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4. The Castalia Mission to Main Belt Comet 133P/Elst-Pizarro

Author

Snodgrass, C., Jones, G. H., Boehnhardt, H., Gibbings, A., Homeister, M., Andre, N., Beck, P., Bentley, M. S., Bertini, I., Bowles, N., Capria, M. T., Carr, C., Ceriotti, M., Coates, A. J., Della Corte, V., Hanna, K. L. Donaldson, Fitzsimmons, A., Gutierrez, P. J., Hainaut, O. R., Herique, A., Hilchenbach, M., Hsieh, H. H., Jehin, E., Karatekin, O., Kofman, W., Lara, L. M., Laudan, K., Licandro, J., Lowry, S. C., Marzari, F., Masters, A., Meech, K. J., Moreno, F., Morse, A., Orosei, R., Pack, A., Plettemeier, D., Prialnik, D., Rotundi, A., Rubin, M., Sanchez, J. P., Sheridan, S., Trieloff, M., and Winterboer, A.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

We describe Castalia, a proposed mission to rendezvous with a Main Belt Comet (MBC), 133P/Elst-Pizarro. MBCs are a recently discovered population of apparently icy bodies within the main asteroid belt between Mars and Jupiter, which may represent the remnants of the population which supplied the early Earth with water. Castalia will perform the first exploration of this population by characterising 133P in detail, solving the puzzle of the MBC's activity, and making the first in situ measurements of water in the asteroid belt. In many ways a successor to ESA's highly successful Rosetta mission, Castalia will allow direct comparison between very different classes of comet, including measuring critical isotope ratios, plasma and dust properties. It will also feature the first radar system to visit a minor body, mapping the ice in the interior. Castalia was proposed, in slightly different versions, to the ESA M4 and M5 calls within the Cosmic Vision programme. We describe the science motivation for the mission, the measurements required to achieve the scientific goals, and the proposed instrument payload and spacecraft to achieve these., Comment: Accepted for publication in Advances in Space Research (special issue on Small Body Exploration). 30 pages

Published
2017
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6. A cosmic dust detection suite for the deep space Gateway

Author

Wozniakiewicz, P.J., Bridges, J., Burchell, M.J., Carey, W., Carpenter, J., Della Corte, V., Dignam, A., Genge, M.J., Hicks, L., Hilchenbach, M., Hillier, J., Kearsley, A.T., Krüger, H., Merouane, S., Palomba, E., Postberg, F., Schmidt, J., Srama, R., Trieloff, M., van-Ginneken, M., and Sterken, V.J.

Published
2021
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7. The formation of the solar system

Author

Pfalzner, S., Davies, M. B., Gounelle, M., Johansen, A., Muenker, C., Lacerda, P., Zwart, S. Portegies, Testi, L., Trieloff, M., and Veras, D.

Subjects
Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics
Abstract

The solar system started to form about 4.56 Gyr ago and despite the long intervening time span, there still exist several clues about its formation. The three major sources for this information are meteorites, the present solar system structure and the planet-forming systems around young stars. In this introduction we give an overview of the current understanding of the solar system formation from all these different research fields. This includes the question of the lifetime of the solar protoplanetary disc, the different stages of planet formation, their duration, and their relative importance. We consider whether meteorite evidence and observations of protoplanetary discs point in the same direction. This will tell us whether our solar system had a typical formation history or an exceptional one. There are also many indications that the solar system formed as part of a star cluster. Here we examine the types of cluster the Sun could have formed in, especially whether its stellar density was at any stage high enough to influence the properties of today's solar system. The likelihood of identifying siblings of the Sun is discussed. Finally, the possible dynamical evolution of the solar system since its formation and its future are considered., Comment: 36 pages, 7 figures, invited review in Physica Scripta

Published
2015
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8. Early Thermal Evolution of Planetesimals and its Impact on Processing and Dating of Meteoritic Material

Author

Gail, H. -P., Trieloff, M., Breuer, D., and Spohn, T.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Radioisotopic ages for meteorites and their components provide constraints on the evolution of small bodies: timescales of accretion, thermal and aqueous metamorphism, differentiation, cooling and impact metamorphism. Realising that the decay heat of short-lived nuclides (e.g. 26Al, 60Fe), was the main heat source driving differentiation and metamorphism, thermal modeling of small bodies is of utmost importance to set individual meteorite age data into the general context of the thermal evolution of their parent bodies, and to derive general conclusions about the nature of planetary building blocks in the early solar system. As a general result, modelling easily explains that iron meteorites are older than chondrites, as early formed planetesimals experienced a higher concentration of short-lived nuclides and more severe heating. However, core formation processes may also extend to 10 Ma after formation of Calcium-Aluminum-rich inclusions (CAIs). A general effect of the porous nature of the starting material is that relatively small bodies (< few km) will also differentiate if they form within 2 Ma after CAIs. A particular interesting feature to be explored is the possibility that some chondrites may derive from the outer undifferentiated layers of asteroids that are differentiated in their interiors. This could explain the presence of remnant magnetization in some chondrites due to a planetary magnetic field., Comment: 24 pages, 9 figures, Accepted for publication as a chapter in Protostars and Planets VI, University of Arizona Press (2014), eds. H. Beuther, R. Klessen, C. Dullemond, Th. Henning

Published
2013
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13. Synergies between interstellar dust and heliospheric science with an interstellar probe

Author

Sterken, Veerle J, primary, Hunziker, S, additional, Dialynas, K, additional, Leitner, J, additional, Sommer, M, additional, Srama, R, additional, Baalmann, L R, additional, Li, A, additional, Herbst, K, additional, Galli, A, additional, Brandt, P, additional, Riebe, M, additional, Baggaley, W J, additional, Blanc, M, additional, Czechowski, A, additional, Effenberger, F, additional, Fields, B, additional, Frisch, P, additional, Horanyi, M, additional, Hsu, H-W, additional, Khawaja, N, additional, Krüger, H, additional, Kurth, W S, additional, Ligterink, N F W, additional, Linsky, J L, additional, Lisse, C, additional, Malaspina, D, additional, Miller, J A, additional, Opher, M, additional, Poppe, A R, additional, Postberg, F, additional, Provornikova, E, additional, Redfield, S, additional, Richardson, J, additional, Rowan-Robinson, M, additional, Scherer, K, additional, Shen, M M, additional, Slavin, J D, additional, Sternovsky, Z, additional, Stober, G, additional, Strub, P, additional, Szalay, J, additional, and Trieloff, M, additional

Published
2023
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14. The science case for an orbital mission to Uranus: Exploring the origins and evolution of ice giant planets

Author

Arridge, C.S., Achilleos, N., Agarwal, J., Agnor, C.B., Ambrosi, R., André, N., Badman, S.V., Baines, K., Banfield, D., Barthélémy, M., Bisi, M.M., Blum, J., Bocanegra-Bahamon, T., Bonfond, B., Bracken, C., Brandt, P., Briand, C., Briois, C., Brooks, S., Castillo-Rogez, J., Cavalié, T., Christophe, B., Coates, A.J., Collinson, G., Cooper, J.F., Costa-Sitja, M., Courtin, R., Daglis, I.A., de Pater, I., Desai, M., Dirkx, D., Dougherty, M.K., Ebert, R.W., Filacchione, G., Fletcher, L.N., Fortney, J., Gerth, I., Grassi, D., Grodent, D., Grün, E., Gustin, J., Hedman, M., Helled, R., Henri, P., Hess, S., Hillier, J.K., Hofstadter, M.H., Holme, R., Horanyi, M., Hospodarsky, G., Hsu, S., Irwin, P., Jackman, C.M., Karatekin, O., Kempf, S., Khalisi, E., Konstantinidis, K., Krüger, H., Kurth, W.S., Labrianidis, C., Lainey, V., Lamy, L.L., Laneuville, M., Lucchesi, D., Luntzer, A., MacArthur, J., Maier, A., Masters, A., McKenna-Lawlor, S., Melin, H., Milillo, A., Moragas-Klostermeyer, G., Morschhauser, A., Moses, J.I., Mousis, O., Nettelmann, N., Neubauer, F.M., Nordheim, T., Noyelles, B., Orton, G.S., Owens, M., Peron, R., Plainaki, C., Postberg, F., Rambaux, N., Retherford, K., Reynaud, S., Roussos, E., Russell, C.T., Rymer, A.M., Sallantin, R., Sánchez-Lavega, A., Santolik, O., Saur, J., Sayanagi, K.M., Schenk, P., Schubert, J., Sergis, N., Sittler, E.C., Smith, A., Spahn, F., Srama, R., Stallard, T., Sterken, V., Sternovsky, Z., Tiscareno, M., Tobie, G., Tosi, F., Trieloff, M., Turrini, D., Turtle, E.P., Vinatier, S., Wilson, R., and Zarka, P.

Published
2014
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25. He–Ne–Ar–N2–CO2 Systematics of Fernando de Noronha Mantle Xenoliths: Confirmation of Mantle Plume Origin.

Author

Buikin, A. I., Hopp, J., Kogarko, L. N., Verchovsky, A. B., and Trieloff, M.

Subjects
MANTLE plumes, HELIUM isotopes, INCLUSIONS in igneous rocks, NOBLE gases, FLUID inclusions, NEON, NITROGEN isotopes
Abstract

The Fernando de Noronha archipelago (southwest Atlantic, 345 km from the coast of Brazil) is considered as the result of mantle plume activity. However, data on the isotopic composition of helium and neon, which are, perhaps, the only unambiguous geochemical criterion for deep mantle plumes have not been published yet for the region. In this paper, we present the first data on the isotopic composition of helium, neon, argon, and nitrogen, obtained by stepwise crushing of mantle xenoliths from the basanites of the San José Formation. The results obtained may indicate that fluid inclusions contain the very first portions of the exsolved gases—they are ultra-depleted in helium in relation to neon and especially argon. This conclusion is also supported by He–Ar–CO2 systematics. The isotopic composition of helium (4He/3He = 31 879 ± 6796) and neon (21Ne/22Ne(mantle) = 0.0453 ± 0.0012) indicates that it was indeed a mantle plume, identical in noble gas composition to the Kerguelen plume. According to the Ar–Ne isotope systematics 40Ar/36Ar (mantle) = 7455 ± 2290. Nitrogen is characterized by a heavy isotopic composition (δ15N = +5.4 ± 0.2‰), which corresponds to the hypothesis of the subduction nature of nitrogen in deep mantle plumes. [ABSTRACT FROM AUTHOR]

Published
2022
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26. SARIM PLUS—sample return of comet 67P/CG and of interstellar matter

Author

Srama, R., Krüger, H., Yamaguchi, T., Stephan, T., Burchell, M., Kearsley, A. T., Sterken, V., Postberg, F., Kempf, S., Grün, E., Altobelli, N., Ehrenfreund, P., Dikarev, V., Horanyi, M., Sternovsky, Z., Carpenter, J. D., Westphal, A., Gainsforth, Z., Krabbe, A., Agarwal, J., Yano, H., Blum, J., Henkel, H., Hillier, J., Hoppe, P., Trieloff, M., Hsu, S., Mocker, A., Fiege, K., Green, S. F., Bischoff, A., Esposito, F., Laufer, R., Hyde, T. W., Herdrich, G., Fasoulas, S., Jäckel, A., Jones, G., Jenniskens, P., Khalisi, E., Moragas-Klostermeyer, G., Spahn, F., Keller, H. U., Frisch, P., Levasseur-Regourd, A. C., Pailer, N., Altwegg, K., Engrand, C., Auer, S., Silen, J., Sasaki, S., Kobayashi, M., Schmidt, J., Kissel, J., Marty, B., Michel, P., Palumbo, P., Vaisberg, O., Baggaley, J., Rotundi, A., and Röser, H. P.

Published
2012
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29. A cosmic dust detection suite for the deep space Gateway

Author

Wozniakiewicz, P. (P.J.), Bridges, J. (J.), Burchell, M. (M.J.), Carey, W. (W.), Carpenter, J. (J.), Corte, V. D. (V. Della), Dignam, A. (A.), Genge, M. (M.J.), Hicks, L. (L.), Hilchenbach, M. (M.), Hillier, J. (J.), Kearsley, A. (A.T.), Krüger, H. (H.), Merouane, S. (S.), Palomba, E. (E.), Postberg, F. (F.), Schmidt, J. (J.), Srama, R. (R.), Trieloff, M. (M.), van-Ginneken, M. (M.), Sterken, V. (V.J.), Wozniakiewicz, P. (P.J.), Bridges, J. (J.), Burchell, M. (M.J.), Carey, W. (W.), Carpenter, J. (J.), Corte, V. D. (V. Della), Dignam, A. (A.), Genge, M. (M.J.), Hicks, L. (L.), Hilchenbach, M. (M.), Hillier, J. (J.), Kearsley, A. (A.T.), Krüger, H. (H.), Merouane, S. (S.), Palomba, E. (E.), Postberg, F. (F.), Schmidt, J. (J.), Srama, R. (R.), Trieloff, M. (M.), van-Ginneken, M. (M.), and Sterken, V. (V.J.)

Abstract

The decade of the 2020s promises to be when humanity returns to space beyond Earth orbit, with several nations trying to place astronauts on the Moon, before going further into deep space. As part of such a programme, NASA and partner organisations, propose to build a Deep Space Gateway in lunar orbit by the mid-2020s. This would be visited regularly and offer a platform for science as well as for human activity. Payloads that can be mounted externally on the Gateway offer the chance to, amongst other scientific goals, monitor and observe the dust flux in the vicinity of the Moon. This paper looks at relevant technologies to measure dust which will impact the exposed surface at high speed. Flux estimates and a model payload of detectors are described. It is predicted that the flux is sufficient to permit studies of cometary vs. asteroidal dust and their composition, and to sample interstellar dust streams. This may also be the last opportunity to measure the natural dust flux near the Moon before the current, relatively pristine environment, is contaminated by debris, as humanity’s interest in the Moon generates increased activity in that vicinity in coming decades.

Published
2021

32. Источники и эволюция флюидной фазы карбонатитов Гулинского массива (Западная Сибирь): обобщение данных по изотопному составу He, Ne, Ar, N 2 , CO 2 и H 2 O, полученных методом ступенчатого дробления

Author

Буйкин, А. И., primary, Hopp, J., additional, Верховский, А. Б., additional, Когарко, Л. Н., additional, and Trieloff, M., additional

Published
2021
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34. Sierra Gorda 009: A New Member of the Metal-Rich G Chondrites Grouplet

Author

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

Abstract

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

Published
2020

35. The Sources and Evolution of Fluid Phases of Guli Massif Carbonatites (West Siberia): Summarizing of Noble Gases, N2, CO2, H2O Stepwise Crushing Data.

Author

Buikin, A. I., Hopp, J., Verchovsky, A. B., Kogarko, L. N., and Trieloff, M.

Subjects
CARBONATITES, NEON, NOBLE gases, CARBON isotopes, FLUIDS, ARGON, HIGH temperatures
Abstract

Here we present summarizing of isotopic compositions and element ratios of noble gases, nitrogen, carbon and hydrogen in carbonatites of different generations of the Guli massif (West Siberia, Russia) obtained by stepwise crushing. The data point to the subcontinental lithospheric mantle (SCLM) as a primary source of the fluid phase in Guli carbonatites. However, the estimated 40Ar/36Ar ratio in the Guli mantle source of about 5400 is similar to the Kola plume value of 5000 ± 1000 (Marty et al., 1998). One explanation of such a low estimated 40Ar/36Ar ratio in the mantle end-member with SCLM type helium (4Не/3Не ~ 120000) and neon (21Nе/22Nеmantle ~ 0.7) is an admixture of atmospheric argon to the local mantle source. This assumption is supported by the Ar-Ne systematics as well as by the data for hydrogen isotopic composition. Early carbonatite differs significantly from the later ones by the concentration of highly volatile components, as well as by the isotopic compositions of carbon (CO2), argon, and hydrogen (H2O). The mantle component dominated in fluids at the early formation stages of the Guli massif rocks, whereas the late stages of carbonatite formation were characterized by an additional fluid source, which introduced atmospheric argon and neon, and most likely a high portion of CO2 with isotopically heavy carbon. The argon-neon-hydrogen isotope systematics suggest that the most plausible source of these late stage fluids are high temperature paleometeoric waters. The absence of a plume signature could be explained in terms that Guli carbonatites have been formed at the waning stage of plume magmatic activity with an essential input of SCLM components. [ABSTRACT FROM AUTHOR]

Published
2021
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36. Noble gases and radionuclides in Washington County iron meteorite

Author

Ott, U., Vogt, M., Merchel, S., Hopp, J., Koll, D., Lachner, J., Trieloff, M., and Wallner, A.

Subjects
AMS, meteorite
Abstract

The Washington County iron meteorite is unique in that it contains solar-type noble gases (He and Ne). We report additional noble gas analyses, supplemented by radionuclide data obtained at ANU (Canberra) and VERA (Univ. Vienna). Activities in dpm/kg measured on two specimens taken close to those analyzed for noble gases are: 5.15/5.40 (¹⁰Be); 3.46/2.66 (²⁶Al); 23.7/22.2 (³⁶Cl); 425/448 (⁵³Mn). ⁶⁰Fe is 1.09/1.29 dpm/kg Ni. Both cosmogenic noble gases and radionuclides indicate a preatmospheric radius of at most 15 cm. The ³⁶Cl-³⁶Ar cosmic ray exposure age of ~120 Ma agrees well with that of [1] based on noble gases only and is in disagreement with the much longer age (575 Ma) obtained by [2] using the ⁴¹K/⁴⁰K method. The new noble gas data further confirm that the solar noble gases are volume-correlated, an inference being that the Earth’s iron core may constitute a potential source reservoir for the solar-type Ne observed in terrestrial mantle materials. We thank S. Beutner for ICP-MS analyses. [1] Vogt, M. (2018), PhD Diss., Univ. Heidelberg. [2] Voshage, H. (1967) Z. Naturforsch 22a, 477–506.

Published
2019

39. Ar-40 to Ar-39 dating of pseudotachylites from the Witwatersrand basin, South Africa, with implications for the formation of the Vredefort Dome

Author

Trieloff, M, Kunz, J, Jessberger, E. K, Reimold, W. U, Boer, R. H, and Jackson, M. C

Subjects
Geophysics
Abstract

The formation of the Vredefort Dome, a structure in excess of 100 km in diameter and located in the approximate center of the Witwatersrand basin, is still the subject of lively geological controversy. It is widely accepted that its formation seems to have taken place in a single sudden event, herein referred to as the Vredefort event, accompanied by the release of gigantic amounts of energy. It is debated, however, whether this central event was an internal one, i.e., a cryptoexplosion triggered by volcanic or tectonic processes, or the impact of an extraterrestrial body. The results of this debate are presented.

Published
1992

40. Ar-40 to Ar-39 ages of the large impact structures Kara and Manicouagan and their relevance to the Cretaceous-Tertiary and the Triassic-Jurassic boundary

Author

Trieloff, M and Jessberger, E. K

Subjects
Geophysics
Abstract

Since the discovery of the Ir enrichment in Cretaceous-Tertiary boundary clays in 1980, the effects of a 10-km asteroid impacting on the Earth 65 Ma ago have been discussed as the possible reason for the mass extinction--including the extinction of the dinosaurs--at the end of the Cretaceous. But up to now no crater of this age that is large enough (ca. 200 km in diameter) has been found. One candidate is the Kara Crater in northern Siberia. Kolesnikov et al. determined a K-Ar isochron of 65.6 +/- 0.5 Ma, indistinguishable from the age of the K-T boundary and interpreted this as confirmation of earlier proposals that the Kara bolide would have been at least one of the K-T impactors. Koeberl et al. determined Ar-40 to Ar-39 ages ranging from 70 to 82 Ma and suggested an association to the Campanian-Maastrichtian boundary, another important extinction horizon 73 Ma ago. We dated four impact melts, KA2-306, KA2-305, SA1-302, and AN9-182. Results from the investigation are discussed.

Published
1992

41. The Castalia mission to Main Belt Comet 133P/Elst-Pizarro

Author

Snodgrass, C., primary, Jones, G.H., additional, Boehnhardt, H., additional, Gibbings, A., additional, Homeister, M., additional, Andre, N., additional, Beck, P., additional, Bentley, M.S., additional, Bertini, I., additional, Bowles, N., additional, Capria, M.T., additional, Carr, C., additional, Ceriotti, M., additional, Coates, A.J., additional, Della Corte, V., additional, Donaldson Hanna, K.L., additional, Fitzsimmons, A., additional, Gutiérrez, P.J., additional, Hainaut, O.R., additional, Herique, A., additional, Hilchenbach, M., additional, Hsieh, H.H., additional, Jehin, E., additional, Karatekin, O., additional, Kofman, W., additional, Lara, L.M., additional, Laudan, K., additional, Licandro, J., additional, Lowry, S.C., additional, Marzari, F., additional, Masters, A., additional, Meech, K.J., additional, Moreno, F., additional, Morse, A., additional, Orosei, R., additional, Pack, A., additional, Plettemeier, D., additional, Prialnik, D., additional, Rotundi, A., additional, Rubin, M., additional, Sánchez, J.P., additional, Sheridan, S., additional, Trieloff, M., additional, and Winterboer, A., additional

Published
2018
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42. Macromolecular organic compounds from the depths of Enceladus

Author

Postberg, F. (Frank), Khawaja, N. (Nozair), Abel, B. (Bernd), Choblet, G. (Gael), Glein, C. R. (Christopher R.), Gudipati, M. S. (Murthy S.), Henderson, B. L. (Bryana L.), Hsu, H.-W. (Hsiang-Wen), Kempf, S. (Sascha), Klenner, F. (Fabian), Moragas-Klostermeyer, G. (Georg), Magee, B. (Brian), Nölle, L. (Lenz), Perry, M. (Mark), Reviol, R. (René), Schmidt, J. (Jürgen), Srama, R. (Ralf), Stolz, F. (Ferdinand), Tobie, G. (Gabriel), Trieloff, M. (Mario), Waite, J. H. (J. Hunter), Postberg, F. (Frank), Khawaja, N. (Nozair), Abel, B. (Bernd), Choblet, G. (Gael), Glein, C. R. (Christopher R.), Gudipati, M. S. (Murthy S.), Henderson, B. L. (Bryana L.), Hsu, H.-W. (Hsiang-Wen), Kempf, S. (Sascha), Klenner, F. (Fabian), Moragas-Klostermeyer, G. (Georg), Magee, B. (Brian), Nölle, L. (Lenz), Perry, M. (Mark), Reviol, R. (René), Schmidt, J. (Jürgen), Srama, R. (Ralf), Stolz, F. (Ferdinand), Tobie, G. (Gabriel), Trieloff, M. (Mario), and Waite, J. H. (J. Hunter)

Abstract

Saturn’s moon Enceladus harbours a global water ocean¹, which lies under an ice crust and above a rocky core². Through warm cracks in the crust³ a cryo-volcanic plume ejects ice grains and vapour into space⁴–⁷ that contain materials originating from the ocean⁸,⁹. Hydrothermal activity is suspected to occur deep inside the porous core¹⁰–¹², powered by tidal dissipation¹³. So far, only simple organic compounds with molecular masses mostly below 50 atomic mass units have been observed in plume material⁶,¹⁴,¹⁵. Here we report observations of emitted ice grains containing concentrated and complex macromolecular organic material with molecular masses above 200 atomic mass units. The data constrain the macromolecular structure of organics detected in the ice grains and suggest the presence of a thin organic-rich film on top of the oceanic water table, where organic nucleation cores generated by the bursting of bubbles allow the probing of Enceladus’ organic inventory in enhanced concentrations.

Published
2018

43. The Castalia mission to Main Belt Comet 133P/Elst-Pizarro

Author

Snodgrass, C., Jones, G.H., Boehnhardt, H., Gibbings, A., Homeister, M., Andre, N., Beck, P., Bentley, M.S., Bertini, I., Bowles, N., Capria, M.T., Carr, C., Ceriotti, M., Coates, A.J., Della Corte, V., Donaldson Hanna, K.L., Fitzsimmons, A., Gutiérrez, P.J., Hainaut, O.R., Herique, A., Hilchenbach, M., Hsieh, H.H., Jehin, E., Karatekin, O., Kofman, W., Lara, L.M., Laudan, K., Licandro, J., Lowry, S.C., Marzari, F., Masters, A., Meech, K.J., Moreno, F., Morse, A., Orosei, R., Pack, A., Plettemeier, D., Prialnik, D., Rotundi, A., Rubin, M., Sánchez, J.P., Sheridan, S., Trieloff, M., Winterboer, A., Snodgrass, C., Jones, G.H., Boehnhardt, H., Gibbings, A., Homeister, M., Andre, N., Beck, P., Bentley, M.S., Bertini, I., Bowles, N., Capria, M.T., Carr, C., Ceriotti, M., Coates, A.J., Della Corte, V., Donaldson Hanna, K.L., Fitzsimmons, A., Gutiérrez, P.J., Hainaut, O.R., Herique, A., Hilchenbach, M., Hsieh, H.H., Jehin, E., Karatekin, O., Kofman, W., Lara, L.M., Laudan, K., Licandro, J., Lowry, S.C., Marzari, F., Masters, A., Meech, K.J., Moreno, F., Morse, A., Orosei, R., Pack, A., Plettemeier, D., Prialnik, D., Rotundi, A., Rubin, M., Sánchez, J.P., Sheridan, S., Trieloff, M., and Winterboer, A.

Abstract

We describe Castalia, a proposed mission to rendezvous with a Main Belt Comet (MBC), 133P/Elst-Pizarro. MBCs are a recently discovered population of apparently icy bodies within the main asteroid belt between Mars and Jupiter, which may represent the remnants of the population which supplied the early Earth with water. Castalia will perform the first exploration of this population by characterising 133P in detail, solving the puzzle of the MBC’s activity, and making the first in situ measurements of water in the asteroid belt. In many ways a successor to ESA’s highly successful Rosetta mission, Castalia will allow direct comparison between very different classes of comet, including measuring critical isotope ratios, plasma and dust properties. It will also feature the first radar system to visit a minor body, mapping the ice in the interior. Castalia was proposed, in slightly different versions, to the ESA M4 and M5 calls within the Cosmic Vision programme. We describe the science motivation for the mission, the measurements required to achieve the scientific goals, and the proposed instrument payload and spacecraft to achieve these.

Published
2018

44. The Castalia mission to Main Belt Comet 133P/Elst-Pizarro

Author

Science and Technology Facilities Council (UK), European Southern Observatory, Snodgrass, C., Jones, G. H., Boehnhardt, H., Gibbings, A., Homeister, M., Andre, N., Beck, P., Bentley, M. S., Bertini, I., Bowles, Neil, Capria, M. T., Carr, C., Ceriotti, M., Coates, A. J., Della Corte, V., Donaldson Hanna, K. L., Fitzsimmons, A., Gutiérrez, Pedro J., Hainaut, O. R., Herique, A., Hilchenbach, M., Hsieh, H. H., Jehin, E., Karatekin, O., Kofman, W., Lara, Luisa María, Laudan, K., Licandro, J., Lowry, S. C., Marzari, F., Masters, A., Meech, K. J., Moreno, Fernando, Morse, A., Orosei, R., Pack, A., Plettemeier, D., Prialnik, D., Rotundi, A., Rubin, M., Sánchez, J. P., Sheridan, S., Trieloff, M., Winterboer, A., Science and Technology Facilities Council (UK), European Southern Observatory, Snodgrass, C., Jones, G. H., Boehnhardt, H., Gibbings, A., Homeister, M., Andre, N., Beck, P., Bentley, M. S., Bertini, I., Bowles, Neil, Capria, M. T., Carr, C., Ceriotti, M., Coates, A. J., Della Corte, V., Donaldson Hanna, K. L., Fitzsimmons, A., Gutiérrez, Pedro J., Hainaut, O. R., Herique, A., Hilchenbach, M., Hsieh, H. H., Jehin, E., Karatekin, O., Kofman, W., Lara, Luisa María, Laudan, K., Licandro, J., Lowry, S. C., Marzari, F., Masters, A., Meech, K. J., Moreno, Fernando, Morse, A., Orosei, R., Pack, A., Plettemeier, D., Prialnik, D., Rotundi, A., Rubin, M., Sánchez, J. P., Sheridan, S., Trieloff, M., and Winterboer, A.

Abstract

We describe Castalia, a proposed mission to rendezvous with a Main Belt Comet (MBC), 133P/Elst-Pizarro. MBCs are a recently discovered population of apparently icy bodies within the main asteroid belt between Mars and Jupiter, which may represent the remnants of the population which supplied the early Earth with water. Castalia will perform the first exploration of this population by characterising 133P in detail, solving the puzzle of the MBC's activity, and making the first in situ measurements of water in the asteroid belt. In many ways a successor to ESA's highly successful Rosetta mission, Castalia will allow direct comparison between very different classes of comet, including measuring critical isotope ratios, plasma and dust properties. It will also feature the first radar system to visit a minor body, mapping the ice in the interior. Castalia was proposed, in slightly different versions, to the ESA M4 and M5 calls within the Cosmic Vision programme. We describe the science motivation for the mission, the measurements required to achieve the scientific goals, and the proposed instrument payload and spacecraft to achieve these. © 2017 COSPAR

Published
2018

49. Annama H chondrite—Mineralogy, physical properties, cosmic ray exposure, and parent body history

Author

Kohout, T., Haloda, J., Halodová, P., Meier, M. M. M., Maden, C., Busemann, H., Laubenstein, M., Caffee, M. W., Welten, K. C., Hopp, J., Trieloff, M., Mahajan, R. R., Naik, S., Trigo-Rodriguez, J. M., Moyano-Cambero, C. E., Oshtrakh, M. I., Maksimova, A. A., Chukin, A. V., Semionkin, V. A., Karabanalov, M. S., Felner, I., Petrova, E. V., Brusnitsyna, E. V., Grokhovsky, V. I., Yakovlev, G. A., Gritsevich, M., Lyytinen, E., Moilanen, J., Kruglikov, N. A., Ishchenko, A. V., Kohout, T., Haloda, J., Halodová, P., Meier, M. M. M., Maden, C., Busemann, H., Laubenstein, M., Caffee, M. W., Welten, K. C., Hopp, J., Trieloff, M., Mahajan, R. R., Naik, S., Trigo-Rodriguez, J. M., Moyano-Cambero, C. E., Oshtrakh, M. I., Maksimova, A. A., Chukin, A. V., Semionkin, V. A., Karabanalov, M. S., Felner, I., Petrova, E. V., Brusnitsyna, E. V., Grokhovsky, V. I., Yakovlev, G. A., Gritsevich, M., Lyytinen, E., Moilanen, J., Kruglikov, N. A., and Ishchenko, A. V.

Abstract

The fall of the Annama meteorite occurred early morning (local time) on April 19, 2014 on the Kola Peninsula (Russia). Based on mineralogy and physical properties, Annama is a typical H chondrite. It has a high Ar-Ar age of 4.4 Ga. Its cosmic ray exposure history is atypical as it is not part of the large group of H chondrites with a prominent 7–8 Ma peak in the exposure age histograms. Instead, its exposure age is within uncertainty of a smaller peak at 30 ± 4 Ma. The results from short-lived radionuclides are compatible with an atmospheric pre-entry radius of 30–40 cm. However, based on noble gas and cosmogenic radionuclide data, Annama must have been part of a larger body (radius >65 cm) for a large part of its cosmic ray exposure history. The 10Be concentration indicates a recent (3–5 Ma) breakup which may be responsible for the Annama parent body size reduction to 30–35 cm pre-entry radius. © The Meteoritical Society, 2017.

Published
2017

50. CASTALIA : A mission to a main belt comet

Author

Jones, G. H., Altwegg, K., Bertini, I., Bieler, A., Boehnhardt, H., Bowles, N., Braukhane, A., Capria, M., T., Coates, A. J., Ciarletti, Valérie, Davidsson, B., Engrand, Cécile, Fitzsimmons, A., Gibbings, A., Hainaut, O., Hallmann, M., Herique, Alain, Hilchenbach, M., Homeister, M., Hsieh, H., Jehin, E., Kofman, W., Lara, L. M., Licandro, J., Lowry, S.C., Moreno, F., Muinonen, Karri, Paetzold, M., Penttilä, Antti, Plettmeier, Dirk, Prialnik, D., Marboeuf, U., Marzari, F., Meech, Karen J., Rotundi, A., Smith, A., Snodgrass, C., Thomas, I., Trieloff, M., Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL), Physikalisches Institut [Bern], Universität Bern [Bern], Centro di Ateneo di Studi e Attività Spaziali 'Giuseppe Colombo' (CISAS), Universita degli Studi di Padova, Department of Atmospheric, Oceanic, and Space Sciences [Ann Arbor] (AOSS), University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, Department of Atmospheric, Oceanic and Planetary Physics [Oxford] (AOPP), University of Oxford [Oxford], DLR Institute of Space Systems, German Aerospace Center (DLR), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Department of Physics and Astronomy [Uppsala], Uppsala University, Centre de Spectrométrie Nucléaire et de Spectrométrie de Masse (CSNSM), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Astrophysics Research Centre [Belfast] (ARC), Queen's University [Belfast] (QUB), Department of Mechanical and Aerospace Engineering [Univ Strathclyde], University of Strathclyde [Glasgow], European Southern Observatory (ESO), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG ), Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), OHB Systems AG, Institute for Astronomy [Honolulu], University of Hawai‘i [Mānoa] (UHM), Academia Sinica Institute of Astronomy and Astrophysics (ASIAA), Academia Sinica, Institut d'Astrophysique et de Géophysique [Liège], Université de Liège, Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Instituto de Astrofisica de Canarias (IAC), Centre for Astrophysics and Planetary Science [Canterbury] (CAPS), University of Kent [Canterbury], Department of Physics [Helsinki], Falculty of Science [Helsinki], University of Helsinki-University of Helsinki, Universität zu Köln, Helsinki Institute of Physics (HIP), University of Helsinki, Technische Universität Dresden = Dresden University of Technology (TU Dresden), Tel Aviv University [Tel Aviv], Istituto Nazionale di Fisica Nucleare, Sezione di Padova (INFN, Sezione di Padova), Istituto Nazionale di Fisica Nucleare (INFN), Universita degli studi di Napoli 'Parthenope' [Napoli], The Open University [Milton Keynes] (OU), Universität Heidelberg [Heidelberg], IMPEC - LATMOS, Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Department of Mechanical and Aerospace Engineering [Glasgow], University of Strathclyde, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Technische Universität Dresden (TUD), National Institute for Nuclear Physics (INFN), Cardon, Catherine, Universität Bern [Bern] (UNIBE), Università degli Studi di Padova = University of Padua (Unipd), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), University of Oxford, Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Orbitale Hochtechnologie Bremen (OHB Systems AG), Helsingin yliopisto = Helsingfors universitet = University of Helsinki-Helsingin yliopisto = Helsingfors universitet = University of Helsinki, Universität zu Köln = University of Cologne, Helsingin yliopisto = Helsingfors universitet = University of Helsinki, Tel Aviv University (TAU), Università degli Studi di Napoli 'Parthenope' = University of Naples (PARTHENOPE), Universität Heidelberg [Heidelberg] = Heidelberg University, Mullard Space Science Laboratory ( MSSL ), University College of London [London] ( UCL ), Centro di Ateneo di Studi e Attività Spaziali 'Giuseppe Colombo' ( CISAS ), Universita degli Studi di Padova = University of Padua = Université de Padoue, Department of Atmospheric, Oceanic, and Space Sciences [Ann Arbor] ( AOSS ), Max-Planck-Institut für Sonnensystemforschung ( MPS ), Department of Atmospheric, Oceanic and Planetary Physics [Oxford] ( AOPP ), German Aerospace Center ( DLR ), Istituto di Astrofisica e Planetologia Spaziali ( IAPS ), Istituto Nazionale di Astrofisica ( INAF ), Laboratoire Atmosphères, Milieux, Observations Spatiales ( LATMOS ), Université de Versailles Saint-Quentin-en-Yvelines ( UVSQ ) -Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université de Versailles Saint-Quentin-en-Yvelines ( UVSQ ) -Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Centre de Spectrométrie Nucléaire et de Spectrométrie de Masse ( CSNSM ), Université Paris-Sud - Paris 11 ( UP11 ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Centre National de la Recherche Scientifique ( CNRS ), Astrophysics Research Centre [Belfast] ( ARC ), Queen's University [Belfast] ( QUB ), European Southern Observatory ( ESO ), Institut de Planétologie et d'Astrophysique de Grenoble ( IPAG ), Observatoire des Sciences de l'Univers de Grenoble ( OSUG ), Université Joseph Fourier - Grenoble 1 ( UJF ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université Grenoble Alpes ( UGA ) -Université Joseph Fourier - Grenoble 1 ( UJF ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université Grenoble Alpes ( UGA ) -Centre National de la Recherche Scientifique ( CNRS ), University of Hawaii at Manoa ( UHM ), Institute of Astronomy and Astrophysics [Taipei] ( ASIAA ), Instituto de Astrofísica de Andalucía ( IAA ), Consejo Superior de Investigaciones Científicas [Spain] ( CSIC ), Instituto de Astrofisica de Canarias ( IAC ), Centre for Astrophysics and Planetary Science [Canterbury] ( CAPS ), University of Helsinki [Helsinki], Helsinki Institute of Physics ( HIP ), Technische Universität Dresden ( TUD ), Istituto Nazionale di Fisica Nucleare, Sezione di Padova ( INFN, Sezione di Padova ), National Institute for Nuclear Physics ( INFN ), and The Open University [Milton Keynes] ( OU )

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

International audience; Main Belt Comets (MBCs), a type of Active Asteroid , constitute a newly identified class of solar system objects. They have stable, asteroid-like orbits and some exhibit a recurrent comet-like appearance. It is believed that they survived the age of the solar system in a dormant state and that their current ice sublimation driven activity only began recently. Buried water ice is the only volatile expected to survive under an insulating surface. Excavation by an impact can expose the ice and trigger the start of MBC activity. We present the case for a mission to one of these objects, to be submitted to the European Space Agency's current call for an M-class mission. The specific science goals of the Castalia mission are: 1. Characterize a new Solar System family, the MBCs, by in-situ investigation 2. Understand the physics of activity on MBCs 3. Directly sample water in the asteroid belt and test if MBCs are a viable source for Earth's water 4. Use the observed structure of an MBC as a tracer of planetary system formation and evolution.

Published
2015

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