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95 results on '"Leese, M. R."'

1. Dust measurements in the coma of comet 67P/Churyumov-Gerasimenko inbound to the Sun

Author

Rotundi, A., Sierks, H., Corte, V. Della, Fulle, M., Gutierrez, P. J., Lara, L., Barbieri, C., Lamy, P. L., Rodrigo, R., Koschny, D., Rickman, H., Keller, H. U., López-Moreno, J. J., Accolla, M., Agarwal, J., A'Hearn, M. F., Altobelli, N., Angrilli, F., Barucci, M. A., Bertaux, J.-L., Bertini, I., Bodewits, D., Bussoletti, E., Colangeli, L., Cosi, M., Cremonese, G., Crifo, J.-F., Da Deppo, V., Davidsson, B., Debei, S., De Cecco, M., Esposito, F., Ferrari, M., Fornasier, S., Giovane, F., Gustafson, B., Green, S. F., Groussin, O., Grün, E., Güttler, C., Herranz, M. L., Hviid, S. F., Ip, W., Ivanovski, S., Jerónimo, J. M., Jorda, L., Knollenberg, J., Kramm, R., Kührt, E., Küppers, M., Lazzarin, M., Leese, M. R., López-Jiménez, A. C., Lucarelli, F., Lowry, S. C., Marzari, F., Epifani, E. Mazzotta, McDonnell, J. A. M., Mennella, V., Michalik, H., Molina, A., Morales, R., Moreno, F., Mottola, S., Naletto, G., Oklay, N., Ortiz, J. L., Palomba, E., Palumbo, P., Perrin, J.-M., Rodríguez, J., Sabau, L., Snodgrass, C., Sordini, R., Thomas, N., Tubiana, C., Vincent, J.-B., Weissman, P., Wenzel, K.-P., Zakharov, V., and Zarnecki, J. C.

Published
2015

3. ExoMars TGO/NOMAD‐UVIS Vertical Profiles of Ozone: 1. Seasonal Variation and Comparison to Water

Author

Patel, M. R., primary, Sellers, G., additional, Mason, J. P., additional, Holmes, J. A., additional, Brown, M. A. J., additional, Lewis, S. R., additional, Rajendran, K., additional, Streeter, P. M., additional, Marriner, C., additional, Hathi, B. G., additional, Slade, D. J., additional, Leese, M. R., additional, Wolff, M. J., additional, Khayat, A. S. J., additional, Smith, M. D., additional, Aoki, S., additional, Piccialli, A., additional, Vandaele, A. C., additional, Robert, S., additional, Daerden, F., additional, Thomas, I. R., additional, Ristic, B., additional, Willame, Y., additional, Depiesse, C., additional, Bellucci, G., additional, and Lopez‐Moreno, J.‐J., additional

Published
2021
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4. 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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7. ExoMars TGO/NOMAD-UVIS Vertical Profiles of Ozone: 1. Seasonal Variation and Comparison to Water

Author

UK Space Agency, Belgian Science Policy Office, European Space Agency, European Commission, Ministerio de Economía y Competitividad (España), Ministerio de Ciencia e Innovación (España), Agenzia Spaziale Italiana, National Fund for Scientific Research (Belgium), Patel, Manish R., Sellers, G., Mason, Jonathon P., Holmes, J. A., Brown, M. A. J., Lewis, S. R., Rajendran, K., Streeter, P. M., Marriner, C., Hathi, B. G., Slade, D. J., Leese, M. R., Wolff, M. J., Khayat, A. S. J., Smith, M. D., Aoki, Shohei, Piccialli, A., Vandaele, Ann Carine, Robert, S., Daerden, Frank, Thomas, Ian R., Ristic, Bojan, Willame, Y., Depiesse, C., Bellucci, Giancarlo, López-Moreno, José Juan, UK Space Agency, Belgian Science Policy Office, European Space Agency, European Commission, Ministerio de Economía y Competitividad (España), Ministerio de Ciencia e Innovación (España), Agenzia Spaziale Italiana, National Fund for Scientific Research (Belgium), Patel, Manish R., Sellers, G., Mason, Jonathon P., Holmes, J. A., Brown, M. A. J., Lewis, S. R., Rajendran, K., Streeter, P. M., Marriner, C., Hathi, B. G., Slade, D. J., Leese, M. R., Wolff, M. J., Khayat, A. S. J., Smith, M. D., Aoki, Shohei, Piccialli, A., Vandaele, Ann Carine, Robert, S., Daerden, Frank, Thomas, Ian R., Ristic, Bojan, Willame, Y., Depiesse, C., Bellucci, Giancarlo, and López-Moreno, José Juan

Abstract

We present ∼1.5 Mars Years (MY) of ozone vertical profiles, covering LS = 163° in MY34 to LS = 320° in MY35, a period which includes the 2018 global dust storm. Since April 2018, the Ultraviolet and Visible Spectrometer channel of the Nadir and Occultation for Mars Discovery (NOMAD) instrument aboard the ExoMars Trace Gas Orbiter has observed the vertical, latitudinal and seasonal distributions of ozone. Around perihelion, the relative abundance of both ozone and water (from coincident NOMAD measurements) increases with decreasing altitude below ∼40 km. Around aphelion, localized decreases in ozone abundance exist between 25 and 35 km coincident with the location of modeled peak water abundances. High-latitude (>±55°), high altitude (40–55 km) equinoctial ozone enhancements are observed in both hemispheres (LS ∼350°–40°) and discussed in the companion article to this work (Khayat et al., 2021). The descending branch of the main Hadley cell shapes the observed ozone distribution at LS = 40°–60°, with the possible signature of a northern hemisphere thermally indirect cell identifiable from LS = 40°–80°. Morning terminator observations show elevated ozone abundances with respect to evening observations, with average ozone abundances between 20 and 40 km an order of magnitude higher at sunrise compared to sunset, attributed to diurnal photochemical partitioning along the line of sight between ozone and O or fluctuations in water abundance. The ozone retrievals presented here provide the most complete global description of Mars ozone vertical distributions to date as a function of season and latitude. © 2021. The Authors.

Published
2021

8. In situ measurements of the physical characteristics of Titan's environment

Author

Fulchignoni, M., Ferri, F., Angrilli, F., Ball, A. J., Bar-Nun, A., Barucci, M. A., Bettanini, C., Bianchini, G., Borucki, W., Colombatti, G., Coradini, M., Coustenis, A., Debei, S., Falkner, P., Fanti, G., Flamini, E., Gaborit, V., Grard, R., Hamelin, M., Harri, A. M., Hathi, B., Jernej, I., Leese, M. R., Lehto, A., Lion Stoppato, P. F., Lopez-Moreno, J. J., Makinen, T., McDonnell, J. A. M., McKay, C. P., Molina-Cuberos, G., Neubauer, F. M., Pirronello, V., Rodrigo, R., Saggin, B., Schwingenschuh, K., Seiff, A., Simoes, F., Svedhem, H., Tokano, T., Towner, M. C., Trautner, R., Withers, P., and Zarnecki, J. C.

Subjects
Environmental issues, Science and technology, Zoology and wildlife conservation
Abstract

Author(s): M. Fulchignoni [1, 2]; F. Ferri (corresponding author) [3]; F. Angrilli [3]; A. J. Ball [4]; A. Bar-Nun [5]; M. A. Barucci [1]; C. Bettanini [3]; G. Bianchini [3]; [...]

Published
2005
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9. Rosetta Lander (“Philae”) Investigations

Author

Bibring, J.-P., primary, Rosenbauer, H., additional, Boehnhardt, H., additional, Ulamec, S., additional, Biele, J., additional, Espinasse, S., additional, Feuerbacher, B., additional, Gaudon, P., additional, Hemmerich, P., additional, Kletzkine, P., additional, Moura, D., additional, Mugnuolo, R., additional, Nietner, G., additional, Pätz, B., additional, Roll, R., additional, Scheuerle, H., additional, Szegö, K., additional, Wittmann, K., additional, team, Philae, additional, Klingelhöfer, G., additional, Brückner, J., additional, d’Uston, C., additional, Gellert, R., additional, Rieder, R., additional, López, J. Gironés, additional, Bibring, J.-P., additional, Lamy, P., additional, Langevin, Y., additional, Soufflot, A., additional, Berthé, M., additional, Borg, J., additional, Poulet, F., additional, Mottola, S., additional, Goesmann, Fred, additional, Rosenbauer, Helmut, additional, Roll, Reinhard, additional, Szopa, Cyril, additional, Raulin, Francois, additional, Sternberg, Robert, additional, Israel, Guy, additional, Meierhenrich, Uwe, additional, Thiemann, Wolfram, additional, Munoz-Caro, Guillermo, additional, Spohn, Tilman, additional, Seiferlin, Karsten, additional, Hagermann, Axel, additional, Knollenberg, Jörg, additional, Ball, Andrew J., additional, Breuer, Doris, additional, Banaszkiewicz, Marek, additional, Benkhoff, Johannes, additional, Gadomski, Stanislaw, additional, Gregorczyk, Wojciech, additional, Grygorczuk, Jerzy, additional, Hlond, Marek, additional, Kargl, Günter, additional, Kührt, Ekkehard, additional, Kömle, Norbert, additional, Kossacki, Konrad, additional, Krasowski, Jacek, additional, Marczewski, Wojciech, additional, Zarnecki, John C., additional, Morse, A. D., additional, Morgan, G. H., additional, Andrews, D. J., additional, Barber, S. J., additional, Leese, M. R., additional, Sheridan, S., additional, Wright, I. P., additional, Pillinger, C. T., additional, Mottola, Stefano, additional, Arnold, Gabriele, additional, Grothues, Hans-Georg, additional, Jaumann, Ralf, additional, Michaelis, Harald, additional, Neukum, Gerhard, additional, Bibring, Jean-Pierre, additional, Auster, H.U., additional, Apathy, I., additional, Berghofer, G., additional, Remizov, A., additional, Fornacon, K.H., additional, Glassmeier, K.H., additional, Haerendel, G., additional, Hejja, I., additional, Kührt, E., additional, Magnes, W., additional, Moehlmann, D., additional, Motschmann, U., additional, Richter, I., additional, Russell, C.T., additional, Rustenbach, J., additional, Sauer, K., additional, Schwingenschuh, K., additional, Szemerey, I., additional, Waesch, R., additional, Zazzera, F. Bernelli, additional, Bologna, P., additional, Dainese, C., additional, Finzi, A. Ercoli, additional, Magnani, P.G., additional, Malnati, F., additional, Olivieri, A., additional, Re, E., additional, Seidensticker, K. J., additional, Möhlmann, D., additional, Schmidt, W., additional, Thiel, K., additional, Arnold, W., additional, Fischer, H.-H., additional, Kretschmer, M., additional, Péter, A., additional, Trautner, R., additional, and Schieke, S., additional

Published
2009
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10. Beagle 2: Mission to Mars - Current Status

Author

Gibson, E. K., Jr, Pillinger, C. T, Wright, I. P, Morgan, G. H, Yau, D, Stewart, J. L. C, Leese, M. R, Praine, I. J, and Sheridan, S

Subjects
Lunar And Planetary Science And Exploration
Abstract

Beagle 2 is a 72 kg probe (with a 32 kg lander) developed in the United Kingdom for inclusion on the European Space Agency's 2003 Mars Express. Beagle 2 was launched on June 2, 2003 with Mars Express on a Soyuz-Fregat rocket from the Baikonur Cosmodrome in Kazakhstan. Beagle 2 landed on Mars on December 25th, 2003 in Isidis Planitia (approx. 10.7 N and 268.6 W), a large sedimentary basin that overlies the boundary between ancient highlands and northern plains. Isidis Planitia, the third largest impact basin on Mars, which is possibly filled with sediment deposited at the bottom of long-standing lakes or seas, offers an ideal environment for preserving traces of life. The team is awaiting signals from the Beagle 2 lander at the time when this abstract was written. Current status of the mission will be reported. Beagle 2 was developed to search for organic material and other volatiles on and below the surface of Mars in addition to the study of the inorganic chemistry and mineralogy. Several fundamental properties can be used to determine the existence of an active or past biology on any planet, Earth or Mars. Beagle 2's targets for investigation included: (a) The presence of water, or the existence of minerals deposited from water to show that water was present, even if only transiently; (b) The detection of carbonaceous debris, the remains of organisms that might have lived in water or were washed to a final resting place by the action of water; (c) The structure of organic matter, to demonstrate that it might have been synthesized for a biological purpose; (d) The recognition of isotopic fractionation between carbonaceous phases (organic vs inorganic carbon phases), a condition which on Earth suggests that life emerged nearly 4 billion years ago.

Published
2004

12. Evolution Of The Dust Size Distribution Of Comet 67P/Churyumov-Gerasimenko From 2.2 Au To Perihelion

Author

Fulle, M., Marzari, F., Della Corte, V., Fornasier, S., Sierks, H., Rotundi, A., Barbieri, C., Lamy, P. L., Rodrigo, R., Koschny, D., Rickman, Hans, Keller, H. U., Lopez-Moreno, J. J., Accolla, M., Agarwal, J., A'Hearn, M. F., Altobelli, N., Barucci, M. A., Bertaux, J. -L, Bertini, I., Bodewits, D., Bussoletti, E., Colangeli, L., Cosi, M., Cremonese, G., Crifo, J. -F, Da Deppo, V., Davidsson, Björn, Debei, S., De Cecco, M., Esposito, F., Ferrari, M., Giovane, F., Gustafson, B., Green, S. F., Groussin, O., Gruen, E., Gutierrez, P., Guettler, C., Herranz, M. L., Hviid, S. F., Ip, W., Ivanovski, S. L., Jeronimo, J. M., Jorda, L., Knollenberg, J., Kramm, R., Kuehrt, E., Kueppers, M., Lara, L., Lazzarin, M., Leese, M. R., Lopez-Jimenez, A. C., Lucarelli, F., Epifani, E. Mazzotta, McDonnell, J. A. M., Mennella, V., Molina, A., Morales, R., Moreno, F., Mottola, S., Naletto, G., Oklay, N., Ortiz, J. L., Palomba, E., Palumbo, P., Perrin, J. -M, Rietmeijer, F. J. M., Rodriguez, J., Sordini, R., Thomas, N., Tubiana, C., Vincent, J. -B, Weissman, P., Wenzel, K. -P, Zakharov, V., Zarnecki, J. C., Fulle, M., Marzari, F., Della Corte, V., Fornasier, S., Sierks, H., Rotundi, A., Barbieri, C., Lamy, P. L., Rodrigo, R., Koschny, D., Rickman, Hans, Keller, H. U., Lopez-Moreno, J. J., Accolla, M., Agarwal, J., A'Hearn, M. F., Altobelli, N., Barucci, M. A., Bertaux, J. -L, Bertini, I., Bodewits, D., Bussoletti, E., Colangeli, L., Cosi, M., Cremonese, G., Crifo, J. -F, Da Deppo, V., Davidsson, Björn, Debei, S., De Cecco, M., Esposito, F., Ferrari, M., Giovane, F., Gustafson, B., Green, S. F., Groussin, O., Gruen, E., Gutierrez, P., Guettler, C., Herranz, M. L., Hviid, S. F., Ip, W., Ivanovski, S. L., Jeronimo, J. M., Jorda, L., Knollenberg, J., Kramm, R., Kuehrt, E., Kueppers, M., Lara, L., Lazzarin, M., Leese, M. R., Lopez-Jimenez, A. C., Lucarelli, F., Epifani, E. Mazzotta, McDonnell, J. A. M., Mennella, V., Molina, A., Morales, R., Moreno, F., Mottola, S., Naletto, G., Oklay, N., Ortiz, J. L., Palomba, E., Palumbo, P., Perrin, J. -M, Rietmeijer, F. J. M., Rodriguez, J., Sordini, R., Thomas, N., Tubiana, C., Vincent, J. -B, Weissman, P., Wenzel, K. -P, Zakharov, V., and Zarnecki, J. C.

Abstract

The Rosetta probe, orbiting Jupiter-family comet 67P/Churyumov-Gerasimenko, has been detecting individual dust particles of mass larger than 10(-10) kg by means of the GIADA dust collector and the OSIRIS Wide Angle Camera and Narrow Angle Camera since 2014 August and will continue until 2016 September. Detections of single dust particles allow us to estimate the anisotropic dust flux from 67P, infer the dust loss rate and size distribution at the surface of the sunlit nucleus, and see whether the dust size distribution of 67P evolves in time. The velocity of the Rosetta orbiter, relative to 67P, is much lower than the dust velocity measured by GIADA, thus dust counts when GIADA is nadir-pointing will directly provide the dust flux. In OSIRIS observations, the dust flux is derived from the measurement of the dust space density close to the spacecraft. Under the assumption of radial expansion of the dust, observations in the nadir direction provide the distance of the particles by measuring their trail length, with a parallax baseline determined by the motion of the spacecraft. The dust size distribution at sizes > 1 mm observed by OSIRIS is consistent with a differential power index of -4, which was derived from models of 67P's trail. At sizes <1 mm, the size distribution observed by GIADA shows a strong time evolution, with a differential power index drifting from -2 beyond 2 au to -3.7 at perihelion, in agreement with the evolution derived from coma and tail models based on ground-based data. The refractory-to-water mass ratio of the nucleus is close to six during the entire inbound orbit and at perihelion.

Published
2016
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13. 67P/C-G inner coma dust properties from 2.2 au inbound to 2.0 au outbound to the Sun

Author

Della Corte, V., primary, Rotundi, A., additional, Fulle, M., additional, Ivanovski, S., additional, Green, S. F., additional, Rietmeijer, F. J. M., additional, Colangeli, L., additional, Palumbo, P., additional, Sordini, R., additional, Ferrari, M., additional, Accolla, M., additional, Zakharov, V., additional, Mazzotta Epifani, E., additional, Weissman, P., additional, Gruen, E., additional, Lopez-Moreno, J. J., additional, Rodriguez, J., additional, Bussoletti, E., additional, Crifo, J. F., additional, Esposito, F., additional, Lamy, P. L., additional, McDonnell, J. A. M., additional, Mennella, V., additional, Molina, A., additional, Morales, R., additional, Moreno, F., additional, Palomba, E., additional, Perrin, J. M., additional, Rodrigo, R., additional, Zarnecki, J. C., additional, Cosi, M., additional, Giovane, F., additional, Gustafson, B., additional, Ortiz, J. L., additional, Jeronimo, J. M., additional, Leese, M. R., additional, Herranz, M., additional, Liuzzi, V., additional, and Lopez-Jimenez, A. C., additional

Published
2016
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14. EVOLUTION OF THE DUST SIZE DISTRIBUTION OF COMET 67P/CHURYUMOV–GERASIMENKO FROM 2.2 au TO PERIHELION

Author

Fulle, M., primary, Marzari, F., additional, Della Corte, V., additional, Fornasier, S., additional, Sierks, H., additional, Rotundi, A., additional, Barbieri, C., additional, Lamy, P. L., additional, Rodrigo, R., additional, Koschny, D., additional, Rickman, H., additional, Keller, H. U., additional, López-Moreno, J. J., additional, Accolla, M., additional, Agarwal, J., additional, A’Hearn, M. F., additional, Altobelli, N., additional, Barucci, M. A., additional, Bertaux, J.-L., additional, Bertini, I., additional, Bodewits, D., additional, Bussoletti, E., additional, Colangeli, L., additional, Cosi, M., additional, Cremonese, G., additional, Crifo, J.-F., additional, Da Deppo, V., additional, Davidsson, B., additional, Debei, S., additional, De Cecco, M., additional, Esposito, F., additional, Ferrari, M., additional, Giovane, F., additional, Gustafson, B., additional, Green, S. F., additional, Groussin, O., additional, Grün, E., additional, Gutierrez, P., additional, Güttler, C., additional, Herranz, M. L., additional, Hviid, S. F., additional, Ip, W., additional, Ivanovski, S. L., additional, Jerónimo, J. M., additional, Jorda, L., additional, Knollenberg, J., additional, Kramm, R., additional, Kührt, E., additional, Küppers, M., additional, Lara, L., additional, Lazzarin, M., additional, Leese, M. R., additional, López-Jiménez, A. C., additional, Lucarelli, F., additional, Mazzotta Epifani, E., additional, McDonnell, J. A. M., additional, Mennella, V., additional, Molina, A., additional, Morales, R., additional, Moreno, F., additional, Mottola, S., additional, Naletto, G., additional, Oklay, N., additional, Ortiz, J. L., additional, Palomba, E., additional, Palumbo, P., additional, Perrin, J.-M., additional, Rietmeijer, F. J. M., additional, Rodríguez, J., additional, Sordini, R., additional, Thomas, N., additional, Tubiana, C., additional, Vincent, J.-B., additional, Weissman, P., additional, Wenzel, K.-P., additional, Zakharov, V., additional, and Zarnecki, J. C., additional

Published
2016
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15. JANUS on JUICE: A Camera to Investigate Ganymede, Europa, Callisto, and the Jovian System

Author

Schmitz, Nicole, Palumbo, P., Jaumann, R., Della Corte, Vincenzo, Zusi, M., Castro, J. M., Leese, M. R., Debei, S., Magrin, D., Michalik, H., Cremonese, G., Hoffmann, Harald, Holland, A., Lara, L. M., Fiethe, B., Friso, Enrico, Greggio, D., Herranz, M., Koncz, Alexander, Lichopoj, A., Martinez-Navajas, I., Mazotta Epifani, E., Michaelis, H., Behnke, T., Ragazzoni, R., Roatsch, Thomas, Rodrigo, R., Rodriguez, E., Schipani, P., Soman, M., and Zaccariotto, M.

Subjects
JANUS, JUICE
Published
2014

16. The JANUS camera onboard JUICE mission for Jupiter system optical imaging

Author

Palumbo, P., Jaumann, R., Della Corte, Vincenzo, Cremonese, Gabriele, Debei, S., Hoffmann, Harald, Holland, A., Lara, Luisa M., Castro, J. M., Friso, E., Greggio, D., Herranz, M., Leese, M. R., Lichopoj, A., Magrin, D., Marra, G., Mazotta Epifani, E., Michaelis, Harald, Ragazzoni, R., Roatsch, Thomas, Rodriguez, E., Schipani, P., Schmitz, Nicole, and Zusi, M.

Subjects
JANUS, Optical Telescope, JUICE
Published
2014

17. Trace gas transport in the subsurface of Mars

Author

Stevens, A. H., Patel, M. R., Lewis, S. R., Ringrose, T. J., and Leese, M. R.

Subjects
Astrophysics::Earth and Planetary Astrophysics, Physics::Atmospheric and Oceanic Physics
Abstract

The ExoMars Trace Gas Orbiter (TGO) will have the capability of detecting and characterizing a broad suite of trace gases in the atmosphere of Mars. Interpreting the results of this mission will require an understanding of how these trace gases are transported from their sources, which may be deep underground, to the atmosphere. Here we present results of modeling designed to measure the timescales of release from putative subsurface methane sources. These transport timescales are far longer than mixing times in the atmosphere and could be up to 10 million years.

Published
2013

18. Trace gas transport in the martian subsurface

Author

Stevens, A. H., Patel, M. R., Ringrose, T. J., Lewis, S. R., and Leese, M. R.

Abstract

A number of sources have been proposed for the methane observed in the atmosphere of Mars [1]. Serpentinisation could be a deep geologic source of the gas, where mafic minerals interact with a subsurface water table. [2] If so, the methane produced would have to travel through kilometres of megaregolith before entering the atmosphere. Although the structure of the martian subsurface is poorly known, this transport can be modelled using carefully chosen parameters and a modified form of Fick’s laws [3]. Such a model can be used to estimate transport timescales and investigate the properties of release.\ud \ud Methane clathrate hydrates are a potentially shallower methane source as they could be stable up to depths of only a few metres near the martian poles. The dissociation of these deposits could more easily explain the observed variation of methane in the atmosphere, as they would be more directly influenced by surface temperature changes [4]. To investigate the potential contributions of methane clathrate hydrates, we create samples in the lab and investigate their behaviour under Mars conditions in environmental simulation chambers.\ud \ud Combining the results of these models and experiments with data from future missions such as the ExoMars Trace Gas Orbiter will allow constraints to be placed on the potential sources of trace gases observed in the martian atmosphere.\ud \ud 1. Atreya, S.K., et al., Planetary and Space Science, 2011. 59(2-3): p. 133-136.\ud 2. Oze, C. and M. Sharma, Geophys. Res. Lett., 2005. 32(10): p. L10203.\ud 3. Sizemore, H.G. and M.T. Mellon, Icarus, 2008. 197(2): p. 606-620.\ud 4. Root, M.J. and M.E. Elwood Madden, Icarus, 2012. 218(1): p. 534-544.

Published
2013

19. 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

20. ExoMars entry, descent and landing science

Author

Ferri, F., Lewis, S. R., Withers, P., Aboudan, A., Bettanini, C., Colombatti, G., Debei, S., Golombek, M., Harri, A. M., Komatsu, G., Leese, M. R., Mäkinen, T., Müller-Wodarg, I., Ori, G. G., Patel, M. R., Pondrelli, M., Siili, T., Tokano, T., Towner, M., and Zarnecki, J. C.

Abstract

The entry, descent and landing of ExoMars offer a rare (once-per-mission) opportunity to perform in situ investigation of the martian environment over a wide altitude range. Entry, Descent and Landing System (EDLS) measurements can provide essential data for atmospheric scientific investigations.\ud \ud We intend to perform atmospheric science measurements by exploiting data from EDLS engineering sensors and exploiting their readings beyond the expected engineering information.

Published
2011

21. GIADA: shining a light on the monitoring of the comet dust production from the nucleus of 67P/Churyumov-Gerasimenko

Author

Della Corte, V., primary, Rotundi, A., additional, Fulle, M., additional, Gruen, E., additional, Weissman, P., additional, Sordini, R., additional, Ferrari, M., additional, Ivanovski, S., additional, Lucarelli, F., additional, Accolla, M., additional, Zakharov, V., additional, Mazzotta Epifani, E., additional, Lopez-Moreno, J. J., additional, Rodriguez, J., additional, Colangeli, L., additional, Palumbo, P., additional, Bussoletti, E., additional, Crifo, J. F., additional, Esposito, F., additional, Green, S. F., additional, Lamy, P. L., additional, McDonnell, J. A. M., additional, Mennella, V., additional, Molina, A., additional, Morales, R., additional, Moreno, F., additional, Ortiz, J. L., additional, Palomba, E., additional, Perrin, J. M., additional, Rietmeijer, F. J. M., additional, Rodrigo, R., additional, Zarnecki, J. C., additional, Cosi, M., additional, Giovane, F., additional, Gustafson, B., additional, Herranz, M. L., additional, Jeronimo, J. M., additional, Leese, M. R., additional, Lopez-Jimenez, A. C., additional, and Altobelli, N., additional

Published
2015
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22. DENSITY AND CHARGE OF PRISTINE FLUFFY PARTICLES FROM COMET 67P/CHURYUMOV–GERASIMENKO

Author

Fulle, M., primary, Corte, V. Della, additional, Rotundi, A., additional, Weissman, P., additional, Juhasz, A., additional, Szego, K., additional, Sordini, R., additional, Ferrari, M., additional, Ivanovski, S., additional, Lucarelli, F., additional, Accolla, M., additional, Merouane, S., additional, Zakharov, V., additional, Epifani, E. Mazzotta, additional, Moreno, J. J. López-, additional, Rodríguez, J., additional, Colangeli, L., additional, Palumbo, P., additional, Grün, E., additional, Hilchenbach, M., additional, Bussoletti, E., additional, Esposito, F., additional, Green, S. F., additional, Lamy, P. L., additional, McDonnell, J. A. M., additional, Mennella, V., additional, Molina, A., additional, Morales, R., additional, Moreno, F., additional, Ortiz, J. L., additional, Palomba, E., additional, Rodrigo, R., additional, Zarnecki, J. C., additional, Cosi, M., additional, Giovane, F., additional, Gustafson, B., additional, Herranz, M. L., additional, Jerónimo, J. M., additional, Leese, M. R., additional, Jiménez, A. C. López-, additional, and Altobelli, N., additional

Published
2015
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23. Exomars entry and descent science

Author

Ferri, F., Stephen Lewis, Ball, A. J., Colombatti, G., Aboudan, A., Angrilli, F., Müller-Wodarg, I., Hathi, B., Leese, M. R., and Zarnecki, J. C.

Abstract

The entry, descent and landing of ExoMars offer a rare (once-per-mission) opportunity to perform in situ investigation of the martian environment over a wide altitude range. We present an initial assessment of the atmospheric science that can be performed using sensors of the Entry, Descent and Landing System (EDLS), over and above the expected engineering information. This is intended to help fulfill the concept of an Atmospheric Parameters Package (APP), as mentioned in the ExoMars draft Science Management Plan [ESA, 2005].\ud Mars' atmosphere is highly variable in time and space, due to phenomena including inertio-gravity waves, thermal tide effects, dust, solar wind conditions, and diurnal, seasonal and topographic effects. Atmospheric profile measurements, drawing on heritage from the Huygens Atmospheric Structure Instrument (HASI), which encountered Titan's atmosphere\ud in 2005 [1], should allow us to address questions of the martian atmosphere's structure, dynamics and variability.

Published
2008

25. In-flight performance of the HASI servo accelerometer and implications for results at Titan

Author

Zarnecki, J. C., Francesca Ferri, Hathi, B., Leese, M. R., Ball, A. J., Colombatti, G., Fulchignoni, M., Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Pôle Planétologie du LESIA, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)

Subjects
[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

International audience

Published
2004

26. A miniature UV-VIS spectrometer for the surface of Mars

Author

Patel, M. R., Towner, M. C., Zarnecki, J. C., Leese, M. R., Davies, A., and Husbands, A.

Abstract

A miniature spectrometer is in the process of development for a future Mars mission, to measure the UV-VIS spectrum encountered at the martian surface. With an intended mass of ~100 g, the spectrometer is planned as part of the ESA ExoMars mission.

Published
2004

27. 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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28. Ptolemy – an Instrument to Measure Stable Isotopic Ratios of Key Volatiles on a Cometary Nucleus

Author

Wright, I. P., primary, Barber, S. J., additional, Morgan, G. H., additional, Morse, A. D., additional, Sheridan, S., additional, Andrews, D. J., additional, Maynard, J., additional, Yau, D., additional, Evans, S. T., additional, Leese, M. R., additional, Zarnecki, J. C., additional, Kent, B. J., additional, Waltham, N. R., additional, Whalley, M. S., additional, Heys, S, additional, Drummond, D. L., additional, Edeson, R. L., additional, Sawyer, E. C., additional, Turner, R. F., additional, and Pillinger, C. T., additional

Published
2006
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30. An impact penetrometer for a landing spacecraft

Author

Lorenz, R D, primary, Bannister, M, additional, Daniell, P M, additional, Krysinski, Z, additional, Leese, M R, additional, Miller, R J, additional, Newton, G, additional, Rabbetts, P, additional, Willett, D M, additional, and Zarnecki, J C, additional

Published
1994
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31. Physical properties as indicators of liquid compositions: Derivation of the composition for Titan's surface liquids from theHuygensSSP measurements.

Author

Hagermann, A., Zarnecki, J. C., Towner, M. C., Rosenberg, P. D., Lorenz, R. D., Leese, M. R., Hathi, B., and Ball, A. J.

Subjects
TITAN (Satellite), COSMOCHEMISTRY, SATELLITES of Saturn, LIQUIDS, METHANE, ETHANES, NITROGEN, ARGON
Abstract

We present a method for inferring the relative molar abundance of constituents of a liquid mixture, in this case methane, ethane, nitrogen and argon, from a measurement of a set of physical properties of the mixture. This problem is of interest in the context of theHuygensSurface Science Package, SSP, equipped to measure several physical properties of a liquid in case of a liquid landing on Saturn's moon Titan. While previous models emphasized the possibility ofverifyinga certain model proposed by atmospheric composition and equations of state, we use an inverse approach to the problem, i.e. we will infer the liquid composition strictly from our measurements of density, refractive index, permittivity, thermal conductivity and speed of sound. Other a priori information can later be used to improve (or reject) the model obtained from these measurements. [ABSTRACT FROM AUTHOR]

Published
2005
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34. Early Grain Detections in the Coma of Comet 67P/Churyumov-Gerasimenko

Author

Rotundi, A., Della Corte, V., Fulle, M., Accolla, M., Ferrari, M., Ivanovski, S., Lucarelli, F., Sordini, R., Zakharov, V., Mazzotta Epifani, E., Lopez-Moreno, J. J., Rodriguez, J., Colangeli, L., Palumbo, P., Crifo, J. C., Bussoletti, E., Esposito, F., Green, S., Grün, E., Lamy, P. L., Mcdonnell, J. A. M., Vito Mennella, Molina, A., Morales, R., Moreno, F., Ortiz, J. L., Palomba, E., Perrin, J. -M, Rietmeijer, F. J. M., Rodrigo, R., Weissman, P. R., Zarnecki, J. C., Cosi, M., Giovane, F., Gustafson, B., Herranz, M. L., Jeronimo, J. M., Leese, M. R., Lopez-Jimenez, A., and Altobelli, N.

37. Dust Measurements in the Coma of Comet 67P/Churyumov-Gerasimenko Inbound to the Sun Between 3.7 and 3.4 AU

Author

Fulle, M., Della Corte, V., Rotundi, A., Accolla, M., Ferrari, M., Ivanovski, S., Lucarelli, F., Sordini, R., Zakharov, V., Mazzotta Epifani, E., Lopez-Moreno, J. J., Rodriguez, J., Colangeli, L., Palumbo, P., Bussoletti, E., Crifo, J., Francesca Esposito, Green, S. F., Gruen, E., Lamy, P. L., Mcdonnell, J. A. M., Mennella, V., Molina, A., Morales, R., Moreno, F., Ortiz, J. L., Palomba, E., Perrin, J., Rodrigo, R., Weissman, P., Zarnecki, J. C., Cosi, M., Giovane, F., Gustafson, B., Herranz, M. L., Jeronimo, J. M., Leese, M. R., Lopez-Jimenez, A. C., Altobelli, N., Sierks, H., Agarwal, J., Bertini, I., Fornasier, S., Gutierrez, P. J., Lara, L., Guettler, C., Marzari, F., Oaklay, N., Snodgrass, C., Tubiana, C., and Vincenzo, J. B.

Abstract

GIADA and OSIRIS dust data, combined with data from MIRO and ROSINA instruments onboard Rosetta, from 3.7 to 3.4 AU inbound provide a dust/gas ratio of 4 ± 2.

38. ProSPA: the Science Laboratory for the Processing and Analysis of Lunar Polar Volatiles within PROSPECT

Author

Barber, S. J., Smith, P. H., Wright, I. P., Abernethy, F., Anand, M., Dewar, K. R., Hodges, M., Landsberg, P., Leese, M. R., Morgan, G. H., Morse, A. D., Mortimer, J., Sargeant, Hannah, Sheard, I., Sheridan, S., Verchovsky, A., Goesmann, S., Howe, C., Morse, T., Lillywhite, N., Quinn, A., Missaglia, N., Pedrali, M., Reiss, P., Rizzi, F., Rusconi, A., Savoia, M., Zamboni, A., Merrifield, J. A., Gibson Jr., E. K., Carpenter, J., Fisackerly, R., and Houdou, B.

39. Evolution of the dust size distribution of comet 67P/Churymov–Gerasimenko from 2.2 au to Perihelion

Author

Rotundi, A., Ortiz, J. L., Mennella, V., Palomba, E., Rickman, H., Bertaux, J.-L., Oklay, N., Altobelli, N., Knollenberg, J., Palumbo, P., Mottola, S., Giovane, F., Grün, E., Küppers, M., Kramm, R., Güttler, C., Barbieri, C., Lamy, P. L., Cremonese, G., Leese, M. R., A’Hearn, M. F., Kührt, E., Bertini, I., Thomas, Nicolas, Fulle, M., Zakharov, V., Lazzarin, M., Esposito, F., Rietmeijer, F. J. M., Barucci, M. A., Sierks, H., Agarwal, J., Davidsson, B., Morales, R., Colangeli, L., Accolla, M., Mazzotta Epifani, E., Molina, A., Keller, H. U., Weissman, P., Green, S. F., Rodrigo, R., De Cecco, M., López-Moreno, J. J., Lara, L., Crifo, J.-F., Ivanovski, S. L., Herranz, M. L., Cosi, M., Tubiana, C., Bussoletti, E., Moreno, F., Marzari, F., Zarnecki, J. C., Jorda, L., Fornasier, S., Groussin, O., Ip, W., Hviid, S. F., Ferrari, M., Vincent, J.-B., Gustafson, B., Jerónimo, J. M., Debei, S., McDonnell, J. A. M., Della Corte, V., Sordini, R., López-Jiménez, A. C., Koschny, D., Da Deppo, V., Naletto, G., Wenzel, K.-P., Lucarelli, F., Perrin, J.-M., Bodewits, D., Gutierrez, P., and Rodríguez, J.

Subjects
13. Climate action, 530 Physics, 520 Astronomy, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, 620 Engineering, Astrophysics::Galaxy Astrophysics
Abstract

The Rosetta probe, orbiting Jupiter-family comet 67P/Churyumov–Gerasimenko, has been detecting individual dust particles of mass larger than 10−10 kg by means of the GIADA dust collector and the OSIRIS Wide Angle Camera and Narrow Angle Camera since 2014 August and will continue until 2016 September. Detections of single dust particles allow us to estimate the anisotropic dust flux from 67P, infer the dust loss rate and size distribution at the surface of the sunlit nucleus, and see whether the dust size distribution of 67P evolves in time. The velocity of the Rosetta orbiter, relative to 67P, is much lower than the dust velocity measured by GIADA, thus dust counts when GIADA is nadir-pointing will directly provide the dust flux. In OSIRIS observations, the dust flux is derived from the measurement of the dust space density close to the spacecraft. Under the assumption of radial expansion of the dust, observations in the nadir direction provide the distance of the particles by measuring their trail length, with a parallax baseline determined by the motion of the spacecraft. The dust size distribution at sizes >1 mm observed by OSIRIS is consistent with a differential power index of −4, which was derived from models of 67P's trail. At sizes

41. DFA - The dust flux analyzer for the Rosetta orbiter

Author

Lamy, P., Perruchot, S., Reynaud, J. -L, Leese, M. R., Mcdonnell, J. A. M., Green, S. F., Busoletti, E., Colangeli, L., marco fulle, Rotundi, A., Giovane, F., Gustafson, B., and Perrin, J. -M

Subjects
Space and Planetary Science, Aerospace Engineering

42. ProSPA: Analysis of Lunar Polar Volatiles and ISRU Demonstration on the Moon

Author

Barber, S. J., Wright, I. P., Abernethy, F., Anand, M., Dewar, K. R., Hodges, M., Landsberg, P., Leese, M. R., Morgan, G. H., Morse, A. D., Mortimer, J., Sargeant, Hannah, Sheard, I., Sheridan, S., Verchovsky, A., Goesmann, F., Howe, C., Morse, T., Lillywhite, N., Quinn, A., Missaglia, N., Pedrali, M., Reiss, P., Rizzi, F., Rusconi, A., Savoia, M., Zamboni, A., Merrifield, J. A., Gibson, E. K., Carpenter, J., Fisackerly, R., Houdou, B., Sefton-Nash, E., and Trautner, R.

43. Recent Results on Titan from the HASI Instrument

Author

Fulchignoni, M., And The Hasi Team Angrilli F, Ferri F., Ball A, J., Bar Nun, A., Barucci M, A., Bettanini Fecia Di Cossato, Carlo, Bianchini, G., Borucki, W., Giacomo Colombatti, Coradini, M., Coustenis, A., Stefano Debei, Falkner, P., Giulio Fanti, Flamini, E., Gaborit, V., Grard, R., Hamelin, M., Hathi B, Harri A. M., Jernej, I., Leese M, R., Lehto, A., López Moreno J, J., Mäkinen, T., Mcdonnell J A, M., Mckay C, P., Molina Cuberos, G., Neubauer F, M., Pirronello, V., Rodrigo, R., Saggin, B., Schwingenschuh, K., Seiff, A., Simões, F., Svedhem, H., Tokano, T., Towner M, C., Trautner, R., And Zarnecki, Withers P., and J. C.

44. ExoMars TGO/NOMAD‐UVIS vertical profiles of ozone: Part 1 – Seasonal variation and comparison to water

Author

Patel, M. R., Sellers, G., Mason, J., Holmes, J.A., Brown, M. A. J., Lewis, S. R., Rajendran, K., Streeter, P. M., Marriner, C., Hathi, B. D., Slade, D. J., Leese, M. R., Wolff, M. J., Khayat, A. S. J., Smith, M. D., Aoki, S., Piccialli, A., Vandaele, A. C., Robert, S., Daerden, F., Thomas, I. R., Ristic, B., Willame, Y., Depiesse, C., Bellucci, G., Lopez‐Moreno, J.‐J., Patel, M. R., Sellers, G., Mason, J., Holmes, J.A., Brown, M. A. J., Lewis, S. R., Rajendran, K., Streeter, P. M., Marriner, C., Hathi, B. D., Slade, D. J., Leese, M. R., Wolff, M. J., Khayat, A. S. J., Smith, M. D., Aoki, S., Piccialli, A., Vandaele, A. C., Robert, S., Daerden, F., Thomas, I. R., Ristic, B., Willame, Y., Depiesse, C., Bellucci, G., and Lopez‐Moreno, J.‐J.

Abstract

We present ∼1.5 Mars Years (MY) of ozone vertical profiles, covering LS = 163° in MY34 to LS = 320° in MY35, a period which includes the 2018 global dust storm. Since April 2018, the Ultraviolet and Visible Spectrometer (UVIS) channel of the Nadir and Occultation for Mars Discovery (NOMAD) instrument aboard the ExoMars Trace Gas Orbiter has observed the vertical, latitudinal and seasonal distributions of ozone. Around perihelion, the relative abundance of both ozone and water (from coincident NOMAD measurements) increases with decreasing altitude below ∼40 km. Around aphelion, localised decreases in ozone abundance exist between 25-35 km coincident with the location of modelled peak water abundances. High latitude (> ± 55°), high altitude (40-55 km) equinoctial ozone enhancements are observed in both hemispheres (LS ∼350-40°) and discussed in the companion paper to this work (Khayat et al, 2021). The descending branch of the main Hadley cell shapes the observed ozone distribution at LS = 40-60°, with the possible signature of a northern hemisphere thermally indirect cell identifiable from LS = 40-80°. Morning terminator observations show elevated ozone abundances with respect to evening observations, with average ozone abundances between 20 and 40 km an order of magnitude higher at sunrise compared to sunset, attributed to diurnal photochemical partitioning along the line of sight between ozone and O or fluctuations in water abundance. The ozone retrievals presented here provide the most complete global description of Mars ozone vertical distributions to date as a function of season and latitude.

45. ProSPA: Analysis of Lunar Polar Volatiles and ISRU Demonstration on the Moon

Author

Barber, S. J., Wright, I. P., Abernethy, F., Anand, M., Dewar, K. R., Hodges, M., Landsberg, P., Leese, M. R., Morgan, G. H., Morse, A. D., Mortimer, J., Sargeant, Hannah, Sheard, I., Sheridan, S., Verchovsky, A., Goesmann, F., Howe, C., Morse, T., Lillywhite, N., Quinn, A., Missaglia, N., Pedrali, M., Reiss, P., Rizzi, F., Rusconi, A., Savoia, M., Zamboni, A., Merrifield, J. A., Gibson, E. K., Carpenter, J., Fisackerly, R., Houdou, B., Sefton-Nash, E., Trautner, R., Barber, S. J., Wright, I. P., Abernethy, F., Anand, M., Dewar, K. R., Hodges, M., Landsberg, P., Leese, M. R., Morgan, G. H., Morse, A. D., Mortimer, J., Sargeant, Hannah, Sheard, I., Sheridan, S., Verchovsky, A., Goesmann, F., Howe, C., Morse, T., Lillywhite, N., Quinn, A., Missaglia, N., Pedrali, M., Reiss, P., Rizzi, F., Rusconi, A., Savoia, M., Zamboni, A., Merrifield, J. A., Gibson, E. K., Carpenter, J., Fisackerly, R., Houdou, B., Sefton-Nash, E., and Trautner, R.

46. 67P/C-G Inner Coma dust properties from 2.2 au inbound to 2.0 au outbound to the Sun

Author

Della Corte, V., Rotundi, A., Fulle, M., Ivanovski, S., Green, S. F., Rietmeijer, F. J. M., Colangeli, L., Palumbo, P., Sordini, R., Ferrari, M., Accolla, M., Zakharov, V., Mazzotta Epifani, E., Weissman, P., Gruen, E., Lopez-Moreno, J. J., Rodriguez, J., Bussoletti, E., Crifo, J. F., Esposito, F., Lamy, P. L., McDonnell, J. A. M., Mennella, V., Molina, A., Morales, R., Moreno, F., Palomba, E., Perrin, J. M., Rodrigo, R., Zarnecki, J. C., Cosi, M., Giovane, F., Gustafson, B., Ortiz, J. L., Jeronimo, J. M., Leese, M. R., Herranz, M., Liuzzi, V., Lopez-Jimenez, A. C., Della Corte, V., Rotundi, A., Fulle, M., Ivanovski, S., Green, S. F., Rietmeijer, F. J. M., Colangeli, L., Palumbo, P., Sordini, R., Ferrari, M., Accolla, M., Zakharov, V., Mazzotta Epifani, E., Weissman, P., Gruen, E., Lopez-Moreno, J. J., Rodriguez, J., Bussoletti, E., Crifo, J. F., Esposito, F., Lamy, P. L., McDonnell, J. A. M., Mennella, V., Molina, A., Morales, R., Moreno, F., Palomba, E., Perrin, J. M., Rodrigo, R., Zarnecki, J. C., Cosi, M., Giovane, F., Gustafson, B., Ortiz, J. L., Jeronimo, J. M., Leese, M. R., Herranz, M., Liuzzi, V., and Lopez-Jimenez, A. C.

Abstract

GIADA (Grain Impact Analyzer and Dust Accumulator) on-board the Rosetta space probe is designed to measure the momentum, mass and speed of individual dust particles escaping the nucleus of comet 67P/Churyumov-Gerasimenko (hereafter 67P). From August 2014 to June 2016 Rosetta escorted comet 67P during its journey around the Sun. Here we focus on GIADA data taken between 2015 January and 2016 February which included 67P's perihelion passage. To better understand cometary activity and more specifically the presence of dust structures in cometary comae, we mapped the spatial distribution of dust density in 67P's coma. In this manner we could track the evolution of high density regions of coma dust and their connections with nucleus illumination conditions, namely tracking 67P's seasons. We also studied the link between dust particle speeds and their masses with respect to heliocentric distance, i.e. the level of cometary activity. This allowed us to derive a global and a local correlation of the dust particles’ speed distribution with respect to the H2O production rate.

47. Evolution of the Dust Size Distribution of Comet 67P/Churyumov–Gerasimenko from 2.2 au to Perihelion

Author

Fulle, M., Marzari, F., Della Corte, V., Fornasier, S., Sierks, H., Rotundi, A., Barbieri, C., Lamy, P. L., Rodrigo, R., Koschny, D., Rickman, H., Keller, H. U., López-Moreno, J. J., Accolla, M., Agarwal, J., A’Hearn, M. F., Altobelli, N., Barucci, M. A., Bertaux, J.-L., Bertini, I., Bodewits, D., Bussoletti, E., Colangeli, L., Cosi, M., Cremonese, G., Crifo, J.-F., Da Deppo, V., Davidsson, B., Debei, S., De Cecco, M., Esposito, F., Ferrari, M., Giovane, F., Gustafson, B., Green, S. F., Groussin, O., Grün, E., Gutierrez, P., Güttler, C., Herranz, M. L., Hviid, S. F., Ip, W., Ivanovski, S. L., Jerónimo, J. M., Jorda, L., Knollenberg, J., Kramm, R., Kührt, E., Küppers, M., Lara, L., Lazzarin, M., Leese, M. R., López-Jiménez, A. C., Lucarelli, F., Mazzotta Epifani, E., McDonnell, J. A. M., Mennella, V., Molina, A., Morales, R., Moreno, F., Mottola, S., Naletto, G., Oklay, N., Ortiz, J. L., Palomba, E., Palumbo, P., Perrin, J.-M., Rietmeijer, F. J. M., Rodríguez, J., Sordini, R., Thomas, N., Tubiana, C., Vincent, J.-B., Weissman, P., Wenzel, K.-P., Zakharov, V., Zarnecki, J. C., Fulle, M., Marzari, F., Della Corte, V., Fornasier, S., Sierks, H., Rotundi, A., Barbieri, C., Lamy, P. L., Rodrigo, R., Koschny, D., Rickman, H., Keller, H. U., López-Moreno, J. J., Accolla, M., Agarwal, J., A’Hearn, M. F., Altobelli, N., Barucci, M. A., Bertaux, J.-L., Bertini, I., Bodewits, D., Bussoletti, E., Colangeli, L., Cosi, M., Cremonese, G., Crifo, J.-F., Da Deppo, V., Davidsson, B., Debei, S., De Cecco, M., Esposito, F., Ferrari, M., Giovane, F., Gustafson, B., Green, S. F., Groussin, O., Grün, E., Gutierrez, P., Güttler, C., Herranz, M. L., Hviid, S. F., Ip, W., Ivanovski, S. L., Jerónimo, J. M., Jorda, L., Knollenberg, J., Kramm, R., Kührt, E., Küppers, M., Lara, L., Lazzarin, M., Leese, M. R., López-Jiménez, A. C., Lucarelli, F., Mazzotta Epifani, E., McDonnell, J. A. M., Mennella, V., Molina, A., Morales, R., Moreno, F., Mottola, S., Naletto, G., Oklay, N., Ortiz, J. L., Palomba, E., Palumbo, P., Perrin, J.-M., Rietmeijer, F. J. M., Rodríguez, J., Sordini, R., Thomas, N., Tubiana, C., Vincent, J.-B., Weissman, P., Wenzel, K.-P., Zakharov, V., and Zarnecki, J. C.

Abstract

The Rosetta probe, orbiting Jupiter-family comet 67P/Churyumov–Gerasimenko, has been detecting individual dust particles of mass larger than 10^(−10) kg by means of the GIADA dust collector and the OSIRIS Wide Angle Camera and Narrow Angle Camera since 2014 August and will continue until 2016 September. Detections of single dust particles allow us to estimate the anisotropic dust flux from 67P, infer the dust loss rate and size distribution at the surface of the sunlit nucleus, and see whether the dust size distribution of 67P evolves in time. The velocity of the Rosetta orbiter, relative to 67P, is much lower than the dust velocity measured by GIADA, thus dust counts when GIADA is nadir-pointing will directly provide the dust flux. In OSIRIS observations, the dust flux is derived from the measurement of the dust space density close to the spacecraft. Under the assumption of radial expansion of the dust, observations in the nadir direction provide the distance of the particles by measuring their trail length, with a parallax baseline determined by the motion of the spacecraft. The dust size distribution at sizes >1 mm observed by OSIRIS is consistent with a differential power index of −4, which was derived from models of 67P’s trail. At sizes <1 mm, the size distribution observed by GIADA shows a strong time evolution, with a differential power index drifting from −2 beyond 2 au to −3.7 at perihelion, in agreement with the evolution derived from coma and tail models based on ground-based data. The refractory-to-water mass ratio of the nucleus is close to six during the entire inbound orbit and at perihelion.

48. Trace gas transport in the subsurface of Mars

Author

Stevens, A. H., Patel, M. R., Lewis, S. R., Ringrose, T. J., Leese, M. R., Stevens, A. H., Patel, M. R., Lewis, S. R., Ringrose, T. J., and Leese, M. R.

Abstract

The ExoMars Trace Gas Orbiter (TGO) will have the capability of detecting and characterizing a broad suite of trace gases in the atmosphere of Mars. Interpreting the results of this mission will require an understanding of how these trace gases are transported from their sources, which may be deep underground, to the atmosphere. Here we present results of modeling designed to measure the timescales of release from putative subsurface methane sources. These transport timescales are far longer than mixing times in the atmosphere and could be up to 10 million years.

49. Trace gas transport in the martian subsurface

Author

Stevens, A. H., Patel, M. R., Ringrose, T. J., Lewis, S. R., Leese, M. R., Stevens, A. H., Patel, M. R., Ringrose, T. J., Lewis, S. R., and Leese, M. R.

Abstract

A number of sources have been proposed for the methane observed in the atmosphere of Mars [1]. Serpentinisation could be a deep geologic source of the gas, where mafic minerals interact with a subsurface water table. [2] If so, the methane produced would have to travel through kilometres of megaregolith before entering the atmosphere. Although the structure of the martian subsurface is poorly known, this transport can be modelled using carefully chosen parameters and a modified form of Fick’s laws [3]. Such a model can be used to estimate transport timescales and investigate the properties of release. Methane clathrate hydrates are a potentially shallower methane source as they could be stable up to depths of only a few metres near the martian poles. The dissociation of these deposits could more easily explain the observed variation of methane in the atmosphere, as they would be more directly influenced by surface temperature changes [4]. To investigate the potential contributions of methane clathrate hydrates, we create samples in the lab and investigate their behaviour under Mars conditions in environmental simulation chambers. Combining the results of these models and experiments with data from future missions such as the ExoMars Trace Gas Orbiter will allow constraints to be placed on the potential sources of trace gases observed in the martian atmosphere. 1. Atreya, S.K., et al., Planetary and Space Science, 2011. 59(2-3): p. 133-136. 2. Oze, C. and M. Sharma, Geophys. Res. Lett., 2005. 32(10): p. L10203. 3. Sizemore, H.G. and M.T. Mellon, Icarus, 2008. 197(2): p. 606-620. 4. Root, M.J. and M.E. Elwood Madden, Icarus, 2012. 218(1): p. 534-544.

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