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1. Constraining the Temperature of Impact Melt from the Mistastin Lake Impact Structure Using Zircon Crystal Structures

Author

Tolometti, G. D, Osinski, G. R, Neish, C. D, Grieve, R. A. F, and Erickson, T. M

Subjects
Space Sciences (General)
Abstract

Impact melt is a product of hyper-velocity impact events formed by the instantaneous melting of near-surface target rocks. Constraining the temperature of impact melt is vital to understanding its prograde heating and cooling history, which can have implications for inferring the environment of early Earth ~4.0 billion years ago when microbial life potentially arose. To date, only one datum on the initial impact melt temperature has been derived by Timms et al. These authors studied zirconia microstructures and crystallographic orientations that revealed the former presence of cubic zirconia, found in a black impact glass at the Mistastin Lake impact structure, Canada. The presence of cubic zirconia indicates a minimum temperature for the impact melt of >2370°C from the dissociation temperature of zircon to cubic zirconia and liquid SiO2. With only one temperature datum, it is still difficult to constrain the entire temperature range experienced during the impact melting process; from its instantaneous formation to thermal equilibrium with the “cold” clasts collected along the crater floor and walls. In addition, obtaining a temperature value from only one type of impactite limits the inferred temperature range, because each impactite experiences a different cooling history. In this study, we present a preliminary investigation of 61 zircon crystals, 14 of which are similar to those studied by Timms et al., from the Mistastin Lake impact structure. To acquire a more accurate temperature profile representative of impact melt, zircon crystals were collected from different types of impactites containing impact melt, including additional samples of the black impact glass studied by Timms et al.

Published
2020

2. Titan as Revealed by the Cassini Radar

Author

Lopes, R. M. C., Wall, S. D., Elachi, C., Birch, S. P. D., Corlies, P., Coustenis, A., Hayes, A. G., Hofgartner, J. D., Janssen, M. A., Kirk, R. L., LeGall, A., Lorenz, R. D., Lunine, J. I., Malaska, M. J., Mastroguiseppe, M., Mitri, G., Neish, C. D., Notarnicola, C., Paganelli, F., Paillou, P., Poggiali, V., Radebaugh, J., Rodriguez, S., Schoenfeld, A., Soderblom, J. M., Solomonidou, A., Stofan, E. R., Stiles, B. W., Tosi, F., Turtle, E. P., West, R. D., Wood, C. A., Zebker, H. A., Barnes, J. W., Casarano, D., Encrenaz, P., Farr, T., Grima, C., Hemingway, D., Karatekin, O., Lucas, A., Mitchell, K. L., Ori, G., Orosei, R., Ries, P., Riccio, D., Soderblom, L. A., and Zhang, Z.

Published
2019
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5. Terrestrial Analogues for Lunar Impact Melt Flows

Author

Neish, C. D, Hamilton, C. W, Hughes, S. S, Nawotniak, S. Kobs, Garry, W. B, Skok, J. R, Elphic, R. C, Schaefer, E, Carter, L. M, Bandfield, J. L, Osinski, G. R, Lim, D, and Heldmann, J. L

Subjects
Lunar And Planetary Science And Exploration
Abstract

Lunar impact melt deposits have unique physical properties. They have among the highest observed radar returns at S-Band (12.6 cm wavelength), implying that they are rough at the decimeter scale. However, they are also observed in high-resolution optical imagery to be quite smooth at the meter scale. These characteristics distinguish them from well-studied terrestrial analogues, such as Hawaiian pahoehoe and ʻa ʻa lava flows. The morphology of impact melt deposits can be related to their emplacement conditions, so understanding the origin of these unique surface properties will help to inform us as to the circumstances under which they were formed. In this work, we seek to find a terrestrial analogue for well-preserved lunar impact melt flows by examining fresh lava flows on Earth. We compare the radar return and high-resolution topographic variations of impact melt flows to terrestrial lava flows with a range of surface textures. The lava flows examined in this work range from smooth Hawaiian pahoehoe to transitional basaltic flows at Craters of the Moon (COTM) National Monument and Preserve in Idaho to rubbly and spiny pahoehoe-like flows at the recent eruption at Holuhraun in Iceland. The physical properties of lunar impact melt flows appear to differ from those of all the terrestrial lava flows studied in this work. This may be due to (a) differences in post-emplacement modification processes or (b) fundamental differences in the surface texture of the melt flows due to the melts' unique emplacement and/or cooling environment. Information about the surface properties of lunar impact melt deposits will be critical for future landed missions that wish to sample these materials.

Published
2016
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6. Bistatic Radar Observations of the Moon Using Mini-RF on LRO and the Arecibo Observatory

Author

Patterson, G. W, Stickle, A. M, Turner, F. S, Jensen, J. R, Bussey, D. B. J, Spudis, P, Espiritu, R. C, Schulze, R. C, Yocky, D. A, Wahl, D. E, Zimmerman, M, Cahill, J. T. S, Nolan, M, Carter, L, Neish, C. D, Raney, R. K, Thomson, B. J, Kirk, R, Thompson, T.W, Tise, B. L, Erteza, I. A, and Jakowatz, C. V

Subjects
Lunar And Planetary Science And Exploration, Geosciences (General)
Abstract

The Miniature Radio Frequency (Mini-RF) instrument aboard NASA's Lunar Reconnaissance Orbiter (LRO) is a hybrid dual-polarized synthetic aperture radar (SAR) that operated in concert with the Arecibo Observatory to collect bistatic radar data of the lunar nearside from 2012 to 2015. The purpose of this bistatic campaign was to characterize the radar scattering properties of the surface and near-surface, as a function of bistatic angle, for a variety of lunar terrains and search for a coherent backscatter opposition effect indicative of the presence of water ice. A variety of lunar terrain types were sampled over a range of incidence and bistatic angles; including mare, highland, pyroclastic, crater ejecta, and crater floor materials. Responses consistent with an opposition effect were observed for the ejecta of several Copernican-aged craters and the floor of the south-polar crater Cabeus. The responses of ejecta material varied by crater in a manner that suggests a relationship with crater age. The response for Cabeus was observed within the portion of its floor that is not in permanent shadow. The character of the response differs from that of crater ejecta and appears unique with respect to all other lunar terrains observed. Analysis of data for this region suggests that the unique nature of the response may indicate the presence of near-surface deposits of water ice.

Published
2016
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7. TandEM: Titan and Enceladus mission

Author

Coustenis, A., Atreya, S. K., Balint, T., Brown, R. H., Dougherty, M. K., Ferri, F., Fulchignoni, M., Gautier, D., Gowen, R. A., Griffith, C. A., Gurvits, L. I., Jaumann, R., Langevin, Y., Leese, M. R., Lunine, J. I., McKay, C. P., Moussas, X., Müller-Wodarg, I., Neubauer, F., Owen, T. C., Raulin, F., Sittler, E. C., Sohl, F., Sotin, C., Tobie, G., Tokano, T., Turtle, E. P., Wahlund, J.-E., Waite, J. H., Baines, K. H., Blamont, J., Coates, A. J., Dandouras, I., Krimigis, T., Lellouch, E., Lorenz, R. D., Morse, A., Porco, C. C., Hirtzig, M., Saur, J., Spilker, T., Zarnecki, J. C., Choi, E., Achilleos, N., Amils, R., Annan, P., Atkinson, D. H., Bénilan, Y., Bertucci, C., Bézard, B., Bjoraker, G. L., Blanc, M., Boireau, L., Bouman, J., Cabane, M., Capria, M. T., Chassefière, E., Coll, P., Combes, M., Cooper, J. F., Coradini, A., Crary, F., Cravens, T., Daglis, I. A., de Angelis, E., de Bergh, C., de Pater, I., Dunford, C., Durry, G., Dutuit, O., Fairbrother, D., Flasar, F. M., Fortes, A. D., Frampton, R., Fujimoto, M., Galand, M., Grasset, O., Grott, M., Haltigin, T., Herique, A., Hersant, F., Hussmann, H., Ip, W., Johnson, R., Kallio, E., Kempf, S., Knapmeyer, M., Kofman, W., Koop, R., Kostiuk, T., Krupp, N., Küppers, M., Lammer, H., Lara, L.-M., Lavvas, P., Le Mouélic, S., Lebonnois, S., Ledvina, S., Li, J., Livengood, T. A., Lopes, R. M., Lopez-Moreno, J.-J., Luz, D., Mahaffy, P. R., Mall, U., Martinez-Frias, J., Marty, B., McCord, T., Menor Salvan, C., Milillo, A., Mitchell, D. G., Modolo, R., Mousis, O., Nakamura, M., Neish, C. D., Nixon, C. A., Nna Mvondo, D., Orton, G., Paetzold, M., Pitman, J., Pogrebenko, S., Pollard, W., Prieto-Ballesteros, O., Rannou, P., Reh, K., Richter, L., Robb, F. T., Rodrigo, R., Rodriguez, S., Romani, P., Ruiz Bermejo, M., Sarris, E. T., Schenk, P., Schmitt, B., Schmitz, N., Schulze-Makuch, D., Schwingenschuh, K., Selig, A., Sicardy, B., Soderblom, L., Spilker, L. J., Stam, D., Steele, A., Stephan, K., Strobel, D. F., Szego, K., Szopa, C., Thissen, R., Tomasko, M. G., Toublanc, D., Vali, H., Vardavas, I., Vuitton, V., West, R. A., Yelle, R., and Young, E. F.

Published
2009
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8. Titan as Revealed by the Cassini Radar

Author

Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences, Lopes, R. M C, Wall, S. D, Elachi, C., Birch, S. P D, Corlies, P., Coustenis, A., Hayes, A. G, Hofgartner, J. D, Janssen, M. A, Kirk, R. L, LeGall, A., Lorenz, R. D, Lunine, J. I, Malaska, M. J, Mastroguiseppe, M., Mitri, G., Neish, C. D, Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences, Lopes, R. M C, Wall, S. D, Elachi, C., Birch, S. P D, Corlies, P., Coustenis, A., Hayes, A. G, Hofgartner, J. D, Janssen, M. A, Kirk, R. L, LeGall, A., Lorenz, R. D, Lunine, J. I, Malaska, M. J, Mastroguiseppe, M., Mitri, G., and Neish, C. D

Abstract

Titan was a mostly unknown world prior to the Cassini spacecraft’s arrival in July 2004. We review the major scientific advances made by Cassini’s Titan Radar Mapper (RADAR) during 13 years of Cassini’s exploration of Saturn and its moons. RADAR measurements revealed Titan’s surface geology, observed lakes and seas of mostly liquid methane in the polar regions, measured the depth of several lakes and seas, detected temporal changes on its surface, and provided key evidence that Titan contains an interior ocean. As a result of the Cassini mission, Titan has gone from an uncharted world to one that exhibits a variety of Earth-like geologic processes and surface-atmosphere interactions. Titan has also joined the ranks of “ocean worlds” along with Enceladus and Europa, which are prime targets for astrobiological research.

Published
2021

10. MP3 - A meteorology and physical properties package to explore air-sea interaction on Titan

Author

Lorenz, R. D., Stofan, E., Lunine, J. I., Zarnecki, J. C., Harri, A.-M., Karkoschka, E., Newman, C. E., Bierhaus, E. B., Clark, B. C., Yelland, M., Leese, M. R., Boldt, J., Darlington, E., Neish, C. D., Sotzen, K., Arvelo, J., Rasbach, C., Kretsch, W., Strohbehn, K., Grey, M., Mann, J., Zimmermann, H., and Reed, C.

Abstract

The exchange of mass, heat and momentum at the air:sea interface are profound influences on the terrestrial environment, affecting the intensity of hurricanes, the size of waves and lake-effect precipitation. Titan presents us with an opportunity to study these processes in a novel physical context, with a different sea, atmosphere and gravity. The MP3 instrument, under development for the proposed Discovery mission TiME (Titan Mare Explorer [1,2]) is an integrated suite of small, simple sensors that combines the function of traditional meteorology packages with liquid physical properties and depth-sounding : these latter functions follow the concept of - and indeed use spare elements from - the Huygens Surface Science Package (SSP,[3]). However, unlike Huygens’ brief and dynamic 3 hours of measurement, in TiME’s 6-Titan-day (96 Earth day) nominal mission enabled by radioisotope power, MP3 will have an unprecedented long-term measurement opportunity in one of the most evocative environments in the solar system, Titan’s sea Ligeia Mare.

Published
2012

11. Spectral properties of Titan's impact craters imply chemical weathering of its surface

Author

Neish, C. D., primary, Barnes, J. W., additional, Sotin, C., additional, MacKenzie, S., additional, Soderblom, J. M., additional, Le Mouélic, S., additional, Kirk, R. L., additional, Stiles, B. W., additional, Malaska, M. J., additional, Le Gall, A., additional, Brown, R. H., additional, Baines, K. H., additional, Buratti, B., additional, Clark, R. N., additional, and Nicholson, P. D., additional

Published
2015
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13. Cryovolcanism on Titan: New results from Cassini RADAR and VIMS

Author

Lopes, R. M. C., primary, Kirk, R. L., additional, Mitchell, K. L., additional, LeGall, A., additional, Barnes, J. W., additional, Hayes, A., additional, Kargel, J., additional, Wye, L., additional, Radebaugh, J., additional, Stofan, E. R., additional, Janssen, M. A., additional, Neish, C. D., additional, Wall, S. D., additional, Wood, C. A., additional, Lunine, J. I., additional, and Malaska, M. J., additional

Published
2013
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16. Initial results for the north pole of the Moon from Mini-SAR, Chandrayaan-1 mission

Author

Spudis, P. D., primary, Bussey, D. B. J., additional, Baloga, S. M., additional, Butler, B. J., additional, Carl, D., additional, Carter, L. M., additional, Chakraborty, M., additional, Elphic, R. C., additional, Gillis-Davis, J. J., additional, Goswami, J. N., additional, Heggy, E., additional, Hillyard, M., additional, Jensen, R., additional, Kirk, R. L., additional, LaVallee, D., additional, McKerracher, P., additional, Neish, C. D., additional, Nozette, S., additional, Nylund, S., additional, Palsetia, M., additional, Patterson, W., additional, Robinson, M. S., additional, Raney, R. K., additional, Schulze, R. C., additional, Sequeira, H., additional, Skura, J., additional, Thompson, T. W., additional, Thomson, B. J., additional, Ustinov, E. A., additional, and Winters, H. L., additional

Published
2010
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17. TandEM: Titan and Enceladus mission

Author

Coustenis, A., primary, Atreya, S. K., additional, Balint, T., additional, Brown, R. H., additional, Dougherty, M. K., additional, Ferri, F., additional, Fulchignoni, M., additional, Gautier, D., additional, Gowen, R. A., additional, Griffith, C. A., additional, Gurvits, L. I., additional, Jaumann, R., additional, Langevin, Y., additional, Leese, M. R., additional, Lunine, J. I., additional, McKay, C. P., additional, Moussas, X., additional, Müller-Wodarg, I., additional, Neubauer, F., additional, Owen, T. C., additional, Raulin, F., additional, Sittler, E. C., additional, Sohl, F., additional, Sotin, C., additional, Tobie, G., additional, Tokano, T., additional, Turtle, E. P., additional, Wahlund, J.-E., additional, Waite, J. H., additional, Baines, K. H., additional, Blamont, J., additional, Coates, A. J., additional, Dandouras, I., additional, Krimigis, T., additional, Lellouch, E., additional, Lorenz, R. D., additional, Morse, A., additional, Porco, C. C., additional, Hirtzig, M., additional, Saur, J., additional, Spilker, T., additional, Zarnecki, J. C., additional, Choi, E., additional, Achilleos, N., additional, Amils, R., additional, Annan, P., additional, Atkinson, D. H., additional, Bénilan, Y., additional, Bertucci, C., additional, Bézard, B., additional, Bjoraker, G. L., additional, Blanc, M., additional, Boireau, L., additional, Bouman, J., additional, Cabane, M., additional, Capria, M. T., additional, Chassefière, E., additional, Coll, P., additional, Combes, M., additional, Cooper, J. F., additional, Coradini, A., additional, Crary, F., additional, Cravens, T., additional, Daglis, I. A., additional, de Angelis, E., additional, de Bergh, C., additional, de Pater, I., additional, Dunford, C., additional, Durry, G., additional, Dutuit, O., additional, Fairbrother, D., additional, Flasar, F. M., additional, Fortes, A. D., additional, Frampton, R., additional, Fujimoto, M., additional, Galand, M., additional, Grasset, O., additional, Grott, M., additional, Haltigin, T., additional, Herique, A., additional, Hersant, F., additional, Hussmann, H., additional, Ip, W., additional, Johnson, R., additional, Kallio, E., additional, Kempf, S., additional, Knapmeyer, M., additional, Kofman, W., additional, Koop, R., additional, Kostiuk, T., additional, Krupp, N., additional, Küppers, M., additional, Lammer, H., additional, Lara, L.-M., additional, Lavvas, P., additional, Le Mouélic, S., additional, Lebonnois, S., additional, Ledvina, S., additional, Li, J., additional, Livengood, T. A., additional, Lopes, R. M., additional, Lopez-Moreno, J.-J., additional, Luz, D., additional, Mahaffy, P. R., additional, Mall, U., additional, Martinez-Frias, J., additional, Marty, B., additional, McCord, T., additional, Menor Salvan, C., additional, Milillo, A., additional, Mitchell, D. G., additional, Modolo, R., additional, Mousis, O., additional, Nakamura, M., additional, Neish, C. D., additional, Nixon, C. A., additional, Nna Mvondo, D., additional, Orton, G., additional, Paetzold, M., additional, Pitman, J., additional, Pogrebenko, S., additional, Pollard, W., additional, Prieto-Ballesteros, O., additional, Rannou, P., additional, Reh, K., additional, Richter, L., additional, Robb, F. T., additional, Rodrigo, R., additional, Rodriguez, S., additional, Romani, P., additional, Ruiz Bermejo, M., additional, Sarris, E. T., additional, Schenk, P., additional, Schmitt, B., additional, Schmitz, N., additional, Schulze-Makuch, D., additional, Schwingenschuh, K., additional, Selig, A., additional, Sicardy, B., additional, Soderblom, L., additional, Spilker, L. J., additional, Stam, D., additional, Steele, A., additional, Stephan, K., additional, Strobel, D. F., additional, Szego, K., additional, Szopa, C., additional, Thissen, R., additional, Tomasko, M. G., additional, Toublanc, D., additional, Vali, H., additional, Vardavas, I., additional, Vuitton, V., additional, West, R. A., additional, Yelle, R., additional, and Young, E. F., additional

Published
2008
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18. Global distribution of lunar impact melt flows.

Author

Neish, C. D., Madden, J., Carter, L. M., Hawke, B. R., Giguere, T., Bray, V. J., Osinski, G. R., and Cahill, J. T. S.

Subjects
*LUNAR craters, *ASTROPHYSICAL collisions, *SURFACE topography, *MELT processing (Manufacturing process), *CIRCULAR polarization, *LUNAR surface
Abstract

In this study, we analyzed the distribution and properties of 146 craters with impact melt deposits exterior to their rims. Many of these craters were only recently discovered due to their unusual radar properties in the near-global Mini-RF data set. We find that most craters with exterior deposits of impact melt are small, ⩽20km, and that the smallest craters have the longest melt flows relative to their size. In addition, exterior deposits of impact melt are more common in the highlands than the mare. This may be the result of differing target properties in the highlands and mare, the difference in titanium content, or the greater variation of topography in the highlands. We find that 80% of complex craters and 60% of simple craters have melt directions that are coincident or nearly coincident with the lowest point in their rim, implying that pre-existing topography plays a dominant role in melt emplacement. This is likely due to movement during crater modification (complex craters) or breached crater rims (simple craters). We also find that impact melt flows have very high circular polarization ratios compared to other features on the Moon. This suggests that their surfaces are some of the roughest material on the Moon at the centimeter to decimeter scale, even though they appear smooth at the meter scale. [ABSTRACT FROM AUTHOR]

Published
2014
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19. Evolution of the Cote Creek Impact Melt Deposit at the Kamestastin Lake Impact Structure.

Author

Tolometti, G. D., Osinski, G. R., Erickson, T. M., and Neish, C. D.

Subjects
LAKE sediments, BRECCIA, MICROPROBE analysis, IMPACT craters, TURBULENT mixing, MELTING, SHORELINES
Abstract

Introduction: The thermal evolution of impact melt distributed and emplaced in different settings across an impact crater remains a topic of debate. Impact melt thermal evolution is an important story for understanding how impact melt devolatilized early crustal material [1], how impact melt cooled during and after deposition [2], and the solubility of elements essential for crustal differentiation [3]. The preferred approach to deconstruct the thermal evolution of impact melt is to constrain pressure and temperature conditions preserved within the microstructures and crystallographic orientations of accessory minerals zircon (ZrSiO4) and zirconia (ZrO2) [e.g., 4-6]. Recent work by [4] and [5] discovered that impact melt at the Kamestastin (Mistastin) Lake impact structure in Labrador, Canada exceeded temperatures >2370 °C, based off cubic zirconia phase orientations within baddeleyite. These superheated temperatures are vital information for understanding the early P-T conditions of impact melt formation, which is a period of the impact cratering process that is rarely preserved. To date, we only have recordings of these superheated temperatures from one sample, from one locality, within a single crater. Therefore, a question that stands is can we identify more recordings of these superheated temperatures and specific moments in impact melt cooling within an impact structures impactite stratigraphy. To address this, we seek to constrain the thermal evolution of the wellexposed impact melt deposit named Cote Creek, located near the northwest shoreline of the Kamestastin Lake impact structure, Labrador, Canada. We will study the thermal evolution of the Cote Creek deposit by analyzing the composition and petrography of the impact melt moving up the impactite stratigraphy and the diagnostic shock microstructures and crystallographic orientations of zircon grain and zirconia crystals encased in impact melt matrices. The impactite stratigraphy contains a collection of melt-poor and melt-rich impactites, including (base ? top) meltfree polymict breccias, impact melt-bearing breccias, clast-rich impact melt rocks, and a clast-poor fine-grained impact melt rock. Impactite Stratigraphy Petrography: We collected impact melt-bearing samples from three sub-vertical transects at the Cote Creek locality during a field deployment to Kamestastin Lake in September 2021. Our petrographic analysis agrees with observations reported by previous workers at Kamestastin Lake impactites [7,8]; impact melt crystallinity increases moving up from the melt-free polymict breccias and target rocks, and petrographic textures transition from glassy-aphanitic to porphyritic in the clast-poor impact melt rock samples. In samples acquired from a contact between the clast-rich impact melt rock and the impact melt-bearing breccias, known as the "transition zone," we discovered three different impact melt textures: (1) cm-sized particles of deep brown impact glass, (2) black aphanitic impact melt, and (3) aphanitic-trachylitic impact melt. We interpret that this zone represents a region where clast content drops drastically and transitions from a clast-dominated impact melt-bearing breccia to an impact melt rock. The presence of flow textures within the transition zone also suggests turbulent mixing, where the multiple impact melts quenched before complete homogenization could occur. Geochemical and P-T Analysis: We are investigating the composition of the impact melt moving up the impactite stratigraphy using both qualitative and quantitative methods. Using a Bruker M4 Tornado micro-x-ray fluorescence (XRF) instrument, we have acquired elemental maps of the impactite thin sections. Preliminary results show the major elemental composition of the Cote Creek impact melt to be homogenous, with the exception of localized pockets of impact melt exhibiting elevated concentrations of alkali elements (Na and K) and Si. These enrichments are the result of clasts not fully assimilating into the melt. The micro-XRF data also provides context for wave-dispersive spectroscopy (WDS) analysis, which will provide quantitative elemental information on the impact melt samples. Using an electron micro-probe analysis (EMPA) instrument and XRF zirconium maps, we have identified zircon grains in each impact melt-bearing impactite located in the Cote Creek outcrop. Our initial findings include the identification of fully granular zircon grains and partially granular zircon grains with lamellae-like textures. We will be analyzing the microstructures and phase heritage of these zircon grains using electron backscatter diffraction (EBSD), which will provide constrains on the P-T conditions of each impactite sample. [ABSTRACT FROM AUTHOR]

Published
2022

29. SEEING PāHOEHOE FROM ORBIT (WITHOUT SQUINTING).

Author

Schaefer, E. I., Hamilton, C. W., Neish, C. D., Sori, M. M., Bramson, A. M., Beard, S. P., Peters, S. I., Miller, T. A., and Rader, E. L.

Subjects
VOLCANOLOGY, GLOBAL Positioning System, RHEOLOGY
Published
2017

32. MP3 - A meteorology and physical properties package to explore air-sea interaction on Titan

Author

Lorenz, R. D., Stofan, E., Lunine, J. I., Zarnecki, J. C., Harri, A.-M., Karkoschka, E., Newman, C. E., Bierhaus, E. B., Clark, B. C., Yelland, M., Leese, M. R., Boldt, J., Darlington, E., Neish, C. D., Sotzen, K., Arvelo, J., Rasbach, C., Kretsch, W., Strohbehn, K., Grey, M., Mann, J., Zimmermann, H., Reed, C., Lorenz, R. D., Stofan, E., Lunine, J. I., Zarnecki, J. C., Harri, A.-M., Karkoschka, E., Newman, C. E., Bierhaus, E. B., Clark, B. C., Yelland, M., Leese, M. R., Boldt, J., Darlington, E., Neish, C. D., Sotzen, K., Arvelo, J., Rasbach, C., Kretsch, W., Strohbehn, K., Grey, M., Mann, J., Zimmermann, H., and Reed, C.

Abstract

The exchange of mass, heat and momentum at the air:sea interface are profound influences on the terrestrial environment, affecting the intensity of hurricanes, the size of waves and lake-effect precipitation. Titan presents us with an opportunity to study these processes in a novel physical context, with a different sea, atmosphere and gravity. The MP3 instrument, under development for the proposed Discovery mission TiME (Titan Mare Explorer [1,2]) is an integrated suite of small, simple sensors that combines the function of traditional meteorology packages with liquid physical properties and depth-sounding : these latter functions follow the concept of - and indeed use spare elements from - the Huygens Surface Science Package (SSP,[3]). However, unlike Huygens’ brief and dynamic 3 hours of measurement, in TiME’s 6-Titan-day (96 Earth day) nominal mission enabled by radioisotope power, MP3 will have an unprecedented long-term measurement opportunity in one of the most evocative environments in the solar system, Titan’s sea Ligeia Mare.

33. A mission control architecture for robotic lunar sample return as field tested in an analogue deployment to the Sudbury impact structure

Author

Moores, John E., Francis, Raymond, Mader, Marianne, Osinski, G. R., Barfoot, T., Barry, N., Basic, G., Battler, M., Beauchamp, M., Blain, S., Bondy, M., Capitan, R-D., Chanou, A., Clayton, J., Cloutis, E., Daly, M., Dickinson, C., Dong, H., Flemming, R., Furgale, P., Gammel, J., Gharfoor, N., Hussein, M., Grieve, R., Henrys, H., Jaziobedski, P., Lambert, A., Leung, K., Marion, C., McCullough, E., McManus, C., Neish, C. D., Ng, H. K., Ozaruk, A., Pickersgill, A., Preston, L. J., Redman, D., Sapers, H., Shankar, B., Singleton, A., Souders, K., Stenning, B., Stooke, P., Sylvester, P., Tornabene, L., Moores, John E., Francis, Raymond, Mader, Marianne, Osinski, G. R., Barfoot, T., Barry, N., Basic, G., Battler, M., Beauchamp, M., Blain, S., Bondy, M., Capitan, R-D., Chanou, A., Clayton, J., Cloutis, E., Daly, M., Dickinson, C., Dong, H., Flemming, R., Furgale, P., Gammel, J., Gharfoor, N., Hussein, M., Grieve, R., Henrys, H., Jaziobedski, P., Lambert, A., Leung, K., Marion, C., McCullough, E., McManus, C., Neish, C. D., Ng, H. K., Ozaruk, A., Pickersgill, A., Preston, L. J., Redman, D., Sapers, H., Shankar, B., Singleton, A., Souders, K., Stenning, B., Stooke, P., Sylvester, P., and Tornabene, L.

Abstract

A Mission Control Architecture is presented for a Robotic Lunar Sample Return Mission which builds upon the experience of the landed missions of the NASA Mars Exploration Program. This architecture consists of four separate processes working in parallel at Mission Control and achieving buy-in for plans sequentially instead of simultaneously from all members of the team. These four processes were: Science Processing, Science Interpretation, Planning and Mission Evaluation. Science Processing was responsible for creating products from data downlinked from the field and is organized by instrument. Science Interpretation was responsible for determining whether or not science goals are being met and what measurements need to be taken to satisfy these goals. The Planning process, responsible for scheduling and sequencing observations, and the Evaluation process that fostered inter-process communications, reporting and documentation assisted these processes. This organization is advantageous for its flexibility as shown by the ability of the structure to produce plans for the rover every two hours, for the rapidity with which Mission Control team members may be trained and for the relatively small size of each individual team. This architecture was tested in an analogue mission to the Sudbury impact structure from June 6-17, 2011. A rover was used which was capable of developing a network of locations that could be revisited using a teach and repeat method. This allowed the science team to process several different outcrops in parallel, downselecting at each stage to ensure that the samples selected for caching were the most representative of the site. Over the course of 10 days, 18 rock samples were collected from 5 different outcrops, 182 individual field activities - such as roving or acquiring an image mosaic or other data product - were completed within 43 command cycles, and the rover travelled over 2,200 m. Data transfer from communications passes were filled to 74%

34. MP3 - A meteorology and physical properties package to explore air-sea interaction on Titan

Author

Lorenz, R. D., Stofan, E., Lunine, J. I., Zarnecki, J. C., Harri, A.-M., Karkoschka, E., Newman, C. E., Bierhaus, E. B., Clark, B. C., Yelland, M., Leese, M. R., Boldt, J., Darlington, E., Neish, C. D., Sotzen, K., Arvelo, J., Rasbach, C., Kretsch, W., Strohbehn, K., Grey, M., Mann, J., Zimmermann, H., Reed, C., Lorenz, R. D., Stofan, E., Lunine, J. I., Zarnecki, J. C., Harri, A.-M., Karkoschka, E., Newman, C. E., Bierhaus, E. B., Clark, B. C., Yelland, M., Leese, M. R., Boldt, J., Darlington, E., Neish, C. D., Sotzen, K., Arvelo, J., Rasbach, C., Kretsch, W., Strohbehn, K., Grey, M., Mann, J., Zimmermann, H., and Reed, C.

Abstract

The exchange of mass, heat and momentum at the air:sea interface are profound influences on the terrestrial environment, affecting the intensity of hurricanes, the size of waves and lake-effect precipitation. Titan presents us with an opportunity to study these processes in a novel physical context, with a different sea, atmosphere and gravity. The MP3 instrument, under development for the proposed Discovery mission TiME (Titan Mare Explorer [1,2]) is an integrated suite of small, simple sensors that combines the function of traditional meteorology packages with liquid physical properties and depth-sounding : these latter functions follow the concept of - and indeed use spare elements from - the Huygens Surface Science Package (SSP,[3]). However, unlike Huygens’ brief and dynamic 3 hours of measurement, in TiME’s 6-Titan-day (96 Earth day) nominal mission enabled by radioisotope power, MP3 will have an unprecedented long-term measurement opportunity in one of the most evocative environments in the solar system, Titan’s sea Ligeia Mare.

35. A mission control architecture for robotic lunar sample return as field tested in an analogue deployment to the Sudbury impact structure

Author

Moores, John E., Francis, Raymond, Mader, Marianne, Osinski, G. R., Barfoot, T., Barry, N., Basic, G., Battler, M., Beauchamp, M., Blain, S., Bondy, M., Capitan, R-D., Chanou, A., Clayton, J., Cloutis, E., Daly, M., Dickinson, C., Dong, H., Flemming, R., Furgale, P., Gammel, J., Gharfoor, N., Hussein, M., Grieve, R., Henrys, H., Jaziobedski, P., Lambert, A., Leung, K., Marion, C., McCullough, E., McManus, C., Neish, C. D., Ng, H. K., Ozaruk, A., Pickersgill, A., Preston, L. J., Redman, D., Sapers, H., Shankar, B., Singleton, A., Souders, K., Stenning, B., Stooke, P., Sylvester, P., Tornabene, L., Moores, John E., Francis, Raymond, Mader, Marianne, Osinski, G. R., Barfoot, T., Barry, N., Basic, G., Battler, M., Beauchamp, M., Blain, S., Bondy, M., Capitan, R-D., Chanou, A., Clayton, J., Cloutis, E., Daly, M., Dickinson, C., Dong, H., Flemming, R., Furgale, P., Gammel, J., Gharfoor, N., Hussein, M., Grieve, R., Henrys, H., Jaziobedski, P., Lambert, A., Leung, K., Marion, C., McCullough, E., McManus, C., Neish, C. D., Ng, H. K., Ozaruk, A., Pickersgill, A., Preston, L. J., Redman, D., Sapers, H., Shankar, B., Singleton, A., Souders, K., Stenning, B., Stooke, P., Sylvester, P., and Tornabene, L.

Abstract

A Mission Control Architecture is presented for a Robotic Lunar Sample Return Mission which builds upon the experience of the landed missions of the NASA Mars Exploration Program. This architecture consists of four separate processes working in parallel at Mission Control and achieving buy-in for plans sequentially instead of simultaneously from all members of the team. These four processes were: Science Processing, Science Interpretation, Planning and Mission Evaluation. Science Processing was responsible for creating products from data downlinked from the field and is organized by instrument. Science Interpretation was responsible for determining whether or not science goals are being met and what measurements need to be taken to satisfy these goals. The Planning process, responsible for scheduling and sequencing observations, and the Evaluation process that fostered inter-process communications, reporting and documentation assisted these processes. This organization is advantageous for its flexibility as shown by the ability of the structure to produce plans for the rover every two hours, for the rapidity with which Mission Control team members may be trained and for the relatively small size of each individual team. This architecture was tested in an analogue mission to the Sudbury impact structure from June 6-17, 2011. A rover was used which was capable of developing a network of locations that could be revisited using a teach and repeat method. This allowed the science team to process several different outcrops in parallel, downselecting at each stage to ensure that the samples selected for caching were the most representative of the site. Over the course of 10 days, 18 rock samples were collected from 5 different outcrops, 182 individual field activities - such as roving or acquiring an image mosaic or other data product - were completed within 43 command cycles, and the rover travelled over 2,200 m. Data transfer from communications passes were filled to 74%

36. Titan as Revealed by the Cassini Radar

Author

Federico Tosi, L. A. Soderblom, Charles Elachi, G. Mitri, Zhimeng Zhang, Alexander G. Hayes, S. D. Wall, Jason M. Soderblom, P. Paillou, Elizabeth P. Turtle, Richard West, R. L. Kirk, Gian Gabriele Ori, Tom G. Farr, Howard A. Zebker, Claudia Notarnicola, Paul Corlies, M. Mastroguiseppe, Jason W. Barnes, Antoine Lucas, K. L. Mitchell, Jason D. Hofgartner, Bryan Stiles, Athena Coustenis, Valerio Poggiali, A. Solomonidou, Cyril Grima, Roberto Orosei, O. Karatekin, E. R. Stofan, Jani Radebaugh, Spd Birch, Rmc Lopes, Domenico Casarano, A. LeGall, P Encrenaz, Michael Malaska, Charles A. Wood, Flora Paganelli, Douglas J. Hemingway, Daniele Riccio, Sebastien Rodriguez, Catherine D. Neish, M. A. Janssen, R. D. Lorenz, Paul Ries, Jonathan I. Lunine, Ashley Schoenfeld, Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Department of Astronomy [Ithaca], Cornell University, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Astrogeology Science Center [Flagstaff], United States Geological Survey [Reston] (USGS), University of Arizona, Lunar and Planetary Laboratory [Tucson] (LPL), Università degli Studi di Roma 'La Sapienza' [Rome], Laboratoire de Planétologie et Géodynamique UMR6112 (LPG), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université de Nantes - Faculté des Sciences et des Techniques, Université de Nantes (UN)-Université de Nantes (UN)-Université d'Angers (UA), Florida Institute of Technology [Melbourne], Institut de génétique humaine (IGH), Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Service de cardiologie [Hôpital Nord - APHM], Aix Marseille Université (AMU)-Assistance Publique - Hôpitaux de Marseille (APHM)- Hôpital Nord [CHU - APHM], Observatoire Bordeaux, Université Sciences et Technologies - Bordeaux 1, Department of Geological Sciences [BYU], Brigham Young University (BYU), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Department of Earth, Planetary and Space Sciences [Los Angeles] (EPSS), University of California [Los Angeles] (UCLA), University of California-University of California, Proxemy Research Inc, Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), Wheeling Jesuit University, Department of Electrical Engineering [Stanford], Stanford University [Stanford], Istituto di Ricerca per la Protezione Idrogeologica [Bari] (IRPI), Consiglio Nazionale delle Ricerche [Roma] (CNR), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS Paris)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Swedish Institute of Space Physics [Uppsala] (IRF), Miller Institute for Basic Research in Science, University of California [Berkeley], Royal Observatory of Belgium [Brussels], Institut de Physique du Globe de Paris (IPGP), Institut national des sciences de l'Univers (INSU - CNRS)-IPG PARIS-Université Paris Diderot - Paris 7 (UPD7)-Université de La Réunion (UR)-Centre National de la Recherche Scientifique (CNRS), International Research School of Planetary Sciences [Pescara] (IRSPS), Università degli studi 'G. d'Annunzio' Chieti-Pescara [Chieti-Pescara] (Ud'A), Istituto di Fisica dello Spazio Interplanetario (IFSI), Consiglio Nazionale delle Ricerche (CNR), Division of Geological and Planetary Sciences [Pasadena], California Institute of Technology (CALTECH), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), IMPEC - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Department of Earth Sciences [London, ON], University of Western Ontario (UWO), Institute for Earth Observation [Bolzano], EURAC Research, Search for Extraterrestrial Intelligence Institute (SETI), ASP 2019, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Université de La Réunion (UR)-Université Paris Diderot - Paris 7 (UPD7)-IPG PARIS-Institut national des sciences de l'Univers (INSU - CNRS), Department of Earth, Atmospheric and Planetary Sciences [MIT, Cambridge] (EAPS), Massachusetts Institute of Technology (MIT), European Space Astronomy Centre (ESAC), European Space Agency (ESA), Smithsonian National Air and Space Museum, Smithsonian Institution, Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Planetary Science Institute [Tucson] (PSI), Department of Physics [Moscow,USA], University of Idaho [Moscow, USA], Istituto di Ricerca per la Protezione Idrogeologica [Padova] (IRPI), Institute of Geophysics [Austin] (IG), University of Texas at Austin [Austin], Istituto di Radioastronomia (IRA), Dipartimento di Ingegneria Elettrica e delle Tecnologie dell'Informazione [Napoli] (DIETI), Università degli studi di Napoli Federico II, Cornell University [New York], Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), PLANETO - LATMOS, Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome], European Academy Bozen/Bolzano (EURAC), Stanford University, Royal Observatory of Belgium [Brussels] (ROB), Istituto di Radioastronomia [Bologna] (IRA), Lopes, R. M. C., Wall, S. D., Elachi, C., Birch, S. P. D., Corlies, P., Coustenis, A., Hayes, A. G., Hofgartner, J. D., Janssen, M. A., Kirk, R. L., Legall, A., Lorenz, R. D., Lunine, J. I., Malaska, M. J., Mastroguiseppe, M., Mitri, G., Neish, C. D., Notarnicola, C., Paganelli, F., Paillou, P., Poggiali, V., Radebaugh, J., Rodriguez, S., Schoenfeld, A., Soderblom, J. M., Solomonidou, A., Stofan, E. R., Stiles, B. W., Tosi, F., Turtle, E. P., West, R. D., Wood, C. A., Zebker, H. A., Barnes, J. W., Casarano, D., Encrenaz, P., Farr, T., Grima, C., Hemingway, D., Karatekin, O., Lucas, A., Mitchell, K. L., Ori, G., Orosei, R., Ries, P., Riccio, D., Soderblom, L. A., Zhang, Z., ITA, USA, FRA, and Hôpital Nord [CHU - APHM]-Assistance Publique - Hôpitaux de Marseille (APHM)-Aix Marseille Université (AMU)

Subjects
Exploration of Saturn, 010504 meteorology & atmospheric sciences, [SDU.STU.GP]Sciences of the Universe [physics]/Earth Sciences/Geophysics [physics.geo-ph], [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], 01 natural sciences, Liquid methane, law.invention, Astrobiology, symbols.namesake, [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, law, 0103 physical sciences, [SDU.STU.GM]Sciences of the Universe [physics]/Earth Sciences/Geomorphology, Radar, Enceladus, [SDU.ENVI]Sciences of the Universe [physics]/Continental interfaces, environment, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astronomy and Astrophysics, Cassini, radar, Titan, Planetary science, 13. Climate action, Space and Planetary Science, symbols, Titan (rocket family), Geology
Abstract

International audience; Titan was a mostly unknown world prior to the Cassini spacecraft’s arrival in July 2004. We review the major scientific advances made by Cassini’s Titan Radar Mapper (RADAR) during 13 years of Cassini’s exploration of Saturn and its moons. RADAR measurements revealed Titan’s surface geology, observed lakes and seas of mostly liquid methane in the polar regions, measured the depth of several lakes and seas, detected temporal changes on its surface, and provided key evidence that Titan contains an interior ocean. As a result of the Cassini mission, Titan has gone from an uncharted world to one that exhibits a variety of Earth-like geologic processes and surface-atmosphere interactions. Titan has also joined the ranks of “ocean worlds” along with Enceladus and Europa, which are prime targets for astrobiological research.

Published
2019
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37. Rate measurements of the hydrolysis of complex organic macromolecules in cold aqueous solutions: implications for prebiotic chemistry on the early Earth and Titan.

Author

Neish CD, Somogyi A, Imanaka H, Lunine JI, and Smith MA

Subjects
Calibration, Hydrolysis, Kinetics, Mass Spectrometry, Reference Standards, Solutions, Water, Cold Temperature, Earth, Planet, Macromolecular Substances analysis, Saturn
Abstract

Organic macromolecules ("complex tholins") were synthesized from a 0.95 N(2)/0.05 CH(4) atmosphere in a high-voltage AC flow discharge reactor. When placed in liquid water, specific water soluble compounds in the macromolecules demonstrated Arrhenius type first order kinetics between 273 and 313 K and produced oxygenated organic species with activation energies in the range of approximately 60+/-10 kJ mol(-1). These reactions displayed half lives between 0.3 and 17 days at 273 K. Oxygen incorporation into such materials--a necessary step toward the formation of biological molecules--is therefore fast compared to processes that occur on geologic timescales, which include the freezing of impact melt pools and possible cryovolcanic sites on Saturn's organic-rich moon Titan.

Published
2008
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