDU]Sciences of the Universe [physics]
Abstract

International audience; The Itokawa particle "Amazon" contains indigenous organic and structural water.

Published
2020

43. Three Isotopes of Oxygen in Lunar Samples - The Same as Earth or Different?

Author

Pillinger, C. T, Greenwood, R. C, Johnson, D, Gibson, E. K, Miller, M. F, and Franchi, I. A

Subjects
Lunar And Planetary Science And Exploration
Abstract

One of the most important measurements that can be made for any extraterrestrial sample is determination of the relative abundance of O-16, O-17 and O-18. To make the comparison, investigators report their results as delta (δ) values compared to terrestrial delta O-17 vs delta O-18 for a suite of specimens because for any given reservoir, i.e. a planetary parent body such as the Earth or Mars, the numbers should define a line of gradient approximately one half. Different bodies should be identified from their delta O-17 which has traditionally been defined by the equation delta O-17 = delta O-17 - (a constant, ca. 0.52) × delta O-18.

Published
2014

44. Oxygen Isotope Evidence for the Relationship between CM and CO Chondrites: Could they Both Coexist on a Single Asteroid

Author

Greenwood, R. C, Howard, K. T, Franchi, I. A, Zolensky, M. E, Buchanan, P. C, and Gibson, J. M

Subjects
Lunar And Planetary Science And Exploration
Abstract

Water played a critical role in the early evolution of asteroids and planets, as well as being an essential ingredient for life on Earth. However, despite its importance, the source of water in the inner solar system remains controversial. Delivery of water to Earth via comets is inconsistent with their relatively elevated D/H ratios, whereas carbonaceous chondrites (CCs) have more terrestrial-like D/H ratios [1]. Of the eight groups into which the CCs are divided, only three (CI, CM, CR) show evidence of extensive aqueous alteration. Of these, the CMs form the single most important group, representing 34% of all CC falls and a similar percentage of finds (Met. Bull. Database). CM material also dominates the population of CC clasts in extraterrestrial samples [2, 3]. The Antarctic micrometeorites population is also dominated by CM and CI-like material and similar particles may have transported water and volatiles to the early Earth [4]. CCs, and CMs in particular, offer the best opportunity for investigating the evolution of water reservoirs in the early solar system. An important aspect of this problem involves identifying the anhydrous silicate component which co-accreted with ice in the CM parent body. A genetic relationship between the essentially anhydrous CO group and the CMs was proposed on the basis of oxygen isotope evidence [5]. However, previous CM whole-rock oxygen isotope data scattered about a line of approximately 0.5 that did not intersect the field of CO chondrites [5]. Here we discuss new oxygen isotope data which provides additional constraints on the relationship between CO and CM chondrites.

Published
2014

45. Mineralogy, petrology, geochemistry, and chronology of the Murrili (H5) meteorite fall: The third recovered fall from the Desert Fireball Network

Author

Anderson, S., primary, Benedix, G. K., additional, Forman, L. V., additional, Daly, L., additional, Greenwood, R. C., additional, Franchi, I. A., additional, Friedrich, J. M., additional, Macke, R., additional, Wiggins, S., additional, Britt, D., additional, Cadogan, J. M., additional, Meier, M. M. M., additional, Maden, C., additional, Busemann, H., additional, Welten, K. C., additional, Caffee, M. W., additional, Jourdan, F., additional, Mayers, C., additional, Kennedy, T., additional, Godel, B., additional, Esteban, L., additional, Merigot, K., additional, Bevan, A. W. R., additional, Bland, P. A., additional, Paxman, J., additional, Towner, M. C., additional, Cupak, M., additional, Sansom, E. K., additional, Howie, R., additional, Devillepoix, H., additional, Jansen‐Sturgeon, T., additional, Stuart, D., additional, and Strangway, D., additional

Published
2021
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47. A New Unusual Bencubbinite (CBa), Sierra Gorda 013 with Unique V-Rich Sulfides

Author

Ivanova, M. A., Ma, C., Lorenz, C. A., Franchi, I. A., and Kononkova, N. N.

Abstract

The metal-rich (>20 vol% Fe,Ni-metal) carbonaceous chondrites include CH chondrites, CB chondrites [1] and the Isheyevo CH/CBb chondrite [2]. The CB chondrites are rare and divided into two subgroups based on their petrologic characteristics: CBa (e.g., Bencubbin, Weatherford, Gujba) and CBb (e.g., Hammadah al Hamra (HH) 237 and Queen Alexandra Range (QUE) 94411/94627) [1]. A recently described chondrite, Quebrada Chimborazo (QC) 001 is similar to CBa but unusual in containing shock melt and high pressure mineral phases [3]. Here we present preliminary results of study of unusual CB chondrite from Chile, Sierra Gorda (SG) 013, and describe V-rich sulfides which have not previously been found in the meteorite material.

Published
2019

48. Coordinated Organic Analyses of Hayabusa Category 3 Carbonaceous Particles

Author

Chan, Q. H. S., Zolensky, M. E., Brunetto, R., Parker, E. T., Dworkin, J. P., Sandt, C., Wright, I. P., Franchi, I. A., NASA Johnson Space Center (JSC), NASA, Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), NASA Goddard Space Flight Center (GSFC), Synchrotron SOLEIL (SSOLEIL), Centre National de la Recherche Scientifique (CNRS), Planetary and Space Sciences [Milton Keynes] (PSS), School of Physical Sciences [Milton Keynes], Faculty of Science, Technology, Engineering and Mathematics [Milton Keynes], The Open University [Milton Keynes] (OU)-The Open University [Milton Keynes] (OU)-Faculty of Science, Technology, Engineering and Mathematics [Milton Keynes], and The Open University [Milton Keynes] (OU)-The Open University [Milton Keynes] (OU)

Subjects
[SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP]
Abstract

International audience; We explore the origins of five Hayabusa category 3 carbonaceous particles via coordinated analyses of their soluble and insoluble organic contents.

Published
2019

49. Evidence for widespread hydrated minerals on asteroid (101955) Bennu

Author

Hamilton, VE, Simon, AA, Christensen, PR, Reuter, DC, Clark, BE, Barucci, MA, Bowles, NE, Boynton, WV, Brucato, JR, Cloutis, EA, Jr, CHC, Hannah, KLD, Emery, JP, Enos, HL, Fornasier, S, Haberle, CW, Hanna, RD, Howell, ES, Kaplan, HH, Keller, LP, Lantz, C, Li, J-Y, Lim, LF, McCoy, TJ, Merlins, F, Nolan, MC, Praet, A, Rozitis, B, Sandford, SA, Schrader, DL, Thomas, CA, Zou, X-D, Lauretta, DS, Highsmith, DE, Small, J, Vokrouhlicky, D, Brown, E, Warren, T, Brunet, C, Chicoine, RA, Desjardins, S, Gaudreau, D, Haltigin, T, Millington-Veloza, S, Rubi, A, Aponte, J, Gorius, N, Lunsford, A, Allen, B, Grindlay, J, Guevel, D, Hoak, D, Hong, J, Bayron, J, Golubov, O, Sanchez, P, Stromberg, J, Hirabayashi, M, Hartzell, CM, Oliver, S, Rascon, M, Harch, A, Joseph, J, Squyres, S, Richardson, D, McGraw, L, Ghent, R, Binzel, RP, Al Asad, MM, Johnson, CL, Philpott, L, Susorney, HCM, Ciceri, F, Hildebrand, AR, Ibrahim, E-M, Breitenfeld, L, Glotch, T, Rogers, AD, Ferrone, S, Campins, H, Fernandez, Y, Chang, W, Cheuvront, A, Trang, D, Tachibana, S, Yurimoto, H, Poggiali, G, Pajola, M, Dotto, E, Epifani, EM, Crombie, MK, Izawa, MRM, De Leon, J, Licandro, J, Garcia, JLR, Clemett, S, Thomas-Keprta, K, Van Wal, S, Yoshikawa, M, Bellerose, J, Bhaskaran, S, Boyles, C, Chesley, SR, Elder, CM, Farnocchia, D, Harbison, A, Kennedy, B, Knight, A, Martinez-Vlasoff, N, Mastrodemos, N, McElrath, T, Owen, W, Park, R, Rush, B, Swanson, L, Takahashi, Y, Velez, D, Yetter, K, Thayer, C, Adam, C, Antreasian, P, Bauman, J, Bryan, C, Carcich, B, Corvin, M, Geeraert, J, Hoffman, J, Leonard, JM, Lessac-Chenen, E, Levine, A, McAdams, J, McCarthy, L, Nelson, D, Page, B, Pelgrift, J, Sahr, E, Stakkestad, K, Stanbridge, D, Wibben, D, Williams, B, Williams, K, Wolff, P, Hayne, P, Kubitschek, D, Deshapriya, JDP, Fulchignoni, M, Hasselmann, P, Merlin, F, Bierhaus, EB, Billett, O, Boggs, A, Buck, B, Carlson-Kelly, S, Cerna, J, Chaffin, K, Church, E, Coltrin, M, Daly, J, Deguzman, A, Dubisher, R, Eckart, D, Ellis, D, Falkenstern, P, Fisher, A, Fisher, ME, Fleming, P, Fortney, K, Francis, S, Freund, S, Gonzales, S, Haas, P, Hasten, A, Hauf, D, Hilbert, A, Howell, D, Jaen, F, Jayakody, N, Jenkins, M, Johnson, K, Lefevre, M, Ma, H, Mario, C, Martin, K, May, C, McGee, M, Miller, B, Miller, C, Miller, G, Mirfakhrai, A, Muhle, E, Norman, C, Olds, R, Parish, C, Ryle, M, Schmitzer, M, Sherman, P, Skeen, M, Susak, M, Sutter, B, Tran, Q, Welch, C, Witherspoon, R, Wood, J, Zareski, J, Arvizu-Jakubicki, M, Asphaug, E, Audi, E, Ballouz, R-L, Bandrowski, R, Becker, KJ, Becker, TL, Bendall, S, Bennett, CA, Bloomenthal, H, Blum, D, Brodbeck, J, Burke, KN, Chojnacki, M, Colpo, A, Contreras, J, Cutts, J, D'Aubigny, CYD, Dean, D, Dellagiustina, DN, Diallo, B, Drinnon, D, Drozd, K, Enos, R, Fellows, C, Ferro, T, Fisher, MR, Fitzgibbon, G, Fitzgibbon, M, Forelli, J, Forrester, T, Galinsky, I, Garcia, R, Gardner, A, Golish, DR, Habib, N, Hamara, D, Hammond, D, Hanley, K, Harshman, K, Hergenrother, CW, Herzog, K, Hill, D, Hoekenga, C, Hooven, S, Huettner, E, Janakus, A, Jones, J, Kareta, TR, Kidd, J, Kingsbury, K, Balram-Knutson, SS, Koelbel, L, Kreiner, J, Lambert, D, Lewin, C, Lovelace, B, Loveridge, M, Lujan, M, Maleszewski, CK, Malhotra, R, Marchese, K, McDonough, E, Mogk, N, Morrison, V, Morton, E, Munoz, R, Nelson, J, Padilla, J, Pennington, R, Polit, A, Ramos, N, Reddy, V, Riehl, M, Rizk, B, Roper, HL, Salazar, S, Schwartz, SR, Selznick, S, Shultz, N, Smith, PH, Stewart, S, Sutton, S, Swindle, T, Tang, YH, Westermann, M, Wolner, CWV, Worden, D, Zega, T, Zeszut, Z, Bjurstrom, A, Bloomquist, L, Dickinson, C, Keates, E, Liang, J, Nifo, V, Taylor, A, Teti, F, Caplinger, M, Bowles, H, Carter, S, Dickenshied, S, Doerres, D, Fisher, T, Hagee, W, Hill, J, Miner, M, Noss, D, Piacentine, N, Smith, M, Toland, A, Wren, P, Bernacki, M, Munoz, DP, Watanabe, S-I, Aqueche, A, Ashman, B, Barker, M, Bartels, A, Berry, K, Bos, B, Burns, R, Calloway, A, Carpenter, R, Castro, N, Cosentino, R, Donaldson, J, Dworkin, JP, Cook, JE, Emr, C, Everett, D, Fennell, D, Fleshman, K, Folta, D, Gallagher, D, Garvin, J, Getzandanner, K, Glavin, D, Hull, S, Hyde, K, Ido, H, Ingegneri, A, Jones, N, Kaotira, P, Liounis, A, Lorentson, C, Lorenz, D, Lyzhoft, J, Mazarico, EM, Mink, R, Moore, W, Moreau, M, Mullen, S, Nagy, J, Neumann, G, Nuth, J, Poland, D, Rhoads, L, Rieger, S, Rowlands, D, Sallitt, D, Scroggins, A, Shaw, G, Swenson, J, Vasudeva, P, Wasser, M, Zellar, R, Grossman, J, Johnston, G, Morris, M, Wendel, J, Burton, A, McNamara, L, Messenger, S, Nakamura-Messenger, K, Nguyen, A, Righter, K, Queen, E, Bellamy, K, Dill, K, Gardner, S, Giuntini, M, Key, B, Kissell, J, Patterson, D, Vaughan, D, Wright, B, Gaskell, RW, Le Corre, L, Molaro, JL, Palmer, EE, Siegler, MA, Tricarico, P, Weirich, JR, Ireland, T, Tait, K, Bland, P, Anwar, S, Bojorquez-Murphy, N, Mehall, G, Rios, K, Franchi, I, Beddingfield, CB, Marshall, J, Brack, DN, French, AS, McMahon, JW, Scheeres, DJ, Jawin, ER, Russell, S, Killgore, M, Bottke, WF, Walsh, KJ, Bandfield, JL, Clark, BC, Chodas, M, Lambert, M, Masterson, RA, Daly, MG, Freemantle, J, Seabrook, JA, Barnouin, OS, Craft, K, Daly, RT, Ernst, C, Espiritu, RC, Holdridge, M, Jones, M, Nair, AH, Nguyen, L, Peachey, J, Perry, ME, Plescia, J, Roberts, JH, Steele, R, Turner, R, Backer, J, Edmundson, K, Mapel, J, Milazzo, M, Sides, S, Manzoni, C, May, B, Delbo, M, Libourel, G, Michel, P, Ryan, A, Thuillet, F, Marty, B, Team, O-R, Southwest Research Institute [Boulder] (SwRI), ASU School of Earth and Space Exploration (SESE), Arizona State University [Tempe] (ASU), NASA Goddard Space Flight Center (GSFC), Ithaca College, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Department of Atmospheric, Oceanic and Planetary Physics [Oxford] (AOPP), University of Oxford, Lunar and Planetary Laboratory [Tucson] (LPL), University of Arizona, INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto Nazionale di Astrofisica (INAF), Department of Geography [Winnipeg], University of Winnipeg, Department of Physics, Rowan University, Glassboro, Rowan University, Department of Earth and Planetary Sciences [Knoxville], The University of Tennessee [Knoxville], Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Department of Geological Sciences, Jackson School of Geosciences, University of Texas at Austin [Austin], The Swiss Light Source (SLS) (SLS-PSI), Paul Scherrer Institute (PSI), NASA Johnson Space Center (JSC), NASA, Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Université Paris-Sud - Paris 11 (UP11), Planetary Science Institute [Tucson] (PSI), Smithsonian Institution, National Museum of Natural History, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), The Open University [Milton Keynes] (OU), NASA Ames Research Center Cooperative for Research in Earth Science in Technology (ARC-CREST), NASA Ames Research Center (ARC), Center for Meteorite Studies [Tempe], Northern Arizona University [Flagstaff], Centre de Mise en Forme des Matériaux (CEMEF), Mines Paris - PSL (École nationale supérieure des mines de Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), University of Oxford [Oxford], Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Paris Sud Orsay, and MINES ParisTech - École nationale supérieure des mines de Paris

Subjects
Mineral hydration, Thermal infrared, 010504 meteorology & atmospheric sciences, Comets and Kuiper belt, Astronomy and Astrophysics, Mineralogy, 01 natural sciences, Article, Asteroids, Astrobiology, [SPI.MAT]Engineering Sciences [physics]/Materials, [SPI]Engineering Sciences [physics], Asteroid, Chondrite, Meteoritics, 0103 physical sciences, Early solar system, Spectral data, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Geology, 0105 earth and related environmental sciences
Abstract

著者人数: 33名ほか (The OSIRIS-REx Team: 所属. 宇宙航空研究開発機構宇宙科学研究所(JAXA)(ISAS): Van wal, S; 吉川, 真; 渡邊, 誠一郎), Number of authors: 33 and The OSIRIS-REx Team (Affiliation. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency(JAXA)(ISAS): Van wal, S; Yoshikawa, Makoto; Watanabe, Sei-icihro), Accepted: 2019-02-12, 資料番号: SA1190036000

Published
2019
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50. The dynamic geophysical environment of (101955) Bennu based on OSIRIS-REx measurements

Author

Scheeres, DJ, McMahon, JW, French, AS, Brack, DN, Chesley, SR, Farnocchia, D, Takahashi, Y, Leonard, JM, Geeraert, J, Page, B, Antreasian, P, Getzandanner, K, Rowlands, D, Mazarico, EM, Small, J, Highsmith, DE, Moreau, M, Emery, JP, Rozitis, B, Hirabayashi, M, Sanchez, P, Van Wal, S, Tricarico, P, Ballouz, R-L, Johnson, CL, Asad, MM, Susorney, HCM, Barnouin, OS, Daly, MG, Seabrook, JA, Gaskell, RW, Palmer, EE, Weirich, JR, Walsh, KJ, Jawin, ER, Bierhaus, EB, Michel, P, Bottke, WF, Nolan, MC, Jr, CHC, Lauretta, DS, Vokrouhlicky, D, Bowles, NE, Brown, E, Hanna, KLD, Warren, T, Brunet, C, Chicoine, RA, Desjardins, S, Gaudreau, D, Haltigin, T, Millington-Veloza, S, Rubi, A, Aponte, J, Gorius, N, Lunsford, A, Allen, B, Grindlay, J, Guevel, D, Hoak, D, Hong, J, Schrader, DL, Bayron, J, Golubov, O, Stromberg, J, Hartzell, CM, Oliver, S, Rascon, M, Harch, A, Joseph, J, Squyres, S, Richardson, D, McGraw, L, Ghent, R, Binzel, RP, Philpott, L, Cloutis, EA, Hanna, RD, Ciceri, F, Hildebrand, AR, Ibrahim, E-M, Breitenfeld, L, Glotch, T, Rogers, AD, Clark, BE, Ferrone, S, Thomas, CA, Campins, H, Fernandez, Y, Chang, W, Cheuvront, A, Trang, D, Tachibana, S, Yurimoto, H, Brucato, JR, Poggiali, G, Pajola, M, Dotto, E, Epifani, EM, Crombie, MK, Lantz, C, Izawa, MRM, De Leon, J, Licandro, J, Garcia, JL, Clemett, S, Thomas-Keprta, K, Yoshikawa, M, Bellerose, J, Bhaskaran, S, Boyles, C, Elder, CM, Harbison, A, Kennedy, B, Knight, A, Martinez-Vlasoff, N, Mastrodemos, N, McElrath, T, Owen, W, Park, R, Rush, B, Swanson, L, Velez, D, Yetter, K, Thayer, C, Adam, C, Bauman, J, Bryan, C, Carcich, B, Corvin, M, Hoffman, J, Lessac-Chenen, E, Levine, A, McAdams, J, McCarthy, L, Nelson, D, Pelgrift, J, Sahr, E, Stakkestad, K, Stanbridge, D, Wibben, D, Williams, B, Williams, K, Wolff, P, Hayne, P, Kubitschek, D, Barucci, MA, Deshapriya, JDP, Fornasier, S, Fulchignoni, M, Hasselmann, P, Merlin, F, Praet, A, Billett, O, Boggs, A, Buck, B, Carlson-Kelly, S, Cerna, J, Chaffin, K, Church, E, Coltrin, 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Berry, K, Bos, B, Burns, R, Calloway, A, Carpenter, R, Castro, N, Cosentino, R, Donaldson, J, Dworkin, JP, Cook, JE, Emr, C, Everett, D, Fennell, D, Fleshman, K, Folta, D, Gallagher, D, Garvin, J, Glavin, D, Hull, S, Hyde, K, Ido, H, Ingegneri, A, Jones, N, Kaotira, P, Lim, LF, Liounis, A, Lorentson, C, Lorenz, D, Lyzhoft, J, Mink, R, Moore, W, Mullen, S, Nagy, J, Neumann, G, Nuth, J, Poland, D, Reuter, DC, Rhoads, L, Rieger, S, Sallitt, D, Scroggins, A, Shaw, G, Simon, AA, Swenson, J, Vasudeva, P, Wasser, M, Zellar, R, Grossman, J, Johnston, G, Morris, M, Wendel, J, Burton, A, Keller, LP, McNamara, L, Messenger, S, Nakamura-Messenger, K, Nguyen, A, Righter, K, Queen, E, Bellamy, K, Dill, K, Gardner, S, Giuntini, M, Key, B, Kissell, J, Patterson, D, Vaughan, D, Wright, B, Le Corre, L, Li, J-Y, Molaro, JL, Siegler, MA, Zou, X-D, Ireland, T, Tait, K, Bland, P, Anwar, S, Bojorquez-Murphy, N, Christensen, PR, Haberle, CW, Mehall, G, Rios, K, Franchi, I, Beddingfield, CB, Marshall, J, McCoy, TJ, Russell, S, Killgore, M, Hamilton, VE, Kaplan, HH, Bandfield, JL, Clark, BC, Chodas, M, Lambert, M, Masterson, RA, Freemantle, J, Craft, K, Daly, RT, Ernst, C, Espiritu, RC, Holdridge, M, Jones, M, Nair, AH, Nguyen, L, Peachey, J, Perry, ME, Plescia, J, Roberts, JH, Steele, R, Turner, R, Backer, J, Edmundson, K, Mapel, J, Milazzo, M, Sides, S, Manzoni, C, May, B, Delbo', M, Libourel, G, Ryan, A, Thuillet, F, Marty, B, Team, The OSIRIS-REx, USDA Agricultural Research Service [Maricopa, AZ] (USDA), United States Department of Agriculture (USDA), Dipartimento di Matematica, University of Pisa - Università di Pisa, Department of Geophysics [Sendai], Tohoku University [Sendai], KinetX Aerospace Inc., Institut de Recherche Interdisciplinaire sur les enjeux Sociaux - sciences sociales, politique, santé (IRIS), Université Paris 13 (UP13)-École des hautes études en sciences sociales (EHESS)-Université Sorbonne Paris Cité (USPC)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS)-Université Paris sciences et lettres (PSL), Institut des Matériaux, de Microélectronique et des Nanosciences de Provence (IM2NP), Aix Marseille Université (AMU)-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), The Open University [Milton Keynes] (OU), National Institute of Polar Research [Tokyo] (NiPR), IHU-LIRYC, Université Bordeaux Segalen - Bordeaux 2-CHU Bordeaux [Bordeaux], Planetary Science Institute [Tucson] (PSI), Institute of Northern Engineering, 455 Duckering Bldg, Centre de Mise en Forme des Matériaux (CEMEF), Mines Paris - PSL (École nationale supérieure des mines de Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), ANR-15-IDEX-0001,UCA JEDI,Idex UCA JEDI(2015), Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Université Sorbonne Paris Cité (USPC)-École des hautes études en sciences sociales (EHESS)-Université Paris 13 (UP13), Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS)-Aix Marseille Université (AMU), and MINES ParisTech - École nationale supérieure des mines de Paris

Subjects
010504 meteorology & atmospheric sciences, biology, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Physics, Spin rate, Equator, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Astronomy and Astrophysics, Geophysics, Astronomy and planetary science, biology.organism_classification, 01 natural sciences, Article, [SPI]Engineering Sciences [physics], Engineering, Asteroid, 0103 physical sciences, Roche lobe, Osiris, 010303 astronomy & astrophysics, Geology, 0105 earth and related environmental sciences
Abstract

著者人数: 41名ほか (The OSIRIS-REx Team: 所属. 宇宙航空研究開発機構宇宙科学研究所 (JAXA)(ISAS): Van wal, Stefaan; 吉川, 真; 渡邊, 誠一郎), Number of authors: 41 and The OSIRIS-REx Team (Affiliation. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA)(ISAS): Yoshikawa, Makoto; Watanabe, Sei-ichiro), Accepted: 2019-02-11, 資料番号: SA1180379000

Published
2019
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