Dante S Lauretta

Interests

Research

AsteroidsCometsMeteoritesOrigins of planetary systemsSpacecraft missions

Teaching

CosmochemistryPlanetary ScienceSpacecraft Mission Design

Courses

Scholarly Contributions

Books

• Apai, D., &  Lauretta, D. (2014). Protoplanetary Dust. Cambridge, UK: Cambridge University Press.

Chapters

• Lauretta, D. S., Enons, H. L., Polit, A. T., Roper, H. L., & Wolner, C. W. (2021). Chapter 8 - OSIRIS-REx at Bennu: Overcoming challenges to collect a sample of the early Solar System. In Sample Return Missions: The Last Frontier of Solar System Exploration. Editor: Andrea Longobardo. Elsevier(pp 163-194).
• Lauretta, D. S., Enos, H. L., Polit, A. T., Roper, H. L., & Wolner, C. W. (2021). OSIRIS-REx at Bennu: Overcoming challenges to collect a sample of the early Solar System. In Sample return missions(pp 163--194). Elsevier.

Journals/Publications

• Aponte, J. C., S{\'eguin}, F., Siguelnitzky, A. J., Dworkin, J. P., Elsila, J. E., Glavin, D. P., Connolly, H. C., & Lauretta, D. S. (2024). Molecular distribution and $^13$C isotope composition of volatile organic compounds in the Murchison and Sutter's Mill carbonaceous chondrites. \maps, 59(2), 286-300.
• Ballouz, R., Ryan, A. J., Barnouin, O. S., Macke, R. J., Connolly, H. C., & Lauretta, D. S. (2024). Insights Into Regolith Development on Rubble-Pile Asteroid (101955) Bennu from Remote Sensing and Sample Analysis. Geological Society of America Abstracts, 56, 403895.
• Cody, G. D., Alexander, C., Foustoukos, D. I., Busemann, H., Eckley, S., Burton, A. S., Berger, E. L., Nuevo, M., Sandford, S. A., Glavin, D. P., Dworkin, J. P., Connolly, H. C., & Lauretta, D. S. (2024). The nature of insoluble organic matter in Sutter's Mill and Murchison carbonaceous chondrites: Testing the effect of x-ray computed tomography and exploring parent body organic molecular evolution. \maps, 59(1), 3-22.
• Fulford, R. E., Golish, D. R., Lauretta, D. S., DellaGiustina, D. N., Meyer, S., Lunning, N., Snead, C., Righter, K., Dworkin, J. P., Bennett, C. A., Connolly, H. C., Johnson, T., Polit, A. T., Haennecour, P., & Ryan, A. J. (2024). QRIS: A Quantitative Reflectance Imaging System for the Pristine Sample of Asteroid Bennu. arXiv e-prints, arXiv:2402.18674.
• Glavin, D. P., Eckley, S. A., Aponte, J. C., Berger, E. L., Burton, A. S., Dworkin, J. P., Elsila, J. E., Ferguson, F. T., Furukawa, Y., Graham, H. V., Koga, T., Liss, M., MCLain, H. L., Naraoka, H., Oba, Y., Parker, E. T., Righter, K., Schmitt-Kopplin, P., Simkus, D. N., , Takano, Y., et al. (2024). Investigating the impact of x-ray computed tomography imaging on soluble organic matter in the Murchison meteorite: Implications for Bennu sample analyses. \maps, 59(1), 105-133.
• Guigoz, V., Seret, A., Portail, M., Ferri{\`ere}, L., Libourel, G., Connolly, H. C., & Lauretta, D. S. (2024). High-resolution cathodoluminescence of calcites from the Cold Bokkeveld chondrite: New insights on carbonatation processes in CM parent bodies. \maps, 59(9), 2432-2452.
• Ishimaru, K., & Lauretta, D. (2024). Analysis of layered boulders on asteroid (101955) Bennu and their implications for fluid flow on the parent body. \maps, 59(1), 193-210.
• Jenniskens, P., Estrada, P. R., Pilorz, S., Gural, P. S., Samuels, D., Rau, S., Abbott, T. M., Albers, J., Austin, S., Avner, D., Baggaley, J. W., Beck, T., Blomquist, S., Boyukata, M., Breukers, M., Cooney, W., Cooper, T., De, C. M., Devillepoix, H., , Egland, E., et al. (2024). Properties of outer solar system pebbles during planetesimal formation from meteor observations. \icarus, 423, 116229.
• Jenniskens, P., Pilorz, S., Gural, P. S., Samuels, D., Rau, S., Abbott, T. M., Albers, J., Austin, S., Avner, D., Baggaley, J. W., Beck, T., Blomquist, S., Boyukata, M., Breukers, M., Cooney, W., Cooper, T., De, C. M., Devillepoix, H., Egland, E., , Fahl, E., et al. (2024). Lifetime of cm-sized zodiacal dust from the physical and dynamical evolution of meteoroid streams. \icarus, 415, 116034.
• Krot, A. N., Nagashima, K., Ivanova, M. A., Lauretta, D., Libourel, G., Johnson, B. C., Brenker, F. E., Hoffman, V., & Bizzarro, M. (2024). Mineralogy, petrology, and oxygen isotopic compositions of chondritic and achondritic lithologies in the anomalous CB carbonaceous chondrites Sierra Gorda 013 and Fountain Hills. \maps, 59(4), 754-777.
• Lauretta, D. S., Connolly, H. C., Aebersold, J. E., Alexander, C., Ballouz, R., Barnes, J. J., Bates, H. C., Bennett, C. A., Blanche, L., Blumenfeld, E. H., Clemett, S. J., Cody, G. D., DellaGiustina, D. N., Dworkin, J. P., Eckley, S. A., Foustoukos, D. I., Franchi, I. A., Glavin, D. P., Greenwood, R. C., , Haenecour, P., et al. (2024). Asteroid (101955) Bennu in the laboratory: Properties of the sample collected by OSIRIS-REx. \maps, 59(9), 2453-2486.
• Lauretta, D. S., Daly, M. G., Christensen, P. R., Hamilton, V. E., Edmundson, K. L., Bennett, C. A., Haberle, C. W., Walsh, K. J., Golish, D. R., Jawin, E. R., Siegler, M., Elder, C. M., Delbo, M., Bernacki, M., Nolan, M. C., Emery, J. P., Becker, K. J., Pino, M. D., Rozitis, B., & Ryan, A. J. (2024). Rocks with Extremely Low Thermal Inertia at the OSIRIS-REx Sample Site on Asteroid Bennu. Planetary Science Journal, 5(4), 92.
• Nguyen, A., Clemett, S., Thomas-Keprta, K. .., Alexander, C. O., Glavin, D., Dworkin, J., Connolly, H., & Lauretta, D. (2024). Micro- and nanoscale studies of insoluble organic matter and C-rich presolar grains in Murchison and Sutter's Mill in preparation for Bennu sample analysis. \maps, 59(10), 2831-2850.
• Palmer, E. E., Weirich, J. R., Gaskell, R. W., Lambert, D., Campbell, T., Drozd, K., Barnouin, O. S., Daly, M. G., Getzandanner, K., Kidd, J. N., Adam, C. D., & Lauretta, D. S. (2024). Sensitivity Testing of Stereophotoclinometry for the OSIRIS-REx Mission. I. The Accuracy and Errors of Digital Terrain Modeling. \psj, 5(2), 46.
• Palmer, E. E., Weirich, J. R., Gaskell, R. W., Lambert, D., Campbell, T., Drozd, K., Barnouin, O. S., Daly, M. G., Getzandanner, K., Kidd, J. N., Adam, C. D., & Lauretta, D. S. (2024). Sensitivity Testing of Stereophotoclinometry for the OSIRIS-REx Mission. II. Effective Observation Geometry for Digital Terrain Modeling. \psj, 5(2), 47.
• Ryan, A. J., Rozitis, B., Pino, M. D., Becker, K. J., Emery, J. P., Nolan, M. C., Bernacki, M., Delbo, M., Elder, C. M., Siegler, M., Jawin, E. R., Golish, D. R., Walsh, K. J., Haberle, C. W., Bennett, C. A., Edmundson, K. L., Hamilton, V. E., Christensen, P. R., Daly, M. G., & Lauretta, D. S. (2024). Rocks with Extremely Low Thermal Inertia at the OSIRIS-REx Sample Site on Asteroid Bennu. \psj, 5(4), 92.
• Saxey, D. W., Fougerouse, D., Dimitriou, D., Barnes, J. J., Rickard, W. D., Timms, N. E., Jourdan, F., Reddy, S. M., Bland, P. A., Ireland, T. R., Nguyen, A., Connolly, H. C., & Lauretta, D. S. (2024). Geochemical Quantification of Olivine Minerals by Atom Probe Tomography. Microscopy and Microanalysis, 30, ozae044.032.
• Tang, Y., Lauretta, D., Ballouz, R. -., DellaGiustina, D., Polit, A., Westermann, M., Bennett, C., Becker, K., Walsh, K., & Golish, D. (2024). Characterization and implications of a mass movement site in Bennu's Bralgah Crater. \icarus, 415, 116056.
• Walsh, K. J., Lauretta, D. S., Ballouz, R. -., Sugita, S., Bottke, W., Schwartz, S., Avdellidou, C., Nolan, M. C., Connolly, H., Morota, T., Delbo, M., Michel, P., DellaGiustina, D., McCoy, T., Jawin, E., Jawin, E., McCoy, T., Della-Giustina, D. N., Michel, P., , Delbo, M., et al. (2024). Numerical simulations suggest asteroids (101955) Bennu and (162173) Ryugu are likely second or later generation rubble piles.. Nature Communications, 15, 5653.
• Yumoto, K., Tatsumi, E., Kouyama, T., Golish, D., Cho, Y., Morota, T., Kameda, S., Sato, H., Rizk, B., DellaGiustina, D., Yokota, Y., Suzuki, H., Le{\'on}, J., Campins, H., Licandro, J., Popescu, M., Rizos, J., Honda, R., Yamada, M., , Sakatani, N., et al. (2024). Comparison of optical spectra between asteroids Ryugu and Bennu: I. Cross calibration between Hayabusa2/ONC-T and OSIRIS-REx/MapCam. \icarus, 417, 116122.
• Yumoto, K., Tatsumi, E., Kouyama, T., Golish, D., Cho, Y., Morota, T., Kameda, S., Sato, H., Rizk, B., DellaGiustina, D., Yokota, Y., Suzuki, H., Le{\'on}, J., Campins, H., Licandro, J., Popescu, M., Rizos, J., Honda, R., Yamada, M., , Sakatani, N., et al. (2024). Comparison of optical spectra between asteroids Ryugu and Bennu: II. High-precision analysis for space weathering trends. \icarus, 420, 116204.
• Adam, C. D., McCarthy, L. K., Leonard, J. M., Gaskell, R., Antreasian, P. G., Liounis, A. J., Getzandanner, K., Moreau, M. C., Palmer, E. E., Weirich, J., Barnouin, O. S., Geeraert, J. L., Sahr, E. M., Ashman, B., Nelson, D. S., Pelgrift, J. Y., Lessac-Chenen, E. J., Wibben, D., Williams, B. G., , Daly, M. G., et al. (2023). Stereophotoclinometry for OSIRIS-REx Spacecraft Navigation. \psj, 4(9), 167.
• Bierhaus, E., Rossmann, F., Johnson, C., Daly, R., Golish, D., Nolau, J., Allen, A., Campins, H., Pajola, M., Rizk, B., D'Aubigny, C., DellaGiustina, D., Cloutis, E., Trang, D., & Lauretta, D. (2023). A subsurface layer on asteroid (101955) Bennu and implications for rubble pile asteroid evolution. \icarus, 406, 115736.
• Clark, B., Sen, A., Zou, X. -., DellaGiustina, D., Sugita, S., Sakatani, N., Thompson, M., Trang, D., Tatsumi, E., Barucci, M., Barker, M., Campins, H., Morota, T., Lantz, C., Hendrix, A., Vilas, F., Keller, L., Hamilton, V., Kitazato, K., , Sasaki, S., et al. (2023). Overview of the search for signs of space weathering on the low-albedo asteroid (101955) Bennu. \icarus, 400, 115563.
• DellaGiustina, D. N., Nolan, M. C., Polit, A. T., Moreau, M. C., Golish, D. R., Simon, A. A., Adam, C. D., Antreasian, P. G., Ballouz, R., Barnouin, O. S., Becker, K. J., Bennett, C. A., Binzel, R. P., Bos, B. J., Burns, R., Castro, N., Chesley, S. R., Christensen, P. R., Crombie, M. K., , Daly, M. G., et al. (2023). OSIRIS-APEX: An OSIRIS-REx Extended Mission to Asteroid Apophis. \psj, 4(10), 198.
• Gaskell, R., Barnouin, O., Daly, M., Palmer, E., Weirich, J., Ernst, C., Daly, R., & Lauretta, D. (2023). Stereophotoclinometry on the OSIRIS-REx Mission: Mathematics and Methods. \psj, 4(4), 63.
• Gross, J., & Lauretta, D. (2023). Nier Prize for Dr. Jessica Barnes. \maps, 58(8), 1169-1170.
• Jenniskens, P., Lauretta, D. S., Koelbel, L. R., Towner, M. C., Bland, P., Heathcote, S., Abbott, T. M., Jehin, E., Hanke, T., Fahl, E., & others, . (2023). An observing campaign to search for meteoroids of Bennu at Earth. Icarus, 394, 115403.
• Lauretta}, D. S., Connolly Jr, ., Grossman, J. N., Polit, A. T., & Team, {. (2023). OSIRIS-REx Sample Analysis Plan -- Revision 3.0. arXiv e-prints, arXiv:2308.11794.
• Leonard, J. M., Geeraert, J. L., McCarthy, L. K., Adam, C. D., Antreasian, P. G., Barnouin, O. S., Daly, M. G., Seabrook, J. A., & Lauretta, D. S. (2023). Post-flight Evaluation of Lidar-based Digital Terrain Models for OSIRIS-REx Navigation at Bennu. \psj, 4(7), 131.
• Marshall, J., Beddingfield, C., Fenton, L., Walsh, K., & Lauretta, D. (2023). Regolith migration on asteroid 101955 Bennu inferred from boulder alignment. \planss, 229, 105659.
• Nakamura, T., Matsumoto, M., Amano, K., Enokido, Y., Zolensky, M., Mikouchi, T., Genda, H., Tanaka, S., Zolotov, M., Kurosawa, K., Wakita, S., Hyodo, R., Nagano, H., Nakashima, D., Takahashi, Y., Fujioka, Y., Kikuiri, M., Kagawa, E., Matsuoka, M., , Brearley, A., et al. (2023). Formation and evolution of carbonaceous asteroid Ryugu: Direct evidence from returned samples. Science, 379(6634), abn8671.
• Naraoka, H., Takano, Y., Dworkin, J. P., Oba, Y., Hamase, K., Furusho, A., Ogawa, N. O., Hashiguchi, M., Fukushima, K., Aoki, D., Schmitt-Kopplin, P., Aponte, J. C., Parker, E. T., Glavin, D. P., McLain, H. L., Elsila, J. E., Graham, H. V., Eiler, J. M., Orthous-Daunay, F., , Wolters, C., et al. (2023). Soluble organic molecules in samples of the carbonaceous asteroid (162173) Ryugu. Science, 379(6634), abn9033.
• Noguchi, T., Matsumoto, T., Miyake, A., Igami, Y., Haruta, M., Saito, H., Hata, S., Seto, Y., Miyahara, M., Tomioka, N., Ishii, H. A., Bradley, J. P., Ohtaki, K. K., Dobric{\v{a}}, E., Leroux, H., Le, G. C., Jacob, D., Pe{\~na}, F., Laforet, S., , Marinova, M., et al. (2023). A dehydrated space-weathered skin cloaking the hydrated interior of Ryugu. Nature Astronomy, 7, 170-181.
• Okazaki, R., Marty, B., Busemann, H., Hashizume, K. o., Gilmour, J. D., Meshik, A., Yada, T., Kitajima, F., Broadley, M. W., Byrne, D., F{\"uri}, E., Riebe, M. E., Krietsch, D., Maden, C., Ishida, A., Clay, P., Crowther, S. A., Fawcett, L., Lawton, T., , Pravdivtseva, O., et al. (2023). Noble gases and nitrogen in samples of asteroid Ryugu record its volatile sources and recent surface evolution. Science, 379(6634), abo0431.
• Righter, K., Lunning, N., Nakamura-Messenger, K. .., Snead, C., MCQuillan, J., Calaway, M., Allums, K., Rodriguez, M., Funk, R., Harrington, R., Connelly, W., Cowden, T., Dworkin, J., Lorentson, C., Sandford, S., Bierhaus, E., Freund, S., Connolly, H., & Lauretta, D. (2023). Curation planning and facilities for asteroid Bennu samples returned by the OSIRIS-REx mission. \maps, 58(4), 572-590.
• Tang, Y., Lauretta, D. S., Ballouz, R., DellaGiustina, D. N., Bennett, C. A., Walsh, K. J., & Golish, D. R. (2023). Simulating impact-induced shaking as a triggering mechanism for mass movements on Bennu. Icarus, 115463.
• Yabuta, H., Cody, G. D., Engrand, C., Kebukawa, Y., De, G. B., Bonal, L., Remusat, L., Stroud, R., Quirico, E., Nittler, L., Hashiguchi, M., Komatsu, M., Okumura, T., Mathurin, J., Dartois, E., Duprat, J., Takahashi, Y., Takeichi, Y., Kilcoyne, D., , Yamashita, S., et al. (2023). Macromolecular organic matter in samples of the asteroid (162173) Ryugu. Science, 379(6634), abn9057.
• Yokoyama, T., Nagashima, K., Nakai, I., Young, E. D., Abe, Y., Al{\'eon}, J., Alexander, C., Amari, S., Amelin, Y., Bajo, K., Bizzarro, M., Bouvier, A., Carlson, R. W., Chaussidon, M., Choi, B., Dauphas, N., Davis, A. M., Di, R. T., Fujiya, W., , Fukai, R., et al. (2023). Samples returned from the asteroid Ryugu are similar to Ivuna-type carbonaceous meteorites. Science, 379(6634), abn7850.
• Yumoto, K., Tatsumi, E., Kouyama, T., Golish, D., Kameda, S., Sato, H., Rizk, B., DellaGiustina, D., Yokota, Y., Suzuki, H., Le{\'on}, J., Campins, H., Licandro, J., Popescu, M., Rizos, J., Honda, R., Yamada, M., Morota, T., Sakatani, N., , Cho, Y., et al. (2023). Cross calibration between Hayabusa2/ONC-T and OSIRIS-REx/MapCam for comparative analyses between asteroids Ryugu and Bennu. arXiv e-prints, arXiv:2306.13321.
• Barnouin, O. S., Daly, M. G., Seabrook, J. A., Zhang, Y., Thuillet, F., Michel, P., Roberts, J. H., Daly, R. T., Perry, M. E., Susorney, H., & others, . (2022). The formation of terraces on asteroid (101955) Bennu. Journal of Geophysical Research: Planets, 127(4), e2021JE006927.
• Barnouin, O. S., Jawin, E. R., Daly, R. T., Ballouz, R., Daly, M. G., Seabrook, J. A., Michel, P., Zhang, Y., Johnson, C. L., Walsh, K. J., & others, . (2022). Geologic context of the OSIRIS-REx sample site from high-resolution topography and imaging. The Planetary Science Journal, 3(4), 75.
• Bierhaus, E. B., Trang, D., Daly, R. T., Bennett, C. A., Barnouin, O. S., Walsh, K. J., Ballouz, R., Bottke, W. F., Burke, K. N., Perry, M. E., & others, . (2022). Crater population on asteroid (101955) Bennu indicates impact armouring and a young surface. Nature Geoscience, 15(6), 440--446.
• Delbo, M., Walsh, K. J., Matonti, C., Wilkerson, J., Pajola, M., Al, A., Avdellidou, C., Ballouz, R., Bennett, C. A., Connolly Jr, ,. H., & others, . (2022). Alignment of fractures on Bennu’s boulders indicative of rapid asteroid surface evolution. Nature Geoscience, 15(6), 453--457.
• Golish, D. R., Simon, A. A., Reuter, D. C., Ferrone, S., Clark, B. E., Li, J., DellaGiustina, D. N., Drouet, d. C., Rizk, B., & Lauretta, D. S. (2022). Cross-Instrument Comparison of MapCam and OVIRS on OSIRIS-REx. Space Science Reviews, 218(2), 5.
• Jawin, E. R., McCoy, T. J., Walsh, K. J., Connolly Jr, ,., Ballouz, R., Ryan, A. J., Kaplan, H. H., Pajola, M., Hamilton, V. E., Barnouin, O. S., & others, . (2022). Global geologic map of asteroid (101955) Bennu indicates heterogeneous resurfacing in the past 500,000 years. Icarus, 381, 114992.
• Lauretta, D. S., Adam, C. D., Allen, A. J., Ballouz, R., Barnouin, O. S., Becker, K. J., Becker, T., Bennett, C. A., Bierhaus, E. B., Bos, B. J., & others, . (2022). Spacecraft sample collection and subsurface excavation of asteroid (101955) Bennu. Science, 377(6603), 285--291.
• Mario, C. E., Miller, C. J., Norman, C. D., Palmer, E. E., Weirich, J., Barnouin, O. S., Daly, M. G., Seabrook, J. A., Lorenz, D. A., Olds, R. D., & others, . (2022). Ground Testing of Digital Terrain Models to Prepare for OSIRIS-REx Autonomous Vision Navigation Using Natural Feature Tracking. The Planetary Science Journal, 3(5), 104.
• Michel, P., K"uppers, M., Bagatin, A. C., Carry, B., Charnoz, S., De, L. J., Fitzsimmons, A., Gordo, P., Green, S. F., H'erique, A., & others, . (2022). The ESA Hera mission: detailed characterization of the DART impact outcome and of the binary asteroid (65803) Didymos. The Planetary Science Journal, 3(7), 160.
• Nakamura, T., Matsumoto, M., Amano, K., Enokido, Y., Zolensky, M. E., Mikouchi, T., Genda, H., Tanaka, S., Zolotov, M. Y., Kurosawa, K., & others, . (2022). Formation and evolution of carbonaceous asteroid Ryugu: Direct evidence from returned samples. Science, eabn8671.
• Noguchi, T., Matsumoto, T., Miyake, A., Igami, Y., Haruta, M., Saito, H., Hata, S., Seto, Y., Miyahara, M., Tomioka, N., & others, . (2022). A dehydrated space-weathered skin cloaking the hydrated interior of Ryugu. Nature Astronomy, 1--12.
• Norman, C. D., Miller, C. J., Olds, R. D., Mario, C. E., Palmer, E. E., Barnouin, O. S., Daly, M. G., Weirich JR, ., Seabrook, J. A., Bennett, C. A., & others, . (2022). Autonomous Navigation Performance Using Natural Feature Tracking during the OSIRIS-REx Touch-and-Go Sample Collection Event. The Planetary Science Journal, 3(5), 101.
• Okazaki, R., Marty, B., Busemann, H., Hashizume, K. o., Gilmour, J. D., Meshik, A., Yada, T., Kitajima, F., Broadley, M. W., Byrne, D., & others, . (2022). Noble gases and nitrogen in samples of asteroid Ryugu record its volatile sources and recent surface evolution. Science, eabo0431.
• Okazaki, R., Miura, Y. N., Takano, Y., Sawada, H., Sakamoto, K., Yada, T., Yamada, K., Kawagucci, S., Matsui, Y., Hashizume, K. o., & others, . (2022). First asteroid gas sample delivered by the Hayabusa2 mission: A treasure box from Ryugu. Science Advances, 8(46), eabo7239.
• Olds, R. D., Miller, C. J., Norman, C. D., Mario, C. E., Berry, K., Palmer, E., Barnouin, O. S., Daly, M. G., Weirich JR, ., Seabrook, J. A., & others, . (2022). The use of digital terrain models for natural feature tracking at asteroid Bennu. The Planetary Science Journal, 3(5), 100.
• Palmer, E. E., Gaskell, R., Daly, M. G., Barnouin, O. S., Adam, C. D., & Lauretta, D. S. (2022). Practical stereophotoclinometry for modeling shape and topography on planetary missions. The Planetary Science Journal, 3(5), 102.
• Perry, M. E., Barnouin, O. S., Daly, R. T., Bierhaus, E. B., Ballouz, R., Walsh, K. J., Daly, M. G., DellaGiustina, D. N., Nolan, M. C., Emery, J. P., & others, . (2022). Low surface strength of the asteroid Bennu inferred from impact ejecta deposit. Nature Geoscience, 15(6), 447--452.
• Rozitis, B., Ryan, A. J., Emery, J. P., Nolan, M. C., Green, S. F., Christensen, P. R., Hamilton, V. E., Daly, M. G., Barnouin, O. S., & Lauretta, D. S. (2022). High-Resolution Thermophysical Analysis of the OSIRIS-REx Sample Site and Three Other Regions of Interest on Bennu. Journal of Geophysical Research: Planets, 127(6), e2021JE007153.
• Seabrook, J. A., Daly, M. G., Barnouin, O. S., Palmer, E. E., Gaskell, R. W., Nair, H., & Lauretta, D. S. (2022). Building a High-resolution Digital Terrain Model of Bennu from Laser Altimetry Data. The Planetary Science Journal, 3(12), 265.
• Tachibana, S., Sawada, H., Okazaki, R., Takano, Y., Sakamoto, K., Miura, Y. N., Okamoto, C., Yano, H., Yamanouchi, S., Michel, P., & others, . (2022). Pebbles and sand on asteroid (162173) Ryugu: In situ observation and particles returned to Earth. Science, 375(6584), 1011--1016.
• Walsh, K. J., Ballouz, R., Jawin, E. R., Avdellidou, C., Barnouin, O. S., Bennett, C. A., Bierhaus, E. B., Bos, B. J., Cambioni, S., Connolly Jr, ,. H., & others, . (2022). Near-zero cohesion and loose packing of Bennu’s near subsurface revealed by spacecraft contact. Science advances, 8(27), eabm6229.
• Walsh, K. J., Bierhaus, E. B., Lauretta, D. S., Nolan, M. C., Ballouz, R., Bennett, C. A., Jawin, E. R., Barnouin, O. S., Berry, K., Burke, K. N., & others, . (2022). Assessing the sampleability of Bennu’s surface for the OSIRIS-REx asteroid sample return mission. Space Science Reviews, 218(4), 20.
• Weirich, J., Palmer, E. E., Daly, M. G., Barnouin, O. S., Getzandanner, K., Kidd, J. N., Adam, C. D., Gaskell, R., & Lauretta, D. S. (2022). Quality Assessment of Stereophotoclinometry as a Shape Modeling Method Using a Synthetic Asteroid. The Planetary Science Journal, 3(5), 103.
• Yokoyama, T., Nagashima, K., Nakai, I., Young, E. D., Abe, Y., Al'eon, J., Alexander, C., Amari, S., Amelin, Y., Bajo, K., & others, . (2022). Samples returned from the asteroid Ryugu are similar to Ivuna-type carbonaceous meteorites. Science, eabn7850.
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  Abstract: Near-Earth Asteroids (NEAs) have garnered ever increasing attention over the past few years due to the insights they offer into Solar System formation and evolution, the potential hazard they pose, and their accessibility for both robotic and human spaceflight missions. Among the NEAs, carbonaceous asteroids hold particular interest because they may contain clues to how the Earth got its supplies of water and organic materials, and because none has yet been studied in detail by spacecraft. (101955) Bennu is special among NEAs in that it will not only be visited by a spacecraft, but the OSIRIS-REx mission will also return a sample of Bennu's regolith to Earth for detailed laboratory study. This paper presents analysis of thermal infrared photometry and spectroscopy that test the hypotheses that Bennu is carbonaceous and that its surface is covered in fine-grained (sub-cm) regolith. The Spitzer Space Telescope observed Bennu in 2007, using the Infrared Spectrograph (IRS) to obtain spectra over the wavelength range 5.2-38μm and images at 16 and 22μm at 10 different longitudes, as well as the Infrared Array Camera (IRAC) to image Bennu at 3.6, 4.5, 5.8, and 8.0μm, also at 10 different longitudes. Thermophysical analysis, assuming a spherical body with the known rotation period and spin-pole orientation, returns an effective diameter of 484±10m, in agreement with the effective diameter calculated from the radar shape model at the orientation of the Spitzer observations (492±20m, Nolan, M.C., Magri, C., Howell, E.S., Benner, L.A.M., Giorgini, J.D., Hergenrother, C.W., Hudson, R.S., Lauretta, D.S., Margo, J.-L., Ostro, S.J., Scheeres, D.J. [2013]. Icarus 226, 629-640) and a visible geometric albedo of 0.046±0.005 (using Hv=20.51, Hergenrother, C.W. et al. [2013]. Icarus 226, 663-670). Including the radar shape model in the thermal analysis, and taking surface roughness into account, yields a disk-averaged thermal inertia of 310±70Jm-2K-1s-1/2, which is significantly lower than several other NEAs of comparable size. There may be a small variation of thermal inertia with rotational phase (±60Jm-2K-1s-1/2). The spectral analysis is inconclusive in terms of surface mineralogy; the emissivity spectra have a relatively low signal-to-noise ratio and no spectral features are detected. The thermal inertia indicates average regolith grain size on the scale of several millimeters to about a centimeter. This moderate grain size is also consistent with low spectral contrast in the 7.5-20μm spectral range. If real, the rotational variation in thermal inertia would be consistent with a change in average grain size of only about a millimeter. The thermophysical properties of Bennu's surface appear to be fairly homogeneous longitudinally. A search for a dust coma failed to detect any extended emission, putting an upper limit of about 106g of dust within 4750km of Bennu. Three common methodologies for thermal modeling are compared, and some issues to be aware of when interpreting the results of such models are discussed. We predict that the OSIRIS-REx spacecraft will find a low albedo surface with abundant sub-cm sized grains, fairly evenly distributed in longitude. © 2014 Elsevier Inc.
• Hergenrother, C., Nolan, M., Binzel, R., Cloutis, E., Barucci, M., Michel, P., Scheeres, D., Drouet, d. C., Lazzaroh, D., Pinilla-Alonsoi, N., Campins, H., Licandro, J., Clark, B., Rizk, B., Beshore, E., & Lauretta, D. (2014). Color and Phase Function Photometry of the OSIRIS-REx Target Asteroid (101955) Bennu. Icarus, 226, 663-670.
• Moores, J., Brown, R., Lauretta, D., Smith, P., & Riofrio, L. (2014). Experimental and theoretical simulation of sublimating dusty water ice with implications for D/H ratios of water ice on Comets and Mars. Planetary Science, 1, 2-28.
• Nolan, M.,  Magri, C.,  Howell, E.,  Benner, L.,  Giorgini, J.,  Hergenrother, C., Hudson, R.,  Lauretta, D.,  Margot, J.,  Ostro, S., &  Scheeres, D. (2014). Asteroid (101955) Bennu Shape Model V1.0 NASA Planetary Data System, EAR-A-I0037-5-BENNUSHAPE-V1.0. Fall.
• {Andronikov}, A., {Subetto}, D., {Lauretta}, D., {Andronikova}, I., {Drosenko}, D., {Kuznetsov}, D., {Sapelko}, T., , L. (2014). In search for fingerprints of an extraterrestrial event: Trace element characteristics of sediments from the lake Medvedevskoye (Karelian Isthmus, Russia). Doklady Earth Sciences, 457, 819-823.
• {Chesley}, S., {Farnocchia}, D., Nolan, M. C., {Vokrouhlick{\'y}}, D., {Chodas}, P., {Milani}, A., {Spoto}, F., {Rozitis}, B., {Benner}, L., {Bottke}, W., {Busch}, M., {Emery}, J., Howell, E. S., Lauretta, D. S., {Margot}, J., , P. (2014). Orbit and bulk density of the OSIRIS-REx target Asteroid (101955) Bennu. \icarus, 235, 5-22.
• {Davidson}, J., {Krot}, A., {Nagashima}, K., {Hellebrand}, E., , D. (2014). Oxygen isotope and chemical compositions of magnetite and olivine in the anomalous CK3 Watson 002 and ungrouped Asuka-881595 carbonaceous chondrites: Effects of parent body metamorphism. Meteoritics and Planetary Science, 49, 1456-1474.
• {Davidson}, J., {Schrader}, D., {Alexander}, C., {Lauretta}, D., {Busemann}, H., {Franchi}, I., {Greenwood}, R., {Connolly}, H., {Domanik}, K., , A. (2014). Petrography, stable isotope compositions, microRaman spectroscopy, and presolar components of Roberts Massif 04133: A reduced CV3 carbonaceous chondrite. Meteoritics and Planetary Science, 49, 2133-2151.
• {Hergenrother}, C., {Barucci}, M., {Barnouin}, O., {Bierhaus}, B., {Binzel}, R., {Bottke}, W., {Chesley}, S., {Clark}, B., {Clark}, B., {Cloutis}, E., {Drouet d'Aubigny}, C., {Delbo}, M., {Emery}, J., {Gaskell}, B., Howell, E. S., {Keller}, L., {Kelley}, M., {Marshall}, J., {Michel}, P., , Nolan, M. C., et al. (2014). The Design Reference Asteroid for the OSIRIS-REx Mission Target (101955) Bennu. ArXiv e-prints.
• Gardner-Vandy, K. G., Lauretta, D. S., & McCoy, T. J. (2013). A petrologic, thermodynamic and experimental study of brachinites: Partial melt residues of an R chondrite-like precursor. Geochimica et Cosmochimica Acta, 122, 36-57.
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  Abstract: The primitive achondrites provide a window into the initial melting of asteroids in the early solar system. The brachinites are olivine-dominated meteorites with a recrystallized texture that we and others interpret as evidence of partial melting and melt removal on the brachinite parent body. We present a petrologic, thermodynamic and experimental study of the brachinites to evaluate the conditions under which they formed and test our hypothesis that the precursor material to the brachinites was FeO-rich compared to the precursors of other primitive achondrites. Petrologic analysis of six brachinites (Brachina, Allan Hills (ALH) 84025, Hughes 026, Elephant Moraine (EET) 99402, Northwest Africa (NWA) 3151, and NWA 4969) and one brachinite-like achondrite (NWA 5400) shows that they are meteorites with recrystallized texture that are enriched in olivine (≥80vol.%) and depleted in other minerals with respect to a chondritic mineralogy. Silicates in the brachinites are FeO-rich (Fa32-36). Brachinite-like achondrite Northwest Africa 5400 is similar in mineralogy and texture to the brachinites but with a slightly lower FeO-content (Fa30). Thermodynamic calculations yield equilibration temperatures above the Fe,Ni-FeS cotectic temperature (~950°C) for all meteorites studied here and temperatures above the silicate eutectic (~1050°C) for all but two. Brachina formed at an fO2 of ~IW, and the other brachinites and NWA 5400 formed at ~IW-1. All the meteorites show great evidence of formation by partial melting having approximately chondritic to depleted chondritic mineralogies, equilibrated mineral compositions, and recrystallized textures, and having reached temperatures above that required for melt generation. In an attempt to simulate the formation of the brachinite meteorites, we performed one-atmosphere, gas-mixing partial melting experiments of R4 chondrite LaPaz Ice Field 03639. Experiments at 1250°C and an oxygen fugacity of IW-1 produce residual phases that are within the mineralogy and mineral compositions of the brachinites. These experiments provide further evidence for the formation of brachinites as a result of partial melting of a chondritic precursor similar in mineralogy and mineral compositions to the R chondrites. © 2013 Elsevier Ltd.
• Hergenrother, C. W., Nolan, M. C., Binzel, R. P., Cloutis, E. A., Barucci, M. A., Michel, P., Scheeres, D. J., d'Aubigny, C. D., Lazzaro, D., Pinilla-Alonso, N., Campins, H., Licandro, J., Clark, B. E., Rizk, B., Beshore, E. C., & Lauretta, D. S. (2013). Lightcurve, Color and Phase Function Photometry of the OSIRIS-REx Target Asteroid (101955) Bennu. Icarus, 226(1), 663-670.
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  Abstract: The NASA OSIRIS-REx mission will retrieve a sample of the carbonaceous near-Earth Asteroid (101955) Bennu and return it to Earth in 2023. Photometry in the Eight Color Asteroid Survey (ECAS) filter system and Johnson-Cousins V and R filters were conducted during the two most recent apparitions in 2005/2006 and 2011/2012. Lightcurve observations over the nights of September 14-17, 2005 yielded a synodic rotation period of 4.2905. ±. 0.0065. h, which is consistent with the results of Nolan et al. (2013). ECAS color measurements made during the same nights confirm the B-type classification of Clark et al. (Clark, B.E., Binzel, R.P., Howell, E.S., Cloutis, E.A., Ockert-Bell, M., Christensen, P., Barucci, M.A., DeMeo, F., Lauretta, D.S., Connolly, H., Soderberg, A., Hergenrother, C., Lim, L., Emery, J., Mueller, M. [2011]. Icarus 216, 462-475). A search for the 0.7. μm hydration feature using the method of Vilas (Vilas, F. [1994]. Icarus 111, 456-467) did not reveal its presence. Photometry was obtained over a range of phase angles from 15° to 96° between 2005 and 2012. The resulting phase function slope of 0.040 magnitudes per degree is consistent with the phase slopes of other low albedo near-Earth asteroids (Belskaya, I.N., Shevchenko, V.G. [2000]. Icarus 147, 94-105). © 2013 Elsevier Inc.
• Lantz, C., Clark, B. E., Barucci, M. A., & Lauretta, D. S. (2013). Evidence for the effects of space weathering spectral signatures on low albedo asteroids. Astronomy and Astrophysics, 554.
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  Abstract: Context. Space weathering changes asteroid surfaces. We know from observations of the Moon and high-albedo asteroids that interplanetary surface processes can alter the spectral properties of silicates. The next step is to extend the study to primitive asteroids. This work supports the OSIRIS-REx mission by providing predictions for what space weathering effects we can expect to find on the mission target: asteroid (101955) 1999 RQ36. Aims. To investigate the possible spectral signatures of surface processes on carbonaceous (low-albedo) asteroids, we study the reflected light spectra of carbonaceous meteorites (assumed to represent asteroid subsurface materials) and compare them with telescopic reflected light spectra of asteroids (assumed to represent asteroid surface materials). Methods. In this work, we assume that primitive C-complex asteroids are the parent bodies of carbonaceous chondrites. We reason that differences between spectra of particulate samples of the meteorites and spectra of the regolith of asteroids can be due to either differences in textural properties, or differences caused by surface processes on the asteroid. We use telescopic observations of Ch/Cgh-type asteroids (0.4 to 2.4 μm) and compare them statistically with 106 CM meteorite spectra from RELAB. Results. Our results indicate spectral blueing of asteroids, with little to no concurrent albedo change or band modification. © 2013 ESO.
• Nolan, M. C., Magri, C., Howell, E. S., Benner, L. A., Giorgini, J. D., Hergenrother, C. W., Hudson, R. S., Lauretta, D. S., Margot, J., Ostro, S. J., & Scheeres, D. J. (2013). Shape model and surface properties of the OSIRIS-REx target Asteroid (101955) Bennu from radar and lightcurve observations. Icarus, 226(1), 629-640.
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  Abstract: We determine the three-dimensional shape of near-Earth Asteroid (101955) Bennu based on radar images and optical lightcurves. Bennu was observed both in 1999 at its discovery apparition, and in 2005 using the 12.6-cm radar at the Arecibo Observatory and the 3.5-cm radar at the Goldstone tracking station. Data obtained in both apparitions were used to construct a shape model of this object. Observations were also obtained at many other wavelengths to characterize this object, some of which were used to further constrain the shape modeling. The lightcurve data, along with an initial determination of the rotation period derived from them, simplified and improved the shape modeling.Below we briefly describe the observations and shape modeling process. We discuss the shape model and the implications for the possible formation and evolution of this object. We also describe the importance and limitations of the shape model in view of the fact that this object is the target of the OSIRIS-REx spacecraft mission. © 2013 Elsevier Inc.
• Nolan, M. C., {Magri}, C., Howell, E. S., {Benner}, L., {Giorgini}, J., {Hergenrother}, C., {Hudson}, R., Lauretta, D. S., {Margot}, J., {Ostro}, S., , D. (2013). Asteroid (101955) Bennu Shape Model V1.0. NASA Planetary Data System, 211.
• Nolan, M. C., {Magri}, C., Howell, E. S., {Benner}, L., {Giorgini}, J., {Hergenrother}, C., {Hudson}, R., Lauretta, D. S., {Margot}, J., {Ostro}, S., , D. (2013). Shape model and surface properties of the OSIRIS-REx target Asteroid (101955) Bennu from radar and lightcurve observations. \icarus, 226, 629-640.
• Schrader, D. L., Connolly, H. C., Lauretta, D. S., Nagashima, K., Huss, G. R., Davidson, J., & Domanik, K. J. (2013). The formation and alteration of the Renazzo-like carbonaceous chondrites II: Linking O-isotope composition and oxidation state of chondrule olivine. Geochimica et Cosmochimica Acta, 101, 302-327.
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  Abstract: To better understand the formation conditions of type-I and type-II chondrules in the Renazzo-like carbonaceous (CR) chondrites, an in situ major- and minor-element and O-isotope study was conducted. Twenty-one ferromagnesian chondrules from three CR chondrites (GRA 95229, GRA 06100, and QUE 99177) were analyzed to establish an internally-consistent data set. From this study we infer that type-II chondrule precursors contained enhanced S-bearing dust and ice abundances relative to type-I chondrules. There is a relationship between the O-isotope composition and oxidation state of olivine, which may be related to the amount of 16O-poor ice and reduced carbon accreted by chondrule precursors before melting. Type-II chondrules formed under H2O/H2 ratios of ∼230-740 times solar. In contrast, type-I chondrules formed under more reducing conditions with lower H2O/H2 ratios of ∼10-100 times solar. We find a relationship between type-II chondrule petrology (relict free vs. relict grain-bearing) and O-isotope composition, which is due to degree of melting and exchange with a 16O-poor gas reservoir. The 16O-poor gas that interacted with both type-I and type-II chondrules is estimated to have an isotopic composition between ∼δ18Og=13-27‰ and δ17Og=10-22‰, different from the O-isotope composition of the water accreted by the CR chondrite parent body. Due to partial melting, type-I chondrules and relict grain-bearing type-II chondrules exchanged with the 16O-poor gas to a lower degree than relict-free type-II chondrules. © 2012 Elsevier Ltd.
• Walsh, K. J., Delbó, M., Bottke, W. F., Vokrouhlický, D., & Lauretta, D. S. (2013). Introducing the Eulalia and new Polana asteroid families: Re-assessing primitive asteroid families in the inner Main Belt. Icarus, 225(1), 283-287.
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  Abstract: The so-called Nysa-Polana complex of asteroids is a diverse and widespread group studied by Cellino et al. (Cellino, A., Zappalà, V., Doressoundiram, A., di Martino, M., Bendjoya, P., Dotto, E., Migliorini, F., 2001. Icarus 152, 225-237) as a dynamically linked asteroid family. It carries the name of two asteroids because it appears to be two overlapping families of different asteroid taxonomies: (44) Nysa is an E-type asteroid with the lowest number in the midst of a predominantly S-type cluster and (142) Polana is a B-type asteroid near the low-albedo B-and C-type cluster. The latter has been shown to be a very important source of primitive near Earth asteroids.Using the data from the Wide-field Infrared Survey Explorer (WISE) mission we have re-analyzed the region around the Nysa-Polana complex in the inner Main Belt, focusing on the low-albedo population. (142) Polana does not appear to be a member of the family of low-albedo asteroids in the Nysa-Polana complex. Rather, the largest is Asteroid (495) Eulalia. This asteroid has never before been linked to this complex for an important dynamical reason: it currently has a proper eccentricity slightly below the range of most of the family members. However, its orbit is very close to the 3:1 mean motion resonance with Jupiter and is in a weak secular resonance. We show that its osculating eccentricity varies widely (e= 0.06-0.19) on short timescales (~1. Myr) and the averaged value diffuses (between e= 0.11-0.15) over long timescales (~100. Myr). The diffusive orbit, low-albedo, taxonomic similarity and semimajor axis strongly suggests that despite its current proper eccentricity, (495) Eulalia could have recently been at an orbit very central to the family. Hierarchical Clustering Method tests confirm that at an eccentricity of e= 0.15, (495) Eulalia could be the parent of the family. The "Eulalia family" was formed between 900 and 1500. Myr ago, and likely resulted from the breakup of a 100 to 160. km parent body.There is also compelling evidence for an older and more widespread primitive family in the same region of the asteroid belt parented by Asteroid (142) Polana. This family, the "new Polana family", is more extended in orbital elements, and is older than 2000. Myr. © 2013 Elsevier Inc.
• Zack, W., Andronikov, A., Rodríguez-Estrella, T., Lopez-Maritínez, M., Haber-Uriarte, M., Holliday, V., Lauretta, D., & Walker, M. (2013). Stone procurement and transport at the late Early Pleistocene site of Cueva Negra del Estrecho del Río Quípar (Murcia, SE Spain). Quartar, 60, 7-28.
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  Abstract: The late Early Pleistocene deposit, dating from ca. 0.8-0.9 Ma, at Cueva Negra del Estrecho del Río Quípar in Murcia, Spain, contains an abundant assemblage of small flaked artifacts of chert, quartzite and limestone, and one bifaciallyflaked limestone hand-axe. We have investigated several possible sources of the chert in an attempt to throw light on Palaeolithic interaction with the environment. Possible sources on the landscape were sampled at distances of up to 30 km from the site. Trace-element fingerprints were analyzed by laser-ablation inductively-coupled plasma mass-spectrometry (ICP-MS). Factor analysis was used to differentiate between sources and as a pointer to where chert analyzed from the cave may have been obtained. Our initial assumption was that most had come from less than 1 km away, namely, from a conglomerate outcrop where chert nodules could be quarried readily. Whilst trace-element evidence supports that hypothesis, it also points to a fair likelihood that some recovered chert lithics had been brought from sources up to 30 km away from the cave. Although evidence is scarce for transport of stone from a similar distance at other late Early Pleistocene sites in Europe, it nevertheless is present in the archaeological record, particularly in Spain where it may be possible to begin to consider differences in stone-procurement strategies between late Early Pleistocene technological assemblages.
• {Hergenrother}, C., Nolan, M. C., {Binzel}, R., {Cloutis}, E., {Barucci}, M., {Michel}, P., {Scheeres}, D., {d'Aubigny}, C., {Lazzaro}, D., {Pinilla-Alonso}, N., {Campins}, H., {Licandro}, J., {Clark}, B., {Rizk}, B., {Beshore}, E., & Lauretta, D. S. (2013). Lightcurve, Color and Phase Function Photometry of the OSIRIS-REx Target Asteroid (101955) Bennu. \icarus, 226, 663-670.
• Brown, R. H., Lauretta, D. S., Schmidt, B., & Moores, J. (2012). Experimental and theoretical simulations of ice sublimation with implications for the chemical, isotopic, and physical evolution of icy objects. Planetary and Space Science, 60(1), 166-180.
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  Abstract: Recent ground-based and spacecraft observations of comets in the inner solar system reveal two distinct features that provide important insight into their origin and evolution. The first of these is the observation that the D/H ratio of water vapor in cometary comae is significantly higher than that in Vienna Standard Mean Ocean Water (VSMOW). The second observation is that cometary jets are bursty (i.e, roughly steady state emissions that are punctuated with short-lived outbursts of water vapor and other materials) (Hughes, 1990; Soderblom et al, 2002; Soderblom et al, 2004a; Soderblom et al, 2004b). We present an experimental and theoretical study of ice sublimation in a vacuum that reveals several heretofore unknown and fundamental characteristics about the kinetics and mechanisms of ice sublimation that may explain both of these observed phenomena. In particular, we observe quasi-periodic sublimation cascades on time scales of hours to days, the D/H ratio in the vapor issuing from the sample is in general different from that of the sample, and in many cases, quasi-periodic changes in the D/H ratio of the vapor accompany the sublimation cascades. Changes are also observed in the infrared spectrum of the sample before, during and after a cascade that are consistent with our hypothesis that vacuum sublimation of water ice is a diffusive process that works to leave behind the most strongly bound molecules. Finally, we speculate as to whether the effects observed in the lab can be extrapolated to cometary-nucleus-scale phenomena. © 2011 Elsevier Ltd. All rights reserved.
• Gardner-Vandy, K. G., Lauretta, D. S., Greenwood, R. C., McCoy, T. J., Killgore, M., & Franchi, I. A. (2012). The Tafassasset primitive achondrite: Insights into initial stages of planetary differentiation. Geochimica et Cosmochimica Acta, 85, 142-159.
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  Abstract: Tafassasset is an exceptional meteorite that has been linked to both the CR chondrites and the primitive achondrites. Because previous evidence suggests it might be a primitive achondrite from a known chondrite type, we have undertaken a study of the petrology, geochemistry, and formation history of the meteorite. Tafassasset is predominantly FeO-rich olivine (~58%) yet contains abundant Fe,Ni-metal (~10vol.%) and sulfide (~3vol.%). Other phases include high- and low-Ca pyroxene, plagioclase, chromite, and phosphate. It has a recrystallized texture, containing equigranular grains that often meet at 120° triple junctions. There are no relict chondrules in the thin sections examined, although they have been reported previously. Electron microprobe analyses reveal homogeneous olivine (Fa 28.6), both low-and high-Ca pyroxene (Fs 23.6Wo 3.7 and Fs 12.2Wo 39.3±1), a range of plagioclase composition (An 23-47), Fe,Ni-metal (with 5.3-36.6wt.% Ni and 0.1-0.8wt.% Co), troilite, chromite, and Ca-phosphate. Bulk composition analyses reveal two chips depleted in refractory lithophile and some siderophile elements compared to CI chondrites. Exceptions are enrichments in Fe, Ni and Co. A third chip is essentially chondritic in bulk composition. Different stones of the meteorite have slightly different oxygen isotope composition, yet all lie in the CR chondrite trend with one in the acapulcoite-lodranite field. Thermodynamic calculations show that Tafassasset equilibrated at a temperature above the Fe,Ni-FeS eutectic and at an oxygen fugacity of ~IW-1. The texture, heterogeneous distribution of mineral phases, plagioclase composition, two-mineral closure temperatures, and bulk composition all provide evidence that Tafassasset partially melted on its parent body. A comparison with the CR chondrites, the brachinites, and two anomalous achondrites indicates that Tafassasset is most similar to ungrouped primitive achondrites Lewis Cliff (LEW) 88763 and Divnoe, and to the brachinites in overall petrography, modal mineralogy, mineral compositions, oxidation state, and bulk composition. The comparison also excludes the possibility that Tafassasset formed by partial melting of a CR chondrite. Tafassasset is a primitive achondrite and likely evolved on a parent body that experienced incomplete melting, never reached isotopic homogeneity, and was from the same oxygen isotopic reservoir as the CR chondrite parent body. © 2012 Elsevier Ltd.
• Pizzarello, S., Schrader, D. L., Monroe, A. A., & Lauretta, D. S. (2012). Large enantiomeric excesses in primitive meteorites and the diverse effects of water in cosmochemical evolution. Proceedings of the National Academy of Sciences of the United States of America, 109(30), 11949-11954.
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  PMID: 22778439;PMCID: PMC3409747;Abstract: Carbonaceous chondrites are meteoritic fragments of asteroids that avoided the geological reprocessing of larger planets and allow laboratory probing of early solar-nebula materials. Among these, Renazzo-type (CR) chondrites found in Antarctica appear remarkably pristine and are distinguished by abundant organic materials and water-soluble molecules such as amino acids and ammonia. We present a comprehensive analysis of the organic composition of selected CR meteorites of different petrographic classification and compare compounds' abundance and distribution as they may relate to asteroidal aqueous processing and concomitant evolution of the mineral phases. We found that several CR compounds such as amino acids and sugar alcohols are fully represented in stones with no or minimal water exposure indicating a formation that, if solar, preceded parent body processes. The most pristine CRs also revealed natal enantiomeric excesses (ee) of up to 60%, much larger than ever recorded. However, aqueous alteration appears to affect CR soluble organic composition and abundances, in particular some diastereomeric amino acids may gauge its extent by the consequent racemization of their ee.
• Berger, E. L., Zega, T. J., Keller, L. P., & Lauretta, D. S. (2011). Evidence for aqueous activity on comet 81P/Wild 2 from sulfide mineral assemblages in Stardust samples and CI chondrites. Geochimica et Cosmochimica Acta, 75(12), 3501-3513.
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  Abstract: The discovery of nickel-, copper-, and zinc-bearing iron sulfides from comet 81P/Wild 2 (Wild 2) represents the strongest evidence, in the Stardust collection, of grains that formed in an aqueous environment. We investigated three microtomed TEM sections which contain crystalline sulfide assemblages from Wild 2 and twelve thin sections of the hydrothermally altered CI chondrite Orgueil. Detailed structural and compositional characterizations of the sulfide grains from both collections reveal striking similarities. The Stardust samples include a cubanite (CuFe2S3) grain, a pyrrhotite [(Fe,Ni)1-xS]/pentlandite [(Fe,Ni)9S8] assemblage, and a pyrrhotite/sphalerite [(Fe,Zn)S] assemblage. Similarly, the CI-chondrite sulfides include individual cubanite and pyrrhotite grains, cubanite/pyrrhotite assemblages, pyrrhotite/pentlandite assemblages, as well as possible sphalerite inclusions within pyrrhotite grains. The cubanite is the low temperature orthorhombic form, which constrains temperature to a maximum of 210°C. The Stardust and Orgueil pyrrhotites are the 4C monoclinic polytype, which is not stable above ~250°C. The combinations of cubanite and pyrrhotite, as well as pyrrhotite and pentlandite signify even lower temperatures. The crystal structures, compositions, and petrographic relationships of these sulfides constrain formation and alteration conditions. Taken together, these constraints attest to low-temperature hydrothermal processing.Our analyses of these minerals provide constraints on large scale issues such as: heat sources in the comet-forming region; aqueous activity on cometary bodies; and the extent and mechanisms of radial mixing of material in the early nebula. The sulfides in the Wild 2 collection are most likely the products of low-temperature aqueous alteration. They provide evidence of radial mixing of material (e.g. cubanite, troilite) from the inner solar system to the comet-forming region and possible secondary aqueous processing on the cometary body. © 2011 Elsevier Ltd.
• Clark, B. E., Binzel, R. P., Howell, E. S., Cloutis, E. A., Ockert-Bell, M., Christensen, P., Barucci, M. A., DeMeo, F., Lauretta, D. S., Connolly, H., Soderberg, A., Hergenrother, C., Lim, L., Emery, J., & Mueller, M. (2011). Asteroid (101955) 1999 RQ36: Spectroscopy from 0.4 to 2.4μm and meteorite analogs. Icarus, 216(2), 462-475.
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  Abstract: We present reflectance spectra from 0.4 to 2.4μm of Asteroid (101955) 1999 RQ36, the target of the OSIRIS-REx spacecraft mission. The visible spectral data were obtained at the McDonald Observatory 2.1-m telescope with the ES2 spectrograph. The infrared spectral data were obtained at the NASA Infrared Telescope Facility using the SpeX instrument. The average visible spectrum is combined with the average near-infrared wavelength spectrum to form a composite spectrum. We use three methods to constrain the compositional information in the composite spectrum of Asteroid (101955) 1999 RQ36 (hereafter RQ36). First, we perform a least-squares search for meteorite spectral analogs using 15,000 spectra from the RELAB database. Three most likely meteorite analogs are proposed based on the least-squares search. Next, six spectral parameters are measured for RQ36 and their values are compared with the ranges in parameter values of the carbonaceous chondrite meteorite classes. A most likely meteorite analog group is proposed based on the depth of overlap in parameter values. The results of the least-squares search and the parametric comparisons point to CIs and/or CMs as the most likely meteorite analogs for RQ36, and COs and CHs as the least likely. RQ36 has a spectrally " blue" continuum slope that is also observed in carbonaceous chondrites containing magnetite. We speculate that RQ36 is composed of a " CM1" -like material. Finally, we compare RQ36 to other B-type asteroids measured by Clark et al. (Clark, B.E. et al. [2010]. J. Geophys. Res. 115, E06005). The results of this comparison are inconclusive. RQ36 is comparable to Themis spectral properties in terms of its albedo, visible spectrum, and near-infrared spectrum from 1.1 to 1.45μm. However, RQ36 is more similar to Pallas in terms of its near-infrared spectrum from 1.6 to 2.3μm. Thus it is possible that B-type asteroids form a spectral continuum and that RQ36 is a transitional object, spectrally intermediate between the two end-members. This is particularly interesting because Asteroid 24 Themis was recently discovered to have H2O ice on the surface (Rivkin, A., Emery, J. [2010]. Nature 464, 1322-1323; Campins, H. et al. [2010a]. Nature 464, 1320-1321). © 2011 Elsevier Inc.
• Gardner-Vandy, K. G., Hill, D. H., Lauretta, D. S., Goreva, Y. S., Domanik, K. J., Greenwood, R. C., Franchi, I. A., & Killgore, M. (2011). Petrology and geochemistry of the Northwest Africa 3368 eucrite. Meteoritics and Planetary Science, 46(7), 1052-1070.
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  Abstract: Analysis of the mineralogy, isotopic, and bulk compositions of the eucrite meteorites is imperative for understanding their origin on the asteroid 4 Vesta, the proposed parent body of the HED meteorites. We present here the petrology, mineral compositions, and bulk chemistry of several lithic components of the new brecciated basaltic eucrite Northwest Africa (NWA) 3368 to determine if all the lithologies reflect formation from one rock type or many rock types. The meteorite has three main lithologies: coarse- and fine-grained clasts surrounded by a fine-grained recrystallized silicate matrix. Silicate compositions are homogeneous, and the average rare earth element pattern for NWA 3368 is approximately 10× CI chondrites with a slight negative Eu anomaly. Major and trace element data place NWA 3368 with the Main Group-Nuevo Laredo trend. High-Ti chromites with ilmenite exsolution lamellae provide evidence of NWA 3368's history of intense metamorphism. We suggest that this meteorite underwent several episodes of brecciation and metamorphism, similar to that proposed by Metzler et al. (1995). We conclude that NWA 3368 is a monomict basaltic eucrite breccia related to known eucrites in texture and in mineral, bulk, and oxygen isotopic composition. © The Meteoritical Society, 2011.
• Lauretta, D. S. (2011). A cosmochemical view of the Solar System. Elements, 7(1), 11-16.
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  Abstract: Cosmochemistry is the study of extraterrestrial materials aimed at understanding the nature of Solar System bodies, including the planets, their natural satellites, and small bodies. An important goal is to increase our understanding of the chemical origin of the Solar System and the processes by which its planets and small bodies have evolved to their present states. Research in cosmochemistry covers an enormous range of disciplines and techniques, including mineralogy, petrology, major and trace element chemistry, isotope compositions, radiometric ages, magnetism, and radiationexposure effects. These studies provide a wealth of data about the processes of stellar evolution, planetary-system formation, alteration in asteroidal and cometary interiors, and the accretion history of the Earth, including the origin of Earth's volatile and organic materials.
• Palmer, E. E., & Lauretta, D. S. (2011). Aqueous alteration of kamacite in CM chondrites. Meteoritics and Planetary Science, 46(10), 1587-1607.
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  Abstract: The study of aqueous alteration of kamacite in CM chondrites provides insight on the conditions, products, and relative timing of aqueous alteration. We studied unaltered, partially altered, and fully altered kamacite grains from Murray, Murchison, Cold Bokkeveld, and Nogoya using optical microscopy, electron microprobe analysis, scanning electron microscopy, and Raman spectroscopy. From textual evidence and chemical analysis, we established three separate microchemical environments. 1) In a microchemical environment with a high S activity, kamacite alters to form tochilinite, P-bearing sulfides, eskolaite, and schreibersite. Mass balance calculations show that 81% of the Fe in kamacite is removed from the alteration region, making it available for the formation of other minerals or Fe-rich aureoles. The release of Fe can alter the mesostasis of type-I chondrules forming cronstedtite. 2) In a microchemical environment with a high Si activity and a low S activity, kamacite alters to form cronstedtite with small accessory sulfide inclusions. 3) A microchemical environment with limited S and Si activity results in kamacite alteration forming magnetite. The resulting magnetite retains associated Ni that can distinguish it from precipitated magnetite. In addition, the accessory phases of pentlandite and apatite can be formed if S or Ca are present. Finally, we note that small tochilinite grains in the matrix lack typical Ni, P, and Co levels, suggesting that they did not form from kamacite but possibly by sulfidization of magnetite. © The Meteoritical Society, 2011.
• Schrader, D. L., Franchi, I. A., Connolly, H. C., Greenwood, R. C., Lauretta, D. S., & Gibson, J. M. (2011). The formation and alteration of the Renazzo-like carbonaceous chondrites I: Implications of bulk-oxygen isotopic composition. Geochimica et Cosmochimica Acta, 75(1), 308-325.
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  Abstract: To better understand the role of aqueous alteration on the CR chondrite parent asteroid, a whole-rock oxygen isotopic study of 20 meteorites classified as Renazzo-like carbonaceous chondrites (CR) was conducted. The CR chondrites analyzed for their oxygen isotopes were Dhofar 1432, Elephant Moraine (EET) 87770, EET 92042, EET 96259, Gao-Guenie (b), Graves Nunataks (GRA) 95229, GRA 06100, Grosvenor Mountains (GRO) 95577, GRO 03116, LaPaz Ice Field (LAP) 02342, LAP 04720, Meteorite Hills (MET) 00426, North West Africa (NWA) 801, Pecora Escarpment (PCA) 91082, Queen Alexandra Range (QUE) 94603, QUE 99177, and Yamato-793495 (Y-793495). Three of the meteorites, Asuka-881595 (A-881595), GRA 98025, and MET 01017, were found not to be CR chondrites. The remaining samples concur petrographically and with the well-established oxygen-isotope mixing line for the CR chondrites. Their position along this mixing line is controlled both by the primary oxygen-isotopic composition of their individual components and their relative degree of aqueous alteration. Combined with literature data and that of this study, we recommend the slope for the CR-mixing line to be 0.70±0.04 (2σ), with a δ17O-intercept of -2.23±0.14 (2σ).Thin sections of Al Rais, Shişr 033, Renazzo, and all but 3 samples analyzed for oxygen isotopes were studied petrographically. The abundance of individual components is heterogeneous among the CR chondrites, but FeO-poor chondrules and matrix are the most abundant constituents and therefore, dominate the whole-rock isotopic composition. The potential accreted ice abundance, physico-chemical conditions of aqueous alteration (e.g. temperature and composition of the fluid) and its duration control the degree of alteration of individual CR chondrites. Combined with literature data, we suggest that LAP 02342 was exposed to lower temperature fluid during alteration than GRA 95229. With only two falls, terrestrial alteration of the CR chondrites complicates the interpretation of their whole rock isotopic composition, particularly in the most aqueously altered samples, and those with relatively higher matrix abundances. We report that QUE 99177 is the isotopically lightest whole rock CR chondrite known (δ18O=-2.29‰, δ17O=-4.08‰), possibly due to isotopically light unaltered matrix; which shows that the anhydrous component of the CR chondrites is isotopically lighter than previously thought. Although it experienced aqueous alteration, QUE 99177 provides the best approximation of the pristine CR-chondrite parent body's oxygen-isotopic composition, before aqueous alteration took place. Using this value as a new upper limit on the anhydrous component of the CR chondrites, water/rock ratios were recalculated and found to be higher than previously thought; ratios now range from 0.281 to 1.157. We also find that, according to their oxygen isotopes, a large number of CR chondrites appear to be minimally aqueously altered; although sample heterogeneity complicates this interpretation. © 2010 Elsevier Ltd.
• Bond, J. C., Lauretta, D. S., & O'Brien, D. P. (2010). Erratum to Making the Earth: Combining dynamics and chemistry in the Solar System[Icarus, 205, (2010), 321-337]. Icarus, 208(1), 504-.
• Bond, J. C., Lauretta, D. S., & O'Brien, D. P. (2010). Making the Earth: Combining dynamics and chemistry in the Solar System. Icarus, 205(2), 321-337.
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  Abstract: No terrestrial planet formation simulation completed to date has considered the detailed chemical composition of the planets produced. While many have considered possible water contents and late veneer compositions, none have examined the bulk elemental abundances of the planets produced as an important check of formation models. Here we report on the first study of this type. Bulk elemental abundances based on disk equilibrium studies have been determined for the simulated terrestrial planets of O'Brien et al. [O'Brien, D.P., Morbidelli, A., Levison, H.F., 2006. Icarus 184, 39-58]. These abundances are in excellent agreement with observed planetary values, indicating that the models of O'Brien et al. [O'Brien, D.P., Morbidelli, A., Levison, H.F., 2006. Icarus 184, 39-58] are successfully producing planets comparable to those of the Solar System in terms of both their dynamical and chemical properties. Significant amounts of water are accreted in the present simulations, implying that the terrestrial planets form "wet" and do not need significant water delivery from other sources. Under the assumption of equilibrium controlled chemistry, the biogenic species N and C still need to be delivered to the Earth as they are not accreted in significant proportions during the formation process. Negligible solar photospheric pollution is produced by the planetary formation process. Assuming similar levels of pollution in other planetary systems, this in turn implies that the high metallicity trend observed in extrasolar planetary systems is in fact primordial. © 2009 Elsevier Inc. All rights reserved.
• Bond, J. C., O'Brien, D. P., & Lauretta, D. S. (2010). The compositional diversity of extrasolar terrestrial planets. I. in situ simulations. Astrophysical Journal Letters, 715(2), 1050-1070.
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  Abstract: Extrasolar planet host stars have been found to be enriched in key planet-building elements. These enrichments have the potential to drastically alter the composition of material available for terrestrial planet formation. Here, we report on the combination of dynamical models of late-stage terrestrial planet formation within known extrasolar planetary systems with chemical equilibrium models of the composition of solid material within the disk. This allows us to determine the bulk elemental composition of simulated extrasolar terrestrial planets. A wide variety of resulting planetary compositions are found, ranging from those that are essentially "Earth like," containing metallic Fe and Mg silicates, to those that are dominated by graphite and SiC. This shows that a diverse range of terrestrial planets may exist within extrasolar planetary systems. © 2010. The American Astronomical Society. All rights reserved.
• Campins, H., Morbidelli, A., Tsiganis, K., León, J. D., Licandro, J., & Lauretta, D. (2010). The origin of asteroid 101955 (1999 RQ₃₆). Astrophysical Journal Letters, 721(1 PART 2), L53-L57.
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  Abstract: Near-Earth asteroid (NEA) 101955 (1999 RQ36; henceforth RQ36) is especially accessible to spacecraft and is the primary target of NASA's OSIRIS-REx sample return mission; it is also a potentially hazardous asteroid. We combine dynamical and spectral information to identify the most likely main-belt origin of RQ36 and we conclude that it is the Polana family, located at a semimajor axis of about 2.42 AU. We also conclude that the Polana family may be the most important inner-belt source of low-albedo NEAs. These conclusions are based on the following results. (1) Dynamical evidence strongly favors an inner-belt, low-inclination (2.15 AU < a < 2.5 AU and i < 10°) origin, suggesting the ?6 resonance as the preferred (95% probability) delivery route. (2) This region is dominated by the Nysa and Polana families. (3) The Polana family is characterized by low albedos and B-class spectra or colors, the same albedo and spectral class as RQ36. (4) The Sloan Digital Sky Survey colors show that the Polana family is the branch of the Nysa-Polana complex that extends toward the ?6 resonance; furthermore, the Polana family has delivered objects of the size of RQ36 and larger into the ?6 resonance. (5) A quantitative comparison of visible and near-infrared spectra does not yield a unique match for RQ36; however, it is consistent with a compositional link between RQ36 and the Polana family. © 2010. The American Astronomical Society. All rights reserved.
• Haynes Jr., C. V., Boerner, J., Domanik, K., Lauretta, D., Ballenger, J., & Goreva, J. (2010). The Murray Springs Clovis site, Pleistocene extinction, and the question of extraterrestrial impact. Proceedings of the National Academy of Sciences of the United States of America, 107(9), 4010-4015.
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  PMID: 20160115;PMCID: PMC2840150;Abstract: Some of the evidence for the recent hypothesis of an extraterrestrial impact that caused late Pleistocene megafaunal extinctions [Firestone et al. (2007) Proc Natl Acad Sci USA 104:16016-16021] was based upon samples collected at Murray Springs, a Clovis archaeological site in southeastern Arizona. Here we describe sampling and analyses of magnetic separates from within, above, and below the lower Younger Dryas boundary (LYDB) black mat at Murray Springs, as well as radiation measurements from the LYDB at Murray Springs and two other well-stratified Clovis sites. The main magnetic fraction at Murray Springs is maghemite. Magnetic microspherules have terrestrial origins but also occur as cosmic dust particles. We failed to find iridium or radiation anomalies. The evidence for massive biomass burning at Murray Springs is addressed and found to be lacking. We could not substantiate some of the claims by Firestone and others, but our findings do not preclude a terminal Pleistocene cosmic event.
• Haynes Jr., C. V., Lauretta, D. S., & A., J. (2010). Reply to Firestone et al.: No confirmation of impact at the lower Younger Dryas boundary at Murray Springs, AZ. Proceedings of the National Academy of Sciences of the United States of America, 107(26), E106.
• Lauretta, D. S., {Drake}, M., {Benzel}, R., {Campins}, H., {Chesley}, S., {Clark}, B., {Delbo}, M., {Emery}, J., {Hergenrother}, C., Nolan, M. C., {Scheeres}, D., & Team, {. (2010). Asteroid (101955) 1999 RQ36: Optimum Target for an Asteroid Sample Return Mission. Meteoritics and Planetary Science Supplement, 73, 5153.
• Schrader, D. L., & Lauretta, D. S. (2010). High-temperature experimental analogs of primitive meteoritic metal-sulfide-oxide assemblages. Geochimica et Cosmochimica Acta, 74(5), 1719-1733.
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  Abstract: We studied the oxidation-sulfidation behavior of an Fe-based alloy containing 4.75 wt.% Ni, 0.99 wt.% Co, 0.89 wt.% Cr, and 0.66 wt.% P in H2-H2O-CO-CO2-H2S gas mixtures at 1000 °C. The samples were cooled at rates of ∼3000 °C/h, comparable to estimates of the conditions after a chondrule-formation event in the early Solar System. Gas compositions were monitored in real time by a quadrupole mass spectrometer residual gas analyzer. Linear rate constants associated with gas-phase adsorption were determined. Reaction products were analyzed by optical microscopy, wavelength-dispersive-spectroscopy X-ray elemental mapping, and electron probe microanalysis. Based on analysis of the Fe-Ni-S ternary phase diagram and the reaction products, the primary corrosion product is a liquid of composition 66.6 wt.% Fe, 3.5 wt.% Ni, 29.9 wt.% S, and minor amounts of P, Cr, and Co. Chromite (FeCr2O4) inclusions formed by oxidation and are present in the metal foil and at the outer boundary between the sulfide and experimental atmosphere. During cooling the liquid initially crystallizes into taenite (average composition ∼15 wt.% Ni), monosulfide solid solution [mss, (Fe,Ni,Co,Cr)1-xS], and Fe-phosphates. Upon further cooling, kamacite exsolves from this metal, enriching the taenite in Ni. The remnant metal core is enriched in P and Co and depleted in Cr at the reaction interface, relative to the starting composition. The unreacted metal core composition remains unchanged, suggesting the reactions did not reach equilibrium. We present a detailed model of reaction mechanisms based on the observed kinetics and sample morphologies, and discuss meteoritic analogs in the CR chondrite MacAlpine Hills 87320. © 2009 Elsevier Ltd. All rights reserved.
• Schrader, D. L., Lauretta, D. S., Connolly Jr., H. C., Goreva, Y. S., Hill, D. H., Domanik, K. J., Berger, E. L., Yang, H., & Downs, R. T. (2010). Sulfide-rich metallic impact melts from chondritic parent bodies. Meteoritics and Planetary Science, 45(5), 743-758.
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  Abstract: Sacramento Wash 005 (SaW) 005, Meteorite Hills 00428 (MET) 00428, and Mount Howe 88403 (HOW) 88403 are S-rich Fe,Ni-rich metal meteorites with fine metal structures and homogeneous troilite. We compare them with the H-metal meteorite, Lewis Cliff 88432. Phase diagram analyses suggest that SaW 005, MET 00428, and HOW 88403 were liquids at temperatures above 1350 °C. Tridymite in HOW 88403 constrains formation to a high-temperature and low-pressure environment. The morphology of their metal-troilite structures may suggest that MET 00428 cooled the slowest, SaW 005 cooled faster, and HOW 88403 cooled the quickest. SaW 005 and MET 00428 contain H-chondrite like silicates, and SaW 005 contains a chondrule-bearing inclusion that is texturally and compositionally similar to H4 chondrites. The compositional and morphological similarities of SaW 005 and MET 00428 suggest that they are likely the result of impact processing on the H-chondrite parent body. SaW 005 and MET 00428 are the first recognized iron- and sulfide-rich meteorites, which formed by impact on the H-chondrite parent body, which are distinct from the IIE-iron meteorite group. The morphological and chemical differences of HOW 88403 suggest that it is not from the H-chondrite body, although it likely formed during an impact on a chondritic parent body. © 2010 The Meteoritical Society.
• Lauretta, D. S., & Schmidt, B. E. (2009). Oxidation of minor elements from an iron-nickel-chromium-cobalt-phosphorus alloy in 17.3% CO ₂-H ₂ gas mixtures at 700-1000 °c. Oxidation of Metals, 71(3-4), 219-235.
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  Abstract: Fe-Ni-Cr-Co-P alloys were exposed to 17.3% CO 2-H 2 gas mixtures to investigate the oxidation of minor elements in metallic alloys in the early solar system. Reaction temperatures varied between 700 and 1000 °C. Gas-phase equilibrium was attained at 800, 900, and 1000 °C, yielding H 2-H 2O-CO-CO 2 gas mixtures. Experiments at 700 and 750 °C did not achieve gas-phase equilibrium and were performed in H 2-CO 2 gas mixtures. Reaction timescales varied from 1 to 742 h. The experimental samples were characterized using optical microscopy, electron microprobe analysis, wavelength-dispersive- spectroscopy X-ray elemental mapping, and X-ray diffraction. In all experiments Cr experiences internal oxidation to produce inclusions of chromite (FeCr 2O 4) and eskolaite (Cr 2O 3) and surface layers of Cr-bearing magnetite [(Fe,Cr) 3O 4]. At 900 and 1000 °C, P is lost from the alloy via diffusion and sublimation from the metal surface. Analysis of P zoning profiles in the remnant metal cores allows for the determination of the P diffusion coefficient in the bulk metal, which is constant, and the internally oxidized layer, which is shown to vary linearly with distance from the metal surface. At 800 and 900 °C, P oxidizes to form a surface layer of graftonite [Fe 3(PO 4) 2] while at 700 and 750 °C P forms inclusions of the phosphide-mineral schreibersite [(Fe,Ni) 3P]. © 2009 Springer Science+Business Media, LLC.
• Lauretta, D. S., Goreva, J. S., Hill, D. H., Killgore, M., R., A., Campbell, A., Greenwood, R. C., Verchovsky, A. B., & Franchi, I. A. (2009). The fountain hills unique CB chondrite: Insights into thermal processes on the CB parent body. Meteoritics and Planetary Science, 44(6), 823-838.
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  Abstract: We report the results of an extensive study of the Fountain Hills chondritic meteorite. This meteorite is closely related to the CBa class. Mineral compositions and O-isotopic ratios are indistinguishable from other members of this group. However, many features of Fountain Hills are distinct from the other CB chondrites. Fountain Hills contains 23 volume percent metal, significantly lower than other members of this class. In addition, Fountain Hills contains porphyritic chondrules, which are extremely rare in other CBa chondrites. Fountain Hills does not appear to have experienced the extensive shock seen in other CB chondrites. The chondrule textures and lack of fine-grained matrix suggests that Fountain Hills formed in a dust-poor region of the early solar system by melting of solid precursors. Refractory siderophiles and lithophile elements are present in near-CI abundances (within a factor of two, related to the enhancement of metal). Moderately volatile and highly volatile elements are significantly depleted in Fountain Hills. The abundances of refractory siderophile trace elements in metal grains are consistent with condensation from a gas that is reduced relative to solar composition and at relatively high pressures (10-3 bars). Fountain Hills experienced significant thermal metamorphism on its parent asteroid. Combining results from the chemical gradients in an isolated spinel grain with olivine-spinel geothermometry suggests a peak temperature of metamorphism between 535 °C and 878 °C, similar to type-4 ordinary chondrites. © The Meteoritical Society, 2009.
• Bond, J. C., Lauretta, D. S., Tinney, C. G., Butler, R. P., Marcy, G. W., Jones, H. R., Carter, B. D., O'Toole, S., & Bailey, J. (2008). Beyond the iron peak: R- and s-process elemental abundances in stars with planets. Astrophysical Journal, 682(2), 1234-1247.
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  Abstract: We present elemental abundances of 118 stars (28 of which are known extrasolar planetary host stars) observed as part of the Anglo-Australian Planet Search. Abundances of O, Mg, Cr, Y, Zr, Ba, Nd, and Eu (along with previously published abundances for C and Si) are presented. This study is one of the first to specifically examine planetary host stars for the heavy elements produced by neutron capture reactions. We find that the abundances in host stars are chemically different from both the standard solar abundances and the abundances in non-host stars in all elements studied, with enrichments over non-host stars ranging from 0.06 dex (for O) to 0.11 dex (for Cr and Y). Such abundance trends are in agreement with other previous studies of field stars and lead us to conclude that the chemical anomalies observed in planetary host stars are the result of normal galactic chemical evolution processes. Based on this observation, we conclude that the observed chemical traits of planetary host stars are primordial in origin, coming from the original nebula and not from a "pollution" process occurring during or after formation, and that planet formation occurs naturally with the evolution of stellar material. © 2008. The American Astronomical Society. All rights reserved.
• Pasek, M., & Lauretta, D. (2008). Extraterrestrial flux of potentially prebiotic C, N, and P to the early earth. Origins of Life and Evolution of Biospheres, 38(1), 5-21.
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  PMID: 17846915;Abstract: With growing evidence for a heavy bombardment period ending 4-3.8 billion years ago, meteorites and comets may have been an important source of prebiotic carbon, nitrogen, and phosphorus on the early Earth. Life may have originated shortly after the late-heavy bombardment, when concentrations of organic compounds and reactive phosphorus were enough to "kick life into gear". This work quantifies the sources of potentially prebiotic, extraterrestrial C, N, and P and correlates these fluxes with a comparison to total Ir fluxes, and estimates the effect of atmosphere on the survival of material. We find (1) that carbonaceous chondrites were not a good source of organic compounds, but interplanetary dust particles provided a constant, steady flux of organic compounds to the surface of the Earth, (2) extraterrestrial metallic material was much more abundant on the early Earth, and delivered reactive P in the form of phosphide minerals to the Earth's surface, and (3) large impacts provided substantial local enrichments of potentially prebiotic reagents. These results help elucidate the potential role of extraterrestrial matter in the origin of life. © 2007 Springer Science+Business Media B.V.
• Schrader, D. L., Connolly Jr., H. C., & Lauretta, D. S. (2008). Opaque phases in type-II chondrules from CR2 chondrites: Implications for CR parent body formation. Geochimica et Cosmochimica Acta, 72(24), 6124-6140.
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  Abstract: We report the results of a detailed study of sulfide-bearing opaque assemblages from the MAC 87320, EET 92011, and Renazzo CR carbonaceous chondrites. The objectives of this study are to (1) characterize sulfide and associated phases within CR2 chondrites; (2) determine the petrographic relationship between sulfides, metals, and chondrules; (3) constrain the history of type-II chondrules; (4) ascertain the environments in which type-II chondrules formed and were altered; and (5) unravel the formation and alteration history of the CR parent body as recorded in sulfide-bearing assemblages. Sulfide-bearing opaque assemblages occur primarily within type-II (FeO-rich) chondrules. The sulfide assemblages are concentrated near the chondrule edges. Assemblages in MAC 87320 are composed of troilite, phosphate, and Ni-rich metal. EET 92011 contains assemblages composed of pentlandite, troilite, and Ni-rich metal. The assemblages in Renazzo contain tochilinite, magnetite, troilite, pentlandite, and phosphate. In all of the assemblages in Renazzo the tochilinite is fine grained and intimately mixed with troilite, pentlandite, or magnetite. Opaque assemblages in CR chondrites record a complex history that includes both high- and low-temperature processes. The morphology and composition of sulfides in CR2 chondrites suggests that the sulfide-bearing assemblages originally formed in gas-solid reactions in the nebula at temperatures above the Fe-FeS eutectic (988 °C). Many of the assemblages were subsequently aqueously altered on the CR-chondrite parent body to various degrees at temperatures from ∼50 to 200 °C. We combine these observations and interpretations to provide a detailed model of the history of the CR parent body. © 2008 Elsevier Ltd.
• Pasek, M. A., Dworkin, J. P., & Lauretta, D. S. (2007). A radical pathway for organic phosphorylation during schreibersite corrosion with implications for the origin of life. Geochimica et Cosmochimica Acta, 71(7), 1721-1736.
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  Abstract: Phosphorylated compounds (e.g., DNA, RNA, phospholipids, and many coenzymes) are critical to biochemistry. Thus, their origin is of prime interest to origin of life studies. The corrosion of the meteoritic mineral schreibersite ((Fe, Ni)3P) may have significantly contributed to the origin of phosphorylated biomolecules. Corrosion of synthetic schreibersite in a variety of solutions was analyzed by nuclear magnetic resonance spectroscopy, mass spectrometry, and electron paramagnetic resonance spectroscopy. These methods suggest a free-radical reaction pathway for the corrosion of schreibersite to form phosphite radicals ({radical dot} PO32 -) in aqueous solution. These radicals can form activated polyphosphates and can phosphorylate organic compounds such as acetate to form phosphonates and organophosphates (3% total yield). Phosphonates (O3P-C) are found in the organic P inventory of the carbonaceous meteorite Murchison. While phosphonates are rare in biochemistry, the ubiquity of corroding iron meteorites on the early Earth could have provided a source of organic phosphorous compounds for the origin of life, and may have led to the role of organophosphates as a product of early evolution. © 2007 Elsevier Ltd. All rights reserved.
• Rosenshein, E. B., Ivanova, M. A., Dickinson, T. L., McCoy, T. J., Lauretta, D. S., Guan, Y., Leshin, L. A., & Benedix, G. K. (2006). Oxide-bearing and FeO-rich clasts in aubrites. Meteoritics and Planetary Science, 41(4), 495-503.
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  Abstract: We report the occurrence of an oxide-bearing clast and an FeO-rich clast from aubrites. The FeO-rich clast in Pesyanoe is dominated by olivine and pyroxene phenocrysts with mineral compositions slightly less FeO-rich than is typical for H chondrites. In Allan Hills (ALH) 84008, the oxide-bearing clast consists of a single forsterite grain rimmed by an array of sulfides, oxides, and phosphides. We consider a number of possible origins. We can exclude formation by melting of oxide-bearing chondrules and CAIs formed in enstatite chondrites. The Pesyanoe clast may have formed in a more oxidized region of the aubrite parent body or, more likely, is a foreign clast from a more oxidized parent body. The ALH 84008 clast likely formed by reaction between sulfides and silicates as a result of cooling, oxidation, or de-sulfidization. This clast appears to be the first oxide-bearing clast from an aubritic breccia that formed on the aubrite parent body. Identification of additional oxide-bearing clasts in aubrites could shed light on whether this was a widespread phenomenon and the origin of these enigmatic objects. © The Meteoritical Society, 2006.
• Benedix, G. K., Lauretta, D. S., & McCoy, T. J. (2005). Thermodynamic constraints on the formation conditions of winonaites and silicate-bearing IAB irons. Geochimica et Cosmochimica Acta, 69(21), 5123-5131.
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  Abstract: Silicate inclusions in IAB irons and related winonaite meteorites have textures, mineralogies and mineral chemistries that indicate a complex formation history of heating, followed by brecciation and metamorphism. Using olivine-orthopyroxene-chromite assemblages in five IAB iron silicate inclusions (Caddo County, Campo del Cielo, Copiapo, Lueders, and Udei Station) and one winonaite (Winona), we calculated closure temperatures and oxygen fugacities for these meteorites. Calculated olivine-chromite Fe-Mg exchange temperatures are compared to two-pyroxene temperatures. Olivine-chromite closure temperatures range from ∼590°C to ∼700°C, while two-pyroxene temperatures range from ∼900°C to ∼1200°C. Oxygen fugacities of these meteorites, determined for the first time in this study, range from 2.3 to 3.2 log units below the Fe-FeO buffer and define a line between the Fe-FeO and Cr-Cr2O3 buffers. Highly variable temperatures were experienced by these rocks on the hand sample, and sometimes even the thin section, scale consistent with the idea that the winonaite-IAB iron parent body experienced collisional fragmentation and reassembly after peak temperatures were reached. Although modest reduction likely occurred during cooling, the oxygen fugacities and mineral compositions recorded at peak metamorphic temperatures suggest that the chondritic precursor for this parent body was initially more reduced than ordinary chondrites. Copyright © 2005 Elsevier Ltd.
• Bullock, E. S., Gounelle, M., Lauretta, D. S., Grady, M. M., & Russell, S. S. (2005). Mineralogy and texture of Fe-Ni sulfides in CI1 chondrites: Clues to the extent of aqueous alteration on the CI1 parent body. Geochimica et Cosmochimica Acta, 69(10), 2687-2700.
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  Abstract: To better understand the role of aqueous alteration on the CI1 parent body, we have analyzed the texture, composition and mineral associations of iron nickel sulfides in four of the five known CI1 chondrites. The most commonly-occurring sulfide present in the CI1 chondrites is the iron-deficient Fe,Ni sulfide pyrrhotite ([Fe,Ni]1-xS), that has a composition close to that of stoichiometric troilite (FeS). Three of the CI1s (Alais, Ivuna and Tonk) also contain pentlandite ([Fe,Ni]9S8), although pentlandite is a rare phase in Ivuna. Cubanite (CuFe2S3) was found in both Alais and Ivuna in this study, although it has also been reported in Orgueil (MacDougall and Kerridge, 1977). The pyrrhotite grains in all four chondrites form hexagonal, rectangular or irregular shapes, and show no evidence of Ni or Co zoning. The pyrrhotite grains in Orgueil and Ivuna are, in general, smaller, and show more "corrosions," or "embayments," than those in Alais or Tonk. We suggest that the precursor sulfide present in the CI1 chondrites was troilite which, during brecciation and oxidation on the parent body at a temperature of 100°C or less, converted the troilite to magnetite and pyrrhotite with pentlandite inclusions. Subsequently, continued alteration on the parent body removed pentlandite-partially from Alais, Tonk and Ivuna, completely from Orgueil-leaving behind pyrrhotite with spaces ("corrosions") where the pentlandite had been. Ni derived from the pentlandite was incorporated into ferrihydrite, onto the surface of which the Ni,Na sulfate Ni-bloedite formed. Based on the size and abundant "corrosions" within pyrrhotite grains, combined with observations from other authors, we conclude that Orgueil and Ivuna have undergone a greater degree of alteration than Alais and Tonk. Further work is needed to assess the conditions under which pentlandite would be dissolved preferentially to pyrrhotite, as the study of terrestrial literature indicates that the latter mineral is preferentially removed. Copyright © 2005 Elsevier Ltd.
• Ciesla, F., & Lauretta, D. (2005). Radial migration and dehydration of phyllosilicates in the solar nebula. Earth and Planetary Science Letters, 231(1-2), 1-8.
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  Abstract: While it is currently thought that Earth's water was delivered by hydrous minerals, the origin of these minerals is still debated. Nebular models suggest that the area where the Earth formed was too hot for these minerals to form, leading many to believe that they were delivered by large planetary embryos which formed in the outer asteroid belt region of the solar nebula. Others have argued that the hydrous minerals were present during the early accretion phase of the Earth in order to explain different aspects of its geochemistry and therefore, must have formed locally, implying that the nebula must have been cooler than the models predict. In this paper we explore a new possibility: that these hydrous minerals were formed in the outer asteroid belt region of the solar nebula and were then brought into the hotter regions of the nebula by gas drag where they were incorporated into the planetesimals which formed there. The hydrated minerals were able to survive for long periods of time in this hot region due to the sluggish dehydration kinetics. We find that this process need not have been efficient, requiring only a small amount (∼few percentages) of the material in the outer asteroid belt region of the nebula to be subject to this process. This delivery mechanism provides a way for hydrous minerals to be incorporated early on into the planetesimals which were accreted by the Earth without having to alter the generally accepted solar nebula models that are consistent with meteoritic and asteroidal observations. © 2004 Elsevier B.V. All rights reserved.
• Lauretta, D. S. (2005). Sulfidation of an iron-nickel-chromium-cobalt- Phosphorus alloy in1% H ₂S-H ₂ gas mixtures at 400-1000°C. Oxidation of Metals, 64(1-2), 1-22.
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  Abstract: The sulfidation of an Fe-based alloy containing 4.75 wt.% Ni, 0.99 wt.% Co, 0.89 wt.% Cr, and 0.66 wt.% P in 1.1% H 2S-H 2 gas mixtures was studied at 400-1000°C. Reaction kinetics were determined by monitoring the abundance of S-gas species continuously throughout each experiment. This approach allows for determination of both linear rate constants associated with adsorption and decomposition of S-gas molecules and parabolic rate constants associated with cation diffusion. The activation energy for these processes are 12 ± 4 kJ/mole and 50 ± 12 kJ/mole, respectively. In all experiments, P is excluded from the sulfide phase and precipitates as the mineral schreibersite [(Fe, Ni, Co) 3P]. In addition a monosulfide solid solution formed containing variable abundances of Ni, Cr, and Co. Analyses of the compositional profiles allows for the determination of activity coefficients for NiS, CrS, and CoS in FeS as well as the self-diffusivities for Ni, Cr, and Co in the sulfide scale, relative to Fe. © 2005 Springer Science+Business Media, Inc.
• Messenger, S., Keller, L. P., & Lauretta, D. S. (2005). Geochemistry: Supernova olivine from cometary dust. Science, 309(5735), 737-741.
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  PMID: 15994379;Abstract: An interplanetary dust particle contains a submicrometer crystalline silicate aggregate of probable supernova origin. The grain has a pronounced enrichment in 18O/16O (13 times the solar value) and depletions in 17O/16O (one-third solar) and 29Si/28Si (
• Pasek, M. A., & Lauretta, D. S. (2005). Aqueous corrosion of phosphide minerals from iron meteorites: A highly reactive source of prebiotic phosphorus on the surface of the early earth. Astrobiology, 5(4), 515-535.
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  PMID: 16078869;Abstract: We present the results of an experimental study of aqueous corrosion of Fe-phosphide under conditions relevant to the early Earth. The results strongly suggest that iron meteorites were an important source of reactive phosphorus (P), a requirement for the formation of P-based life. We further demonstrate that iron meteorites were an abundant source of phosphide minerals early in Earth history. Phosphide corrosion was studied in five different solutions: deionized water, deionized water buffered with sodium bicarbonate, deionized water with dissolved magnesium and calcium chlorides, deionized water containing ethanol and acetic acid, and deionized water containing the chlorides, ethanol, and acetic acid. Experiments were performed in the presence of both air and pure Ar gas to evaluate the effect of atmospheric chemistry. Phosphide corrosion in deionized water results in a metastable mixture of mixed-valence, P-bearing ions including pyrophosphate and triphosphate, key components for metabolism in modern life. In a pH-buffered solution of NaHCO3, the condensed and reduced species diphosphonate is an abundant corrosion product. Corrosion in ethanol- and acetic acid-containing solutions yields additional P-bearing organic molecules, including acetyl phosphonate and a cyclic triphosphorus molecule. Phosphonate is a major corrosion product of all experiments and is the only P-bearing molecule that persists in solutions with high concentrations of magnesium and calcium chlorides, which suggests that phosphonate may have been a primitive oceanic source of P. The stability and reactivity of phosphonate and hypophosphite in solution were investigated to elucidate reaction mechanisms and the role of mineral catalysts on P-solution chemistry. Phosphonate oxidation is rapid in the presence of Fe metal but negligible in the presence of magnetite and in the control sample. The rate of hypophosphite oxidation is independent of reaction substrate. © Mary Ann Liebert, Inc.
• Pasek, M. A., Milsom, J. A., Ciesla, F. J., Lauretta, D. S., Sharp, C. M., & Lunine, J. I. (2005). Sulfur chemistry with time-varying oxygen abundance during Solar System formation. Icarus, 175(1), 1-14.
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  Abstract: Chemical models of solar nebula chemistry are presented which show the influence of progressive water depletion from the inner solar nebula. The main focus of this work is the equilibrium distribution of S resulting from this process. Under canonical solar nebula conditions, H2S is the dominant S-bearing species in the gas phase and troilite (FeS) is the primary reservoir for S after condensation. As water vapor diffuses out to its condensation front, the equilibrium distribution of S changes significantly. With the removal of water vapor, SiS becomes the most abundant S-bearing gas and MgS and CaS compete with FeS as the main sulfide reservoir. These results allow us to argue that some of the minerals in the enstatite chondrites formed through the heterogeneities associated with the nebular ice condensation front, and that the sulfur abundance in Jupiter reflects a depletion in H2S that is the result of inner nebula sulfur chemistry under varying oxygen abundance. © 2004 Elsevier Inc. All rights reserved.
• Ciesla, F. J., Lauretta, D. S., & Hood, L. L. (2004). The frequency of compound chondrules and implications for chondrule formation. Meteoritics and Planetary Science, 39(4), 531-544.
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  Abstract: The properties of compound chondrules and the implications that they have for the conditions and environment in which chondrules formed are investigated. Formulae to calculate the probability of detecting compound chondrules in thin sections are derived and applied to previous studies. This reinterpretation suggests that at least 5% of chondrules are compounds, a value that agrees well with studies in which whole chondrules were removed from meteorites. The observation that adhering compounds tend to have small contact arcs is strengthened by application of these formulae. While it has been observed that the secondaries of compound chondrules are usually smaller than their primaries, these same formulae suggest that this could be an observation bias. It is more likely than not that thin section analyses will identify compounds with secondaries that are smaller than their primaries. A new model for chondrule collisional evolution is also developed. From this model, it is inferred that chondrules would have formed, on average, in areas of the solar nebula that had solids concentrated at least 45 times over the canonical solar value. © Meteoritical Society, 2004.
• Lauretta, D. S. (2004). Corrosion of solar-composition Fe-based alloys: First results from the nine circles experimental cosmochemistry laboratory. Meteoritics and Planetary Science, 39(SUPPL.), A59.
• Marsh, C. A., Lauretta, D. S., & Domanik, K. J. (2004). Thermal metamorphism: Results from a new technique for determining homogeneity of major minerals in ordinary chondrites. Meteoritics and Planetary Science, 39(SUPPL.), A62.
• Stimpfl, M., Lauretta, D. S., & Drake, M. J. (2004). Adsorption as a mechanism to deliver water to the earth. Meteoritics and Planetary Science, 39(SUPPL.), A99.
• Ciesla, F. J., Lauretta, D. S., Cohen, B. A., & Hood, L. L. (2003). A nebular origin for chondritic fine-grained phyllosilicates. Science, 299(5606), 549-552.
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  PMID: 12543970;Abstract: Hydrated minerals occur in accretionary rims around chondrules in CM chondrites. Previous models suggested that these phyllosilicates did not form by gas-solid reactions in the canonical solar nebula. We propose that chondrule-forming shock waves in icy regions of the nebula produced conditions that allowed rapid mineral hydration. The time scales for phyllosilicate formation are similar to the time it takes for a shocked system to cool from the temperature of phyllosilicate stability to that of water ice condensation. This scenario allows for simultaneous formation of chondrules and their fine-grained accretionary rims.
• Kojima, T., Lauretta, D. S., & Buseck, P. R. (2003). Accretion, dispersal, and reaccumulation of the Bishunpur (LL3.1) brecciated chondrite Evidence from troilite-silicate-metal inclusions and chondrule rims. Geochimica et Cosmochimica Acta, 67(16), 3065-3078.
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  Abstract: A set of troilite-silicate-metal (TSM) inclusions and chondrule rims in the Bishunpur (LL3.1) chondrite provide information regarding impact brecciation of small bodies in the early solar system. The TSM inclusions and chondrule rims consist of numerous angular to subrounded silicate grains that are individually enclosed by fine networks of troilite. FeNi metal also occurs in the troilite matrix. The silicates include olivine (Fo55-98),low-Ca pyroxene (En78-98), and high-Ca pyroxene (En48-68Wo11-32). Al- and Si-rich glass coexists with the silicates. Relatively coarse silicate grains are apparently fragments of chondrules typical of petrologic type-3 chondrites. Troilite fills all available cracks and pores in the silicate grains. Some of the TSM inclusions and rims are themselves surrounded by fine-grained silicate-rich rims (FGR). The TSM inclusions and rims texturally resemble the troilite-rich regions in the Smyer H-chondrite breccia. They probably formed by shock-induced mobilization of troilite during an impact event on a primitive asteroidal body. Because silicates in the TSM inclusions and rims have highly unequilibrated compositions, their precursor was presumably type-3 chondritic material like Bishunpur itself. The TSM inclusions and the chondrules with the TSM rims were fragmented and dispersed after the impact-induced compaction, then reaccreted onto the Bishunpur parent body. FGR probably formed around the TSM inclusions and rims, as well as around some chondrules, during the reaccumulation process. Components of most type-2 and 3 chondrites probably experienced similar processing, i.e., dispersal of unconsolidated materials and subsequent reaccumulation. © 2003 Elsevier Ltd.
• Lauretta, D. S., & Buseck, P. R. (2003). Opaque minerals in chondrules and fine-grained chondrule rims in the Bishunpur (LL3.1) chondrite. Meteoritics and Planetary Science, 38(1), 59-79.
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  Abstract: We present a detailed petrographic and electron microprobe study of metal grains and related opaque minerals in the chondrule interiors and rims of the Bishunpur (LL3.1) ordinary chondrite. There are distinct differences between metal grains that are completely encased in chondrule interiors and those that have some portion of their surface exposed outside of the chondrule boundary, even though the two types of metal grains can be separated by only a few microns. Metal grains in chondrule interiors exhibit minor alteration in the form of oxidized P-, Cr-, and Si-bearing minerals. Metal grains at chondrule boundaries and in chondrule rims are extensively altered into troilite and fayalite. The results of this study suggest that many metal grains in Bishunpur reacted with a type-I chondrule melt and incorporated significant amounts of P, Cr, and Si. As the system cooled, some metal oxidation occurred in the chondrule interior, producing metal-associated phosphate, chromite, and silica. Metal that migrated to chondrule boundaries experienced extensive corrosion as a result of exposure to the external atmosphere present during chondrule formation. It appears that chondrule-derived metal and its corrosion products were incorporated into the fine-grained rims that surround many type-I chondrules, contributing to their Fe-rich compositions. We propose that these fine-grained rims formed by a combination of corrosion of metal expelled from the chondrule interior and accretion of fine-grained mineral fragments and microchondrules.
• Lauretta, D. S., Buseck, P. R., & Zega, T. J. (2001). Opaque minerals in the matrix of the Bishunpur (LL3.1) chondrite: Constraints on the chondrule formation environment. Geochimica et Cosmochimica Acta, 65(8), 1337-1353.
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  Abstract: The chemistry and mineralogy of a group of opaque mineral assemblages in the matrix of the Bishunpur LL3.1 ordinary chondrite provide insight into the nebular environment in which they formed. The assemblages consist of a kamacite (Fe,Ni) core that is rimmed by troilite (FeS) and fayalite (Fe2SiO4). Accessory phases in the rims include silica (SiO2), chromite (FeCr2O4), whitlockite (Ca3(PO4)2), maricite (FeNaPO4), magnetite (Fe3O4), and tetrataenite (FeNi). We suggest that the metal melted in and equilibrated with an igneous chondrule under high-temperature, reducing conditions. In this environment the molten alloys incorporated varied amounts of Si, Ni, P, Cr, and Co, depending on the oxygen fugacity and temperature of the melt. Some of the metal was subsequently expelled from the chondrule interiors into the surrounding nebular gas. As the temperature dropped, the alloy solidified and volatile elements corroded the metal. The main reaction products were troilite and fayalite. Thermodynamic equilibrium calculations are used to constrain the conditions under which these two phases can form simultaneously in the solar nebula. Kinetic factors are used to place a lower limit on the formation temperature. We determine that the metal corroded between 1173 and 1261 K at a total pressure in the range of 10-5.0 to 10-4.1 bars and a dust/gas ratio of 302 to 355 x relative to solar composition. These conditions are consistent with our model that the metal corroded in a dust-rich region of the solar nebula that was cooling after a chondrule formation event. Copyright © 2001 Elsevier Science Ltd.
• Lauretta, D. S., Klaue, B., Blum, J. D., & Buseck, P. R. (2001). Mercury abundances and isotopic compositions in the murchison (CM) and Allende (CV) carbonaceous chondrites. Geochimica et Cosmochimica Acta, 65(16), 2807-2818.
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  Abstract: The abundance and isotopic composition of Hg was determined in bulk samples of both the Murchison (CM) and Allende (CV) carbonaceous chondrites using single- and multi-collector inductively coupled plasma mass spectrometry (ICP-MS). The bulk abundances of Hg are 294 ± 15 ng/g in Murchison and 30.0 ± 1.5 ng/g in Allende. These values are within the range of previous measurements of bulk Hg abundances by neutron activation analysis (NAA). Prior studies suggested that both meteorites contain isotopically anomalous Hg, with δ196/202Hg values for the anomalous, thermal-release components from bulk samples ranging from -260 ‰ to +440 ‰ in Murchison and from -620 ‰ to +540 ‰ in Allende (Jovanovic and Reed, 1976a; 1976b; Kumar and Goel, 1992). Our multi-collector ICP-MS measurements suggest that the relative abundances of all seven stable Hg isotopes in both meteorites are identical to terrestrial values within 0.2 to 0.5 ‰. On-line thermal-release experiments were performed by coupling a programmable oven with the single-collector ICP-MS. Powdered aliquots of each meteorite were linearly heated from room temperature to 900°C over twenty-five minutes under an Ar atmosphere to measure the isotopic composition of Hg released from the meteorites as a function of temperature. In separate experiments, the release profiles of S and Se were determined simultaneously with Hg to constrain the Hg distribution within the meteorites and to evaluate the possibility of Se interferences in previous NAA studies. The Hg-release patterns differ between Allende and Murchison. The Hg-release profile for Allende contains two distinct peaks, at 225° and 343°C, whereas the profile for Murchison has only one peak, at 344°C. No isotopically anomalous Hg was detected in the thermal-release experiments at a precision level of 5 to 30 ‰, depending on the isotope ratio. In both meteorites the Hg peak at Ο340°C correlates with a peak in the S-release profile. This correlation suggests that Hg is associated with S-bearing phases and, thus, that HgS is a major Hg-bearing phase in both meteorites. The Hg peak at 225°C for Allende is similar to release patterns of physically adsorbed Hg on silicate and metal grains. Prior studies suggested that the isotopic anomalies reported from NAA resulted from interference between 203Hg and 75Se. However, the amount of Se released from both meteorites, relative to Hg, is insufficient to produce all of the observed anomalies. Copyright © 2001 Elsevier Science Ltd.
• Lauretta, D. S., Hua, X., & Buseck, P. R. (2000). Mineralogy of fine-grained rims in the ALH 81002 CM chondrite. Geochimica et Cosmochimica Acta, 64(19), 3263-3273.
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  Abstract: The mineralogy of fine-grained rims in ALH 81002, a relatively primitive CM carbonaceous chondrite, has been determined by using transmission electron microscopy. The most abundant phase is Mg-rich serpentine, which occurs in small (≤20 nm) crystals with cylindrical or fibrous morphologies. Cronstedtite, an Fe-rich phyllosilicate, occurs as relatively large (100 to 2500 nm), platy crystals. Some cronstedtite is coherently intergrown with tochilinite. In many cases, cronstedtite has been partially altered to serpentine. The compositions and textures of these two phases provide a mineralogical and morphologic alteration sequence that parallels the known compositional trend for CM chondrite matrix. Accessory minerals embedded within the phyllosilicates include chlorite, pentlandite, gypsum, olivine, kamacite, taenite, and chromite. Regions containing only anhydrous minerals also occur. The hydrated and anhydrous regions are in direct contact with each other, suggesting that the rims accreted material from multiple reservoirs. Copyright (C) 2000 Elsevier Science Ltd.
• Lauretta, D. S., Devouard, B., & Buseck, P. R. (1999). The cosmochemical behavior of mercury. Earth and Planetary Science Letters, 171(1), 35-47.
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  Abstract: We review long-standing reports of both the 'Hg paradox' that Hg abundances in meteorites are inconsistent with its volatile behavior and the anomalous 196Hg/202Hg ratios in all types of extraterrestial material. A careful study of the literature suggests that both results may be due to overestimation of 202Hg abundances from neutron activation analysis. We reevaluate Hg condensation in the solar nebula using both volatility trends for chondritic meteorites and thermodynamic calculations. The extent of Hg depletion in Allende indicates a 50% condensation temperature of 350 K. Thermodynamic calculations show that Hg condenses into various metal alloys at 300 K or lower. At lower temperatures, Hg can be incorporated into Fe, Ni sulfides as a trace element. We investigate chemisorption as a method for incorporating Hg into solid material in the solar nebula. A large fraction of Hg can chemisorb on metal surfaces at temperatures as high as 515 K, depending on the grain size.
• Lauretta, D. S. (1998). Kamacite sulfurization in the solar nebula. Meteoritics and Planetary Science, 33(4), 821-833.
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  Abstract: The kinetics and mechanisms of kamacite sulfurization were studied experimentally at temperatures and H2S/H2 ratios relevant to the solar nebula. Pieces of the Canyon Diablo meteorite were heated at 558 K, 613 K, and 643 K in 50 parts per million by volume (ppmv) H2S-H2 gas mixtures for up to one month. Optical microscopy and x-ray diffraction analyses show that the morphology and crystal orientation of the resulting sulfide layers vary with both time and temperature. Electron microprobe analyses reveal three distinct phases in the reaction products: monosulfide solid solution (mss), (Fe, Ni, Co)i_xS, pentlandite (Fe, Ni, Co)9-xS8, and a P-rich phase. The bulk composition of the remnant metal was not significantly changed by sulfurization. Kamacite sulfurization at 558 K followed parabolic kinetics for the entire duration of the experiments. Sulfide layers that formed at 613 K grew linearly with time, while those that formed at 643 K initially grew linearly with time then switched to parabolic kinetics upon reaching a critical thickness. The experimental results suggest that a variety of thermodynamic, kinetic, and physical processes control the final composition and morphology of the sulfide layers. We combine morphological, x-ray diffraction, electron microprobe, and kinetic data to produce a comprehensive model of sulfide formation in the solar nebula. Then, we present a set of criteria to assist in the identification of solar nebula condensate sulfides in primitive meteorites. © Meteoritical Society, 1998.
• Lauretta, D. S., & Lodders, K. (1997). The cosmochemical behavior of beryllium and boron. Earth and Planetary Science Letters, 146(1-2), 315-327.
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  Abstract: The chemistry of Be and B in the solar nebula is reinvestigated using thermodynamic equilibrium calculations. The dominant Be gases are monatomic Be at high temperatures and the hydroxides BeOH and Be(OH)2 at lower temperatures. Beryllium condenses as gugiaite (Ca2BeSi2O7) in solid solution with melilite with a 50% condensation temperature of 1490 K. If an ideal solid solution of chrysoberyl (BeAl2O4) into spinel is assumed, most of the Be condenses into spinel, yielding a 50% condensation temperature of 1501 K. However, the difference in the crystal structures of spinel and chrysoberyl indicates that their solid solution may be non-ideal. At high temperatures the dominant B gases are BO, HBO, and HBO2, while NaBO2, KBO2, and LiBO2 are dominant at lower temperatures. Boron is less refractory than Be and is calculated to condense into solid solution with feldspar. The majority of B condenses as danburite (CaB2Si2O8) in solid solution with anorthite. At lower temperatures, when the feldspar composition is more albitic, the remaining B condenses as reedmergnerite (NaBSi3O8). The 50% condensation temperature of B is 964 K. The 50% condensation temperature of B is similar to that of Na and much higher than that of S. Therefore, normalized B abundances in chondrites are expected to correlate with Na abundances. Be is predicted to be concentrated in melilite, a conclusion which is consistent with the few measurements of Be concentrations in calcium aluminum-rich inclusions (CAIs). Boron is predicted to be concentrated in feldspar, but no analytical data are available to test this prediction.
• Lauretta, D. S., Lodders, K., & Fegley Jr., B. (1997). Experimental simulations of sulfide formation in the solar nebula. Science, 277(5324), 358-360.
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  PMID: 9219690;Abstract: Sulfurization of meteoritic metal in H2S-H2 gas produced three different sulfides: monosulfide solid solution [(Fe, Ni)(1-x)S], pentlandite [(Fe,Ni)(9-x)S8], and a phosphorus-rich sulfide. The corn position of the remnant metal was unchanged. These results are contrary to theoretical predictions that sulfide formation in the solar nebula produced troilite (FeS) and enriched the remaining metal in nickel. The experimental sulfides are chemically and morphologically similar to sulfide grains in the matrix of the Alais (class Cl) carbonaceous chondrite, suggesting that these meteoritic sulfides may be condensates from the solar nebula.
• Lauretta, D. S., Lodders, K., Fegley Jr., B., & Kremser, D. T. (1997). The origin of sulfide-rimmed metal grains in ordinary chondrites. Earth and Planetary Science Letters, 151(3-4), 289-301.
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  Abstract: We report results from an experimental study of sulfide chemistry during metamorphism on ordinary chondrite parent bodies. Artificial LL-chondrite material, composed of silicate, iron metal, and sulfide grains, was placed in sealed, evacuated silica tubes and heated to either 500°C or 900°C. These temperatures are representative peak metamorphic temperatures experienced by type 3 and type 6 ordinary chondrites, respectively. Rapid sulfur mobilization occurs during heating and results in the formation of sulfide rims around the metal grains and sulfur loss from the original sulfide crystals. The newly formed sulfide rims have two distinct layers that incorporate nearby silicate grains. We also observe narrow sulfide trails that follow silicate grain boundaries and connect separate sulfide-rimmed metal grains. The morphologies of the sulfide rims suggest that vapor transport is the main mechanism for sulfur mobilization. Sulfur loss is observed along cracks and crystal boundaries of the initial sulfide grains. After extensive reaction, patches of iron metal appear at the outer edges of the sulfide crystals and large pore spaces form throughout the original sulfides. The experimental metaf-sulfide assemblages resemble those found in low metamorphic grade ordinary chondrites. This suggests metamorphism is mainly responsible for the observed metal-sulfide textures in these chondrites. © 1997 Elsevier Science B.V.
• Lauretta, D. S., Kremser, D. T., & Fegley Jr., B. (1996). The rate of iron sulfide formation in the solar nebula. Icarus, 122(2), 288-315.
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  Abstract: The kinetics and mechanism of the reaction H2S(g) + Fe(s) = FeS(s) + H2(g) was studied at temperatures and compositions relevant to the solar nebula. Fe foils were heated at 558-1173 K in H2S/H2 gas mixtures (∼25 to ∼10,000 parts per million by volume (ppmv) H2S) at atmospheric pressure. Optical microscopy and X-ray diffraction show that the microstructures and preferred growth orientations of the Fe sulfide scales vary with temperature and H2S/H2 ratio. Initially, compact, uniformly oriented scales grow on the Fe metal. As sulfidation proceeds, the scales crack and finer grained, randomly oriented crystals grow between the metal and the initial sulfide scale. The composition of the scales varies from Fe0.90S to FeS with temperature and H2S/H2 ratio, in agreement with thermodynamic calculations. The weight gain and thickness change of the samples give nearly identical measures of the reaction progress. Sulfide layers formed in 25-100 ppmv H2S grow linearly with time. Iron sulfides formed in ∼1000 ppmv H2S originally grow linearly with time. Upon reaching a critical thickness growth follows parabolic kinetics. Iron sulfide formation in 10,000 ppmv H2S also follows parabolic kinetics. The linear rate equation for sulfidation of Fe grains (≤20 μm diameter) in the solar nebula is d(FeS)/dt = kfPH2S - kr PH2(cm hour-1). The forward and reverse rate constants are (cm hour-1 atm-1) kf = 5.6(±1.3)exp(-27950(±7280)/RT) and kr = 10.3(±1.0)exp(-92610(±350)/RT), respectively. The activation energies for the forward and reverse reactions are ∼28 kJ mole-1 and ∼93 kJ mole-1, respectively. FeS formation in the solar nebula is rapid (e.g., ∼200 years at 700 K and 10-3 bars total pressure for 20 μm diameter Fe grains) as predicted by simple collision theory models of FeS formation. © 1996 Academic Press, Inc.

Proceedings Publications

• Almeida, N., Russell, S., King, A., Zega, T., McCoy, T., Keller, L., Haenecour, P., Thompson, M., Thomas-Keprta, K. .., Le, L., Tu, V., Connolly, H., & Lauretta, D. (2024, mar). X-Ray Computed Tomography of Bennu Particle OREX-501054-0. In 55th Lunar and Planetary Science Conference, 3040.
• Aponte, J. C., Dworkin, J. P., Elsila, J. E., Glavin, D. P., Connolly, H. C., & Lauretta, D. S. (2024, apr). Two-Dimensional Gas Chromatography Analysis of Samples Returned from Asteroid Bennu by OSIRIS-REx. In EGU General Assembly Conference Abstracts.
• Aponte, J., S{\'eguin}, F., Siguelnitzky, A., Dworkin, J., Elsila, J., Glavin, D., Connolly, H., & Lauretta, D. (2024, mar). Smells Like Teen Spirit: Volatile Organic Compounds in Carbonaceous Chondrites. In 55th Lunar and Planetary Science Conference, 3040.
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• {Daly}, M., {Barnouin}, O., {Johnson}, C., {Bierhaus}, E., {Seabrook}, J., {Dickinson}, C., {Haltigin}, T., {Gaudreau}, D., {Brunet}, C., {Cunningham}, G., {Lauretta}, D., {Boynton}, W., , E. (2014, jul). The OSIRIS-REx laser altimeter (OLA): Development progress. In Asteroids, Comets, Meteors 2014.
• {Emery}, J., {Fernandez}, Y., {Kelley}, M., {Warden}, K., {Hergenrother}, C., {Lauretta}, D., {Drake}, M., {Campins}, H., , J. (2014, jul). Thermal infrared observations and thermophysical characterization of the OSIRIS-REx target asteroid (101955) Bennu. In Asteroids, Comets, Meteors 2014.
• {Hergenrother}, C., {Hill}, D., {Spitz}, A., {Barucci}, M., {Binzel}, R., {Beshore}, E., {Bottke}, W., {Brucato}, J., {Clark}, B., {Cloutis}, E., {Connolly}, H., {Delbo}, M., {Dotto}, E., {Ieva}, S., {Licandro}, J., {Nolan}, M., {Perna}, D., {Sandford}, S., {Takir}, D., , D. (2014, nov). Crowd-sourcing Near-Earth Asteroid Science with the OSIRIS-REx Target Asteroids! Program. In AAS/Division for Planetary Sciences Meeting Abstracts, 46.
• {Lauretta}, D. (2014, jul). Integrated science and engineering for the OSIRIS-REx asteroid sample return mission. In Asteroids, Comets, Meteors 2014.
• {Lauretta}, D. (2014, nov). The Physical, Geological, and Dynamical Nature of Asteroid (101955) Bennu - Target of OSIRIS-REx. In AAS/Division for Planetary Sciences Meeting Abstracts, 46.
• {Spitz}, A., {Dykhuis}, M., {Platts}, S., {Keane}, J., {Tanquary}, H., {Zellem}, R., {Hawley}, T., {Lauretta}, D., {Beshore}, E., {Bottke}, B., {Hergenrother}, C., {Dworkin}, J., {Patchell}, R., {Spitz}, S., , Z. (2014, nov). Communicating Science on YouTube and Beyond: OSIRIS-REx Presents 321Science!. In AAS/Division for Planetary Sciences Meeting Abstracts, 46.
• {Springmann}, A., {Taylor}, P., {Nolan}, M., {Howell}, E., {Brozovi?}, M., {Benner}, L., {Giorgini}, J., {Busch}, M., {Margot}, J., {Lee}, C., {Jao}, J., , D. (2014, nov). Radar-Derived Shape Model of Near-Earth Binary Asteroid System (285263) 1998 QE2. In AAS/Division for Planetary Sciences Meeting Abstracts, 46.
• {Subetto}, D., {Andronikov}, A., {Lauretta}, D., {Drosenko}, D., , L. (2014, may). Variation of trace element concentrations in a lake sediment sequence in the Al-YD transition zone (NW Russia). In EGU General Assembly Conference Abstracts, 16.
• {Takir}, D., {Clark}, B., {Lauretta}, D., {d'Aubigny}, C., {Hergenrother}, C., {Li}, J., , R. (2014, nov). Bidirectional Reflectance Distribution Functions For the OSIRIS-REx Target Asteroid (101955) Bennu. In AAS/Division for Planetary Sciences Meeting Abstracts, 46.
• {Tanquary}, H., {Sahr}, E., {Habib}, N., {Hawley}, C., {Weber}, N., {Boynton}, W., {Kinney-Spano}, E., , D. (2014, nov). Optimization of Sample Site Selection Imaging for OSIRIS-REx Using Asteroid Surface Analog Images. In AAS/Division for Planetary Sciences Meeting Abstracts, 46.
• Chesley SR, ., Nolan, M., Farnocchia, D., Milani, A., Emery, J., Vokrouhlicky, D., Lauretta, D., Taylor, P., Benner, L., Giorgini, J., & coauthors, 7. (2012, May). The Trajectory Dynamics of Near-Earth Asteroid 101955 (1999 RQ36). In Asteroids, Comets, Meteors 2012.
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  LPI Contribution No. 1667; id. 6470
• Lauretta, D., Barucci, M., Bierhaus, E., Brucato JR, ., Campins, H., Christensen, P., Clark, B., Connolly, H., Dotto, E., Dworkin, J., & coauthors, 1. (2012, May). The OSIRIS-REx Mission — Sample Acquisition Strategy and Evidence for the Nature of Regolith on Asteroid (101955) 1999 RQ36. In Asteroids, Comets, Meteors 2012.
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  LPI Contribution No. 1667; id. 6291
• Nolan, M., Magri, C., Benner, L., Giorgini, J., Hergenrother, C., Howell, E., Hudson, R., Lauretta, D., & Margot, J. (2012, May). The Shape of OSIRIS-REx Mission Target 1999 RQ36 from Radar and Lightcurve Data. In Asteroids, Comets, Meteors 2012.
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  LPI Contribution No. 1667; id. 6345

Presentations

• Nolan, M. C., Benner, L. A., Giorgini, J. D., Howell, E. S., Kerr, R., Lauretta, D. S., Magri, C., Margot, J. L., & Scheeres, D. J. (2017, December). Radar Observations of Asteroid 101955 Bennu and the OSIRIS-REx Sample Return Mission. 2017 Fall Meeting, AGU. New Orleans, LA: AGU.

Poster Presentations

• Andronikov, A.,  Lauretta, D.,  Hill, D., &  Andronikova, I. (2014, March). Chemical Composition of Metals and Sulfides from the Chelyabinsk Meteorite: Electron Microprobe and LA-ICP-MS Study. 45th Lunar and Planetary Science Conference. The Woodlands, TX.
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  Dates: 03/17-21/14; LPI Contribution No. 1777, p. 1407
• Bottke, W.,  Vokrouhlicky, D.,  Nesvorny, D.,  Walsh, K.,  Delbo, M.,  Lauretta, D., &  Connolly, H. (2014, Fall). OSIRIS-REx Team The Unusual Evolution of Billion-Year Old Asteroid Families by the Yarkovsky and YORP Effects. DPS meeting #45American Astronomical Society.
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  #106.06
• Brown, R., Lauretta, D., Schmidt, B., & Moores, J. (2014, Fall). Experimental and Theoretical Simulations of Ice Sublimation with Implications for the Chemical, Isotopic, and Physical Evolution of Icy Objects. Planetary and Space Science.
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  Volume: 60; Page: 166-180
• Chesley SR, ., Nolan, M., Farnocchia, D., Milani, A., Emery, J., Vokrouhlický, D., Lauretta, D., Taylor, P., Benner, L., Giorgini, J., & coauthors, 7. (2014, Fall). The Trajectory Dynamics of Near-Earth Asteroid 101955 (1999 RQ36). DDA meeting #43American Astronomical Society.
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  #7.08
• Davidson, J., Lauretta, D., & Schrader, D. (2014, Fall). Compositional Variations in Silicate Phases Within the CV and CK Carbonaceous Chondrites. 43rd Lunar and Planetary Science Conference.
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  Abstract #1494
• Emery, J.,  Kelley, M.,  Fernandez, Y.,  Hergenrother, C.,  Crane, K.,  Ziffer, J., Campins, H.,  Lauretta, D., &  Drake, M. (2014, Fall). Thermal and Physical Characterization of the OSIRIS-REx Target Asteroid (101955) 1999 RQ36. DPS meeting #44American Astronomical Society.
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  #102.05
• Gardner-Vandy, K., Lauretta, D., & McCoy, T. (2014, Fall). Formation History of the Brachinites: Partial Melts from an R Chondrite-Like Parent Body. 43rd Lunar and Planetary Science Conference.
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  Abstract #1610
• Gardner-Vandy, K., Lauretta, D., Greenwood, R., McCoy, T., Killgore, M., & Franchi, I. (2014, Fall). The Tafassasset Primitive Achondrite: Insights into Initial Stages of Planetary Differentiation. Geochimica et Cosmochimica Acta.
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  Volume: 85; Page: 142-159
• Hergenrother, C., Scheeres, D., Nolan, M., D'Aubigny, C., Barucci, M., Clark, B., Dotto, E., Emery, J., Lauretta, D., Licandro, J., & Rizk, B. (2014, Fall). Lightcurve and Phase Function Photometry of the OSIRIS-REx Target (101955) 1999 RQ36. 43rd Lunar and Planetary Science Conference.
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  Dates: Abstract #2219
• Lauretta, D., & Team, t. O. (2014, Fall). An Overview of the OSIRIS-REx Asteroid Sample Return Mission. 43rd Lunar and Planetary Science Conference.
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  Dates: Abstract #2491
• Messenger, S.,  Connolly, H.,  Lauretta, D., &  Bottke, W. (2014, March). Investigating the Geological History of Asteroid 101955 Bennu Through Remote Sensing and Returned Sample Analyses. 45th Lunar and Planetary Science Conference. The Woodlands, TX.
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  Dates: 03/17-21/14; LPI Contribution No. 1777, p. 1904
• Miller, K.,  Thompson, M.,  Lauretta, D., &  Zega, T. (2014, March). Conditions for Formation of Chalcopyrite in the Rumuruti Chondrites. 45th Lunar and Planetary Science Conference. The Woodlands, TX.
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  Dates: 03/17-21/14; LPI Contribution No. 1777, p. 1461
• Moores, J., Brown, R., Lauretta, D., Smith, P., & Riofrio, L. (2014, Fall). Experimental and theoretical simulation of sublimating dusty water ice with implications for D/H ratios of water ice on Comets and Mars. Planetary Science.
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  Volume: 1; Page: 2-28
• Nakamura-Messenger, K.,  Connolly, H., &  Lauretta, D. (2014, March). Osiris-Rex Science Team Strategy for Ranking the Science Value of the Surface of Asteroid 101955 Bennu for Sample Site Selection for OSIRIS-Rex. 45th Lunar and Planetary Science Conference. The Woodlands, TX.
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  Dates: 03/17-21/14; LPI Contribution No. 1777, p. 2023
• Nolan, M., Magri, C., Benner, L., Hergenrother, C., Howell, E., Hudson, R., Giorgini, J., Lauretta, D., & Margot, J. (2014, Fall). The Shape of OSIRIS-REx Mission Target 1999 RQ36 from RADAR and Lightcurve Data. DPS meeting #44American Astronomical Society.
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  #110.02
• Nolan, M.,  Magri, C.,  Benner, L.,  Hergenrother, C.,  Howell, E.,  Hudson, R., Giorgini, J.,  Lauretta, D., &  Margot, J. (2014, Fall). The Shape of OSIRIS-REx Mission Target 1999 RQ₃₆ from RADAR and Lightcurve Data.
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  #110.02
• Schrader, D., Connolly, H., Lauretta, D., Nagashima, K., Huss, G., Davidson, J., & Domanik, K. (2014, Fall). O-Isotope Composition of the Gas Present During Chondrule Formation as Recorded in CR Chondrites. 43rd Lunar and Planetary Science Conference.
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  Dates: Abstract #1627
• Thomas, I.,  Bowles, N.,  Donaldson, H. K.,  Connolly, H.,  Killgore, M., &  Lauretta, D. (2014, March). The Effects of Varying Environmental Conditions on the Emissivity Spectra of Meteorites. 45th Lunar and Planetary Science Conference. The Woodlands, TX.
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  Dates: 03/17-21/14; LPI Contribution No. 1777, p. 1989
• Andronikov, A.,  Lauretta, D.,  Connolly, H., &  Andronikova, I. (2013, March). Determination of Trace-Element Bulk Composition of Equilibrated Ordinary Chondrite Meteorite Samples by LA-ICP-MS Using Various Reference Materials. 44th Lunar and Planetary Science Conference. The Woodlands, TX.
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  Dates: 03/18-22/13; LPI Contribution No. 1719, p. 1603
• Berger, E.,  Lauretta, D.,  Zega, T., &  Keller, L. (2013, March). FIB-TEM Investigations of Fe-Ni-Sulfides in the CI Chondrites Alais and Orgueil. 44th Lunar and Planetary Science Conference. The Woodlands, TX.
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  Dates: 03/18-22/13; LPI Contribution No. 1719, p. 1615
• Davidson, J.,  Nagashima, K.,  Krot, A., &  Lauretta, D. (2013, March). Oxygen Isotopic Compositions of Magnetite and Chondrule Olivine in CK3 Carbonaceous Chondrites: Links to the CV3 Chondrites. 44th Lunar and Planetary Science Conference. The Woodlands, TX.
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  Dates: 03/18-22/13; LPI Contribution No. 1719, p. 2522
• Gardner-Vandy, K.,  McCoy, T.,  Corrigan, C.,  Lauretta, D., &  Benedix, G. (2013, March). Implications of R Chondrite Melting Experiments on the Formation of GRA 06128/9. 44th Lunar and Planetary Science Conference. The Woodlands, TX.
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  Dates: 03/18-22/13; LPI Contribution No. 1719, p. 2595
• Lauretta, D. S. (2013, April). Asteroids Coming to Earth – NASA Headquarters. Asteroids Coming to Earth – NASA Headquarters.
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  Date: 04/30
• Lauretta, D. S. (2013, February). University of Arizona President’s Distinguished Speaker Series. University of Arizona President’s Distinguished Speaker Series. Washington DC.
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  Date: 02/07
• Lauretta, D. S. (2013, February). Will Asteroids End the World? – TEDx Tucson. Will Asteroids End the World? – TEDx Tucson.
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  Date: 02/26
• Lauretta, D. S. (2013, March). House of Representatives Committee on Science, Space, and Technology. House of Representatives Committee on Science, Space, and Technology.
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  Date: 03/25
• Lauretta, D. S. (2013, March). White House Office of Science and Technology Policy Brown Bag. White House Office of Science and Technology Policy Brown Bag.
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  Date: 03/25
• Lauretta, D. S. (2013, May). Carnegie Institute of Science. Carnegie Institute of Science.
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  Date: 05/14
• Lauretta, D. S. (2013, May). NASA Headquarters Office of the Chief Technologist. NASA Headquarters Office of the Chief Technologist.
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  Date: 05/14
• Lauretta, D. S. (2013, May). National Academy of Engineering Regional Meeting. National Academy of Engineering Regional Meeting.
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  Date: 05/20
• Righter, K.,  Nakamura-Messnger, K., &  Lauretta, D. (2013, July/August). Osiris-Rex Curation Working Group Curation of OSIRIS-REx Asteroid Samples. 76th Annual Meeting of the Meteoritical Society. Edmonton, Canada.
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  Dates: 07/29/13 - 08/07/13
• Spitz, A.,  Hergenrother, C.,  Hill, D., &  Lauretta, D. (2013, March). OSIRIS-REx Target Asteroids! Involving the Public in Asteroid Research and Scientists with the Public. 44th Lunar and Planetary Science Conference. The Woodlands, TX.
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  Dates: 03/18-22/13; LPI Contribution No. 1719, p. 2934
• Thomas, I.,  Bowles, N.,  Connolly, H.,  Kilgore, M., &  Lauretta, D. (2013, September). The Effects of Varying Environmental Conditions on the Emission Spectra of Meteorites. European Planetary Science Congress. London, UK.
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  Dates: 09/08-13/13
• Walsh, K.,  Delbo, M.,  Bottke, W.,  Vokrouhlicky, D., &  Lauretta, D. (2013, March). Introducing the Eulalia and New Polana Families: Re-Assesing Primitive Asteroid Families in the Inner Main-Belt. 44th Lunar and Planetary Science Conference. The Woodlands, TX.
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  Dates: 03/18-22/13; LPI Contribution No. 1719, p. 2835
• Berger, E., Lauretta, D., & Keller, L. (2012, August). The Thermodynamic Properties of Cubanite. 75th Annual Meeting of the Meteoritical Society. Cairns, Australia.
• Boynton, W., Lauretta, D., Beshore, E., Barnouin, O., Bierhaus, E., Binzel, R., Christensen, P., Daly, M., Grindlay, J., Hamilton, V., & coauthors, 6. (2012, Fall). The OSIRIS-REx mission to RQ36: nature of the remote sensing observations. European Planetary Science Congress 2012.
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  Dates: – EPSC Abstracts Vol. 7 EPSC2012-875
• Kidd, J., Furfaro, R., Wibben, D., Hergenrother, C., & Lauretta, D. (2012, August). Mission Analysis for a Temporary Geocentric Asteroids. AIAA/AAS Astrodynamics Specialist Conference.
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  Dates: 08/13-16/12
• Lauretta, D. S. (2012, Fall). OSIRIS-REx, Spacefest IV. OSIRIS-REx, Spacefest IV.
• Lauretta, D. S. (2012, Fall). Panel Moderator, Asteroid Exploration Panel, Spacefest IV. Panel Moderator, Asteroid Exploration Panel, Spacefest IV.
• Lauretta, D. S. (2012, February). Arizona Engineer’s Week Banquet. Arizona Engineer’s Week Banquet.
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  Date: 02/21
• Lauretta, D. S. (2012, February). Science Downtown Sunday Lecture Series. Science Downtown Sunday Lecture Series.
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  Date: 02/12
• Lauretta, D. S. (2012, February). UA President’s Distinguished Speaker Series – Washington DC. UA President’s Distinguished Speaker Series – Washington DC.
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  Date: 02/07
• Lauretta, D. S. (2012, February). UA Science Café – Saddlebrooke. UA Science Café – Saddlebrooke.
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  Date: 02/16
• Lauretta, D. S. (2012, January). Steward Observatory Public Evening Lecture Series. Steward Observatory Public Evening Lecture Series.
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  Date: 01/30
• Lauretta, D. S. (2012, March). Association of American Universities Data Exchange. Association of American Universities Data Exchange.
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  Date: 03/12
• Lauretta, D. S. (2012, March). Tucson Festival Books – Science Café. Tucson Festival Books – Science Café.
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  Date: 03/11
• Lauretta, D. S. (2012, May). NASA Headquarters Science Mission Directorate Brown Bag Luncheon. NASA Headquarters Science Mission Directorate Brown Bag Luncheon.
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  Date: 05/24
• Lauretta, D. S. (2012, May). National Research Council Committee on Astrobiology and Planetary Science. National Research Council Committee on Astrobiology and Planetary Science.
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  Date: 05/25
• Lauretta, D. S. (2012, May). The OSIRIS-REx Mission – Sample Acquisition Strategy and Evidence for the Nature of Regolith on Asteroid 101955 (1999 RQ36). The OSIRIS-REx Mission – Sample Acquisition Strategy and Evidence for the Nature of Regolith on Asteroid 101955 (1999 RQ36).
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  Date: 05/16
• Lauretta, D. S. (2012, November). UA Homecoming Luncheon. UA Homecoming Luncheon.
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  Date: 11/09
• Lauretta, D. S. (2012, September). Ithaca College, Department of Physics Colloquium. Ithaca College, Department of Physics Colloquium.
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  Date: 09/13