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1. Irradiation dose affects the composition of organic refractory materials in space: Results from laboratory analogues

Author

Urso, R. G., Vuitton, V., Danger, G., d'Hendecourt, L. Le Sergeant, Flandinet, L., Djouadi, Z., Mivumbi, O., Orthous-Daunay, F. R., Ruf, A., Vinogradoff, V., Wolters, C., and Brunetto, R.

Subjects
Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Physics - Chemical Physics, Physics - Space Physics
Abstract

Context. Near- and mid-infrared observations have revealed the presence of organic refractory materials in the solar system, in cometary nuclei and on the surface of centaurs, Kuiper-belt and trans-neptunian objects. In these astrophysical environments, organic materials can be formed because of the interaction of frozen volatile compounds with cosmic rays, stellar/solar particles, and favoured by thermal processing. The analysis of laboratory analogues of such materials gives information on their properties, complementary to observations. Aims. We present new experiments to contribute in the understanding of the chemical composition of organic refractory materials in space. Methods. We bombard frozen water, methanol and ammonia mixtures with 40 keV H$^+$ and we warm the by-products up to 300~K. The experiments allow the production of organic residues that we analyse by means of infrared spectroscopy and by Very High Resolution Mass Spectrometry to study their chemical composition and their high molecular diversity, including the presence of hexamethylenetetramine and its derivatives. Results. We find that the accumulated irradiation dose plays a role in determining the residue's composition. Conslusions. Based on the laboratory doses, we estimate the astrophysical timescales to be short enough to induce an efficient formation of organic refractory materials at the surface of icy bodies in the outer solar system., Comment: in publication on Astronomy & Astrophysics, sect. Planets and planetary systems

Published
2020
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2. Detection of CH$_3$C$_3$N in Titan's Atmosphere

Author

Thelen, A. E., Cordiner, M. A., Nixon, C. A., Vuitton, V., Kisiel, Z., Charnley, S. B., Palmer, M. Y., Teanby, N. A., and Irwin, P. G. J.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Titan harbors a dense, organic-rich atmosphere primarily composed of N$_2$ and CH$_4$, with lesser amounts of hydrocarbons and nitrogen-bearing species. As a result of high sensitivity observations by the Atacama Large Millimeter/submillimeter Array (ALMA) in Band 6 ($\sim$230-272 GHz), we obtained the first spectroscopic detection of CH$_3$C$_3$N (methylcyanoacetylene or cyanopropyne) in Titan's atmosphere through the observation of seven transitions in the $J = 64\rightarrow63$ and $J = 62\rightarrow61$ rotational bands. The presence of CH$_3$C$_3$N on Titan was suggested by the Cassini Ion and Neutral Mass Spectrometer detection of its protonated form: C$_4$H$_3$NH$^+$, but the atmospheric abundance of the associated (deprotonated) neutral product is not well constrained due to the lack of appropriate laboratory reaction data. Here, we derive the column density of CH$_3$C$_3$N to be (3.8-5.7)$\times10^{12}$ cm$^{-2}$ based on radiative transfer models sensitive to altitudes above 400 km Titan's middle atmosphere. When compared with laboratory and photochemical model results, the detection of methylcyanoacetylene provides important constraints for the determination of the associated production pathways (such as those involving CN, CCN, and hydrocarbons), and reaction rate coefficients. These results also further demonstrate the importance of ALMA and (sub)millimeter spectroscopy for future investigations of Titan's organic inventory and atmospheric chemistry, as CH$_3$C$_3$N marks the heaviest polar molecule detected spectroscopically in Titan's atmosphere to date., Comment: 17 pages, 6 figures, 2 tables. Accepted in ApJ Letters

Published
2020
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4. ALMA Spectral Imaging of Titan Contemporaneous with Cassini's Grand Finale

Author

Cordiner, M. A., Teanby, N. A., Nixon, C. A., Vuitton, V., Thelen, A. E., and Charnley, S. B.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

The Cassini mission performed 127 targeted flybys of Titan during its 13-year mission to Saturn, culminating in the Grand Finale between April-September 2017. Here we demonstrate the use of the Atacama Large Millimeter/submillimeter Array (ALMA) to continue Cassini's legacy for chemical and climatological studies of Titan's atmosphere. Whole-hemisphere, interferometric spectral maps of HCN, HNC, HC3N, CH3CN, C2H3CN, C2H5CN and C3H8 were obtained using ALMA in May 2017 at moderate (~0.2'', or 1300 km) spatial resolution, revealing the effects of seasonally-variable chemistry and dynamics on the distribution of each species. The ALMA sub-mm observations of HCN and HC3N are consistent with Cassini infrared data on these species, obtained in the same month. Chemical/dynamical lifetimes of a few years are inferred for C2H3CN and C2H5CN, in reasonably close agreement with the latest chemical models incorporating sticking of C2H5CN to stratospheric aerosol particles. ALMA radial limb flux profiles provide column density information as a function of altitude, revealing maximum abundances in the thermosphere (above 600 km) for HCN, HNC, HC3N and C2H5CN. This constitutes the first detailed measurement of the spatial distribution of HNC, which is found to be confined predominantly to altitudes above 730 $\pm$ 60 km. The HNC emission map shows an east-west hemispheric asymmetry of (13$\pm$3)%. These results are consistent with very rapid production (and loss) of HNC in Titan's uppermost atmosphere, making this molecule an effective probe of short-timescale (diurnal) ionospheric processes., Comment: AJ; submitted March 2019; accepted for publication June 2019

Published
2019
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5. Identification of organic molecules with a laboratory prototype based on the Laser Ablation-CosmOrbitrap

Author

Selliez, L., Briois, C., Carrasco, N., Thirkell, L., Thissen, R., Ito, M., Orthous-Daunay, F. -R., Chalumeau, G., Colin, F., Cottin, H., Engrand, C., Flandinet, L., Fray, N., Gaubicher, B., Grand, N., Lebreton, J. -P., Makarov, A., Ruocco, S., Szopa, C., Vuitton, V., and Zapf, P.

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

In the Solar System, extra-terrestrial organic molecules have been found on cometary primitive objects, on Titan and Enceladus icy moons and on Mars. Identification could be achieved for simple organic species by remote sensing based on spectroscopic methods. However in situ mass spectrometry is a key technology to determine the nature of more complex organic matter. A new concept of mass analyser offering ultra-high mass resolving power of more than 50,000 at m/z 56 (under high vacuum condition about 10-9 mbar) is currently being developed for space applications: the CosmOrbitrap (Briois et al., 2016), based on the OrbitrapTM technology. This work challenges the use of LAb-CosmOrbitrap, a space instrument prototype combining Laser Ablation ionisation and the CosmOrbitrap mass analyser, to identify solid organic molecules of relevance to the future space exploration. For this purpose a blind test was jointly organised by the JAXA-HRMS team (Japan Aerospace Exploration Agency-High Resolution Mass Spectrometry) and the CosmOrbitrap consortium. The JAXA team provided two organic samples, whereas the CosmOrbitrap consortium analysed them without prior information. Thanks to the high analytical performances of the prototype and our HRMS data post-processing, we successfully identified the two molecules as HOBt, hydroxybenzotriazole (C6H5N3O) and BBOT, 2,5-Bis(5-tert-butyl-benzoxazol-2-yl)thiophene (C26H26N2O2S), with a mass resolving power of, respectively, 123 540 and 69 219. The success of this blind test on complex organic molecules shows the strong potential of LAb-CosmOrbitrap for future space applications.

Published
2019
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6. Interferometric imaging of Titan's HC$_3$N, H$^{13}$CCCN and HCCC$^{15}$N

Author

Cordiner, M. A., Nixon, C. A., Charnley, S. B., Teanby, N. A., Molter, E. M., Kisiel, Z., and Vuitton, V.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

We present the first maps of cyanoacetylene isotopologues in Titan's atmosphere, including H$^{13}$CCCN and HCCC$^{15}$N, detected in the 0.9 mm band using the Atacama Large Millimeter/submillimeter array (ALMA) around the time of Titan's (southern winter) solstice in May 2017. The first high-resolution map of HC$_3$N in its $v_7=1$ vibrationally excited state is also presented, revealing a unique snapshot of the global HC$_3$N distribution, free from the strong optical depth effects that adversely impact the ground-state ($v=0$) map. The HC$_3$N emission is found to be strongly enhanced over Titan's south pole (by a factor of 5.7 compared to the north pole), consistent with rapid photochemical loss of HC$_3$N from the summer hemisphere combined with production and transport to the winter pole since the April 2015 ALMA observations. The H$^{13}$CCCN/HCCC$^{15}$N flux ratio is derived at the southern HC$_3$N peak, and implies an HC$_3$N/HCCC$^{15}$N ratio of $67\pm14$. This represents a significant enrichment in $^{15}$N compared with Titan's main molecular nitrogen reservoir, which has a $^{14}$N/$^{15}$N ratio of 167, and confirms the importance of photochemistry in determining the nitrogen isotopic ratio in Titan's organic inventory., Comment: Accepted for publication in ApJL, May 2018

Published
2018
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8. Carbon chain anions and the growth of complex organic molecules in Titan's ionosphere

Author

Desai, R. T., Coates, A. J., Wellbrock, A., Vuitton, V., Crary, F. J., González-Caniulef, D., Shebanits, O., Jones, G. H., Lewis, G. R., Waite, J. H., Taylor, S. A., Kataria, D. O., Wahlund, J. -E., Edberg, N. J. T., and Sittler, E. C.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Cassini discovered a plethora of neutral and ionised molecules in Titan's ionosphere including, surprisingly, anions and negatively charged molecules extending up to 13,800 u/q. In this letter we forward model the Cassini electron spectrometer response function to this unexpected ionospheric component to achieve an increased mass resolving capability for negatively charged species observed at Titan altitudes of 950-1300 km. We report on detections consistently centered between 25.8-26.0 u/q and between 49.0-50.1 u/q which are identified as belonging to the carbon chain anions, CN$^-$/C$_3$N$^-$ and/or C$_2$H$^-$/C$_4$H$^-$, in agreement with chemical model predictions. At higher ionospheric altitudes, detections at 73-74 u/q could be attributed to the further carbon chain anions C$_5$N$^-$/C$_6$H$^-$ but at lower altitudes and during further encounters, extend over a higher mass/charge range. This, as well as further intermediary anions detected at $>$100 u, provide the first evidence for efficient anion chemistry in space involving structures other than linear chains. Furthermore, at altitudes below $\sim$1100 km, the low mass anions ($<$150 u/q) were found to deplete at a rate proportional to the growth of the larger molecules, a correlation that indicates the anions are tightly coupled to the growth process. This study adds Titan to an increasing list of astrophysical environments where chain anions have been observed and shows that anion chemistry plays a role in the formation of complex organics within a planetary atmosphere as well as in the interstellar medium., Comment: 8 pages, 3 figures, 1 table, Astrophysical Journal Letter accepted June 01 2017

Published
2017
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11. An estimate of the chemical composition of Titan's lakes

Author

Cordier, D., Mousis, O., Lunine, J. -I., Lavvas, P., and Vuitton, V.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Hundreds of radar-dark patches interpreted as lakes have been discovered in the north and south polar regions of Titan. We have estimated the composition of these lakes by using the direct abundance measurements from the Gas Chromatograph Mass Spectrometer (GCMS) aboard the Huygens probe and recent photochemical models based on the vertical temperature profile derived by the Huygens Atmospheric Structure Instrument (HASI). Thermodynamic equilibrium is assumed between the atmosphere and the lakes, which are also considered as nonideal solutions. We find that the main constituents of the lakes are ethane (C2H6) (~76-79%), propane (C3H8) (~7-8%), methane (CH4) (~5-10%), hydrogen cyanide (HCN) (~2-3%), butene (C4H8) (~1%), butane (C4H10) (~1%) and acetylene (C2H2) (~1%). The calculated composition of lakes is then substantially different from what has been expected from models elaborated prior to the exploration of Titan by the Cassini-Huygens spacecraft., Comment: 5 pages, 2 figures, accepted in ApJL

Published
2009
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12. Photochemical enrichment of deuterium in Titan's atmosphere: new insights from Cassini-Huygens

Author

Cordier, D., Mousis, O., Lunine, I. J., Moudens, A., and Vuitton, V.

Subjects
Astrophysics
Abstract

Cassini-Huygens data are used to re-examine the potential sources of the D/H enhancement over solar, measured in methane, in Titan's atmosphere. Assuming that the system is closed with respect to carbon, the use of constraints from the Huygens probe for the determination of the current mass of atmospheric methane and the most up-to-date determination of D/H from Cassini/CIRS infrared spectra allow us to show that photochemical enrichment of deuterium is not sufficient to be the sole mechanism yielding the measured D/H value. A possible fractionation between CH3D and CH4 during the escape process may slightly enhance the deuterium enrichment, but is not sufficient to explain the observed D/H value over the range of escape values proposed in the literature. Hence, alternative mechanisms such as a primordial deuterium enrichment must be combined with the photochemical enrichment in Titan's atmosphere in order to explain its current D/H value., Comment: 4 pages, 3 figures, accepted in ApJL

Published
2008
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13. Titan's cold case files - Outstanding questions after Cassini-Huygens

Author

Nixon, C.A., Lorenz, R.D., Achterberg, R.K., Buch, A., Coll, P., Clark, R.N., Courtin, R., Hayes, A., Iess, L., Johnson, R.E., Lopes, R.M.C., Mastrogiuseppe, M., Mandt, K., Mitchell, D.G., Raulin, F., Rymer, A.M., Todd Smith, H., Solomonidou, A., Sotin, C., Strobel, D., Turtle, E.P., Vuitton, V., West, R.A., and Yelle, R.V.

Published
2018
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31. 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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33. Irradiation dose affects the composition of organic refractory materials in space

Author

Urso, R. G., Vuitton, V., Danger, G., Le Sergeant d’Hendecourt, L., Flandinet, L., Djouadi, Z., Mivumbi, O., Orthous-Daunay, F. R., Ruf, A., Vinogradoff, V., Wolters, C., Brunetto, R., Institut d'astrophysique spatiale (IAS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Lunar and Planetary Laboratory [Tucson] (LPL), University of Arizona, Physique des interactions ioniques et moléculaires (PIIM), Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, ANR-16-CE29-0015,RAHIIA_SSOM,Analyses de résidus provenant d'analogues de glace interstellaire pour la compréhension de la formation de la matière organique du Système Solaire(2016), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), and Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)

Subjects
solid state: refractory, astrochemistry, methods: laboratory: solid state, astrobiology, Kuiper belt: general, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

International audience; Context. Near- and mid-infrared observations have revealed the presence of organic refractory materials in the Solar System, in cometary nuclei and on the surface of centaurs, Kuiper-belt and trans-neptunian objects. In these astrophysical environments, organic materials can be formed because of the interaction of frozen volatile compounds with cosmic rays and solar particles, and favoured by thermal processing. The analysis of laboratory analogues of such materials gives information on their properties, complementary to observations.Aims. We present new experiments to contribute to the understanding of the chemical composition of organic refractory materials in space.Methods. We bombard frozen water, methanol and ammonia mixtures with 40 keV H+ and we warmed the by-products up to 300 K. The experiments enabled the production of organic residues that we analysed by means of infrared spectroscopy and by very high resolution mass spectrometry to study their chemical composition and their high molecular diversity, including the presence of hexamethylenetetramine and its derivatives.Results. We find that the accumulated irradiation dose plays a role in determining the composition of the residue.Conclusions. Based on the laboratory doses, we estimate the astrophysical timescales to be short enough to induce an efficient formation of organic refractory materials at the surface of icy bodies in the outer Solar System.

Published
2020
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34. Testing tholins as analogues of the dark reddish material covering Pluto's Cthulhu region

Author

Fayolle-Chambe, M.S. (author), Quirico, E. (author), Schmitt, B. (author), Jovanovic, L. (author), Gautier, T. (author), Carrasco, N. (author), Grundy, W. (author), Vuitton, V. (author), Poch, O. (author), Protopapa, Silvia (author), Fayolle-Chambe, M.S. (author), Quirico, E. (author), Schmitt, B. (author), Jovanovic, L. (author), Gautier, T. (author), Carrasco, N. (author), Grundy, W. (author), Vuitton, V. (author), Poch, O. (author), and Protopapa, Silvia (author)

Abstract

Pluto's fly-by by the New Horizons spacecraft in July 2015 has revealed a dark reddish equatorial region, named Cthulhu, covered by a dark, non-icy material whose origin and composition have yet to be determined. It has been suggested that this material could form from the sedimentation of photochemical aerosols, originating from dissociation and ionisation processes in Pluto's high atmosphere (similarly to aerosols forming Titan's haze). This hypothesis is here further investigated by comparing New Horizons spectra collected both in the visible and the near-infrared to laboratory reflectance measurements of analogues of Pluto's aerosols (Pluto tholins). These aerosols were synthesised in conditions mimicking Pluto's atmosphere, and their optical and reflectance properties were determined, before being used in Hapke models. In particular, the single scattering albedo and phase function of Pluto tholins were retrieved through Hapke model inversion, performed from laboratory reflectance spectra collected under various geometries. From reconstructed reflectance spectra and direct comparison with New Horizons data, some of these tholins are shown to reproduce the photometric level (i.e. reflectance continuum) reasonably well in the near-infrared. Nevertheless, a misfit of the red visible slope still remains and tholins absorption bands present in the modelled spectra are absent in those collected by the New Horizons instruments. Several hypotheses are considered to explain the absence of these absorption features in LEISA data, namely high porosity effects or GCR irradiation. The formation of highly porous structures, which is currently our preferred scenario, could be promoted by either sublimation of ices initially mixed with the aerosols, or gentle deposition under Pluto's weak gravity., Astrodynamics & Space Missions

Published
2021
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35. Ion chemistry and N-containing molecules in Titan's upper atmosphere

Author

Vuitton, V., Yelle, R.V., and Mcewan, M.J.

Subjects
Astronomy, Earth sciences
Abstract

To link to full-text access for this article, visit this link: http://dx.doi.org/10.1016/j.icarus.2007.06.023 Byline: V. Vuitton (a), R.V. Yelle (a), M.J. McEwan (b) Keywords: Atmospheres; composition; Ionospheres; Organic chemistry; Titan Abstract: High-energy photons, electrons, and ions initiate ion-neutral chemistry in Titan's upper atmosphere by ionizing the major neutral species (nitrogen and methane). The Ion and Neutral Mass Spectrometer (INMS) onboard the Cassini spacecraft performed the first composition measurements of Titan's ionosphere. INMS revealed that Titan has the most compositionally complex ionosphere in the Solar System, with roughly 50 ions at or above the detection threshold. Modeling of the ionospheric composition constrains the density of minor neutral constituents, most of which cannot be measured with any other technique. The species identified with this approach include the most complex molecules identified so far on Titan. This confirms the long-thought idea that a very rich chemistry is actually taking place in this atmosphere. However, it appears that much of the interesting chemistry occurs in the upper atmosphere rather than at lower altitudes. The species observed by INMS are probably the first intermediates in the formation of even larger molecules. As a consequence, they affect the composition of the bulk atmosphere, the composition and optical properties of the aerosols and the flux of condensable material to the surface. In this paper, we discuss the production and loss reactions for the ions and how this affects the neutral densities. We compare our results to neutral densities measured in the stratosphere by other instruments, to production yields obtained in laboratory experiments simulating Titan's chemistry and to predictions of photochemical models. We suggest neutral formation mechanisms and highlight needs for new experimental and theoretical data. Author Affiliation: (a) Lunar and Planetary Laboratory, Kuiper Space Sciences Bldg, University of Arizona, 1629 E. University Blvd., Tucson, AZ 85721-0092, USA (b) Department of Chemistry, University of Canterbury, Christchurch, New Zealand Article History: Received 14 February 2007; Revised 30 May 2007

Published
2007

36. Experimental and theoretical study of hydrocarbon photochemistry applied to Titan stratosphere

Author

Vuitton, V., Doussin, J.-F., Benilan, Y., Raulin, F., and Gazeau, M.-C.

Subjects
Hydrocarbons -- Properties, Photochemistry -- Research, Titan (Satellite) -- Environmental aspects, Stratosphere -- Optical properties, Stratosphere -- Chemical properties, Astronomy, Earth sciences
Abstract

To link to full-text access for this article, visit this link: http://dx.doi.org/10.1016/j.icarus.2006.06.002 Byline: V. Vuitton (a)(b), J.-F. Doussin (b), Y. Benilan (b), F. Raulin (b), M.-C. Gazeau (b) Keywords: Photochemistry; Titan; Experimental techniques; Atmospheres; composition Abstract: None of the Titan photochemical models currently available have been able to reproduce the full set of stratospheric molecular mixing ratios inferred from observations. In order to assess how well reaction sets describe hydrocarbon chemistry, theoretical modeling predictions were compared to the results of a laboratory experiment. A CH.sub.4-C.sub.2H.sub.2 mixture was irradiated at 185 nm in an atmospheric simulation chamber and the evolution of the gas mixture was followed in situ and in real time by infrared spectroscopy. In parallel, a 0D theoretical model of the laboratory experiment was developed. A new reaction set describing Titan's chemistry was built and incorporated in the model. Lebonnois et al. [Lebonnois, S., Toublanc, D., Hourdin, F., Rannou, P., 2001. Icarus 152, 384-406] reaction set was also used for comparison. The presence of small amounts of atmospheric O.sub.2 in the experiment was properly accounted for and led us to suggest that oxygenated chemistry might be a source of C.sub.2H.sub.4 in Titan's atmosphere. With Lebonnois et al. [Lebonnois, S., Toublanc, D., Hourdin, F., Rannou, P., 2001. Icarus 152, 384-406] reaction set, the model could not fit at all the experimental evolution of the compounds. This is explained by some of the choices made for crucial kinetic parameters such as the quantum yield of photolysis of C.sub.2H.sub.2. Also, the absence of some reactions led to the enhancement of pathways that would otherwise be negligible. For example, the lack of reactions between C.sub.4H.sub.4 and radicals induced an erroneously high photolysis rate for this species. With the reaction set built in this study, the model much better fits the experiment, especially when the 'soot,' which includes C.sub.4H.sub.4, is recycled into C.sub.2H.sub.2. This shows that photochemistry of the larger species has a role in determining the lighter species concentrations and that considering that they are simply lost from the system is not a valid assumption. Including even an abridged set of C.sub.4 +hydrocarbon reactions will be required in future photochemical models. Especially, photolysis rates and yields for C.sub.2H.sub.2, C.sub.4H.sub.2, and C.sub.4H.sub.4, are important parameters in need of a better determination. Author Affiliation: (a) Lunar & Planetary Laboratory (LPL), University of Arizona, 1629 E. University Blvd., Tucson, AZ 85721-0092, USA (b) Laboratoire Interuniversitaire des Systemes Atmospheriques (LISA), Universite Paris 12 Val de Marne, 61 Ave. du General de Gaulle, Creteil Cedex 94010, France Article History: Received 6 October 2005; Revised 8 June 2006

Published
2006

37. Science goals and mission concepts for a future orbital and in situ exploration of Titan

Author

Rodriguez, S��bastien, Vinatier, Sandrine, Cordier, Daniel, Carrasco, Nathalie, Charnay, Benjamin, Cornet, Thomas, Coustenis, Athena, de Kok, Remco, Freissinet, Caroline, Galand, Marina, Geppert, Wolf D., Jauman, Ralf, Kalousova, Klara, Koskinen, Tommi T., Lebonnois, S��bastien, Gall, Alice Le, Mou��lic, St��phane Le, Lucas, Antoine, Mandt, Kathleen, Mastrogiuseppe, Marco, Nixon, Conor A., Radebaugh, Jani, Rannou, Pascal, Soderblom, Jason M., Solomonidou, Anezina, Sotin, Christophe, Stephan, Katrin, Teanby, Nick, Tobie, Gabriel, Vuitton, V��ronique, Institut de Physique du Globe de Paris (IPGP), and Centre National de la Recherche Scientifique (CNRS)-Université de La Réunion (UR)-Université Paris Diderot - Paris 7 (UPD7)-IPG PARIS-Institut national des sciences de l'Univers (INSU - CNRS)

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, [SDU.STU.GP]Sciences of the Universe [physics]/Earth Sciences/Geophysics [physics.geo-ph], FOS: Physical sciences, [SDU.STU.GM]Sciences of the Universe [physics]/Earth Sciences/Geomorphology, [SDU.ENVI]Sciences of the Universe [physics]/Continental interfaces, environment, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics - Earth and Planetary Astrophysics
Abstract

In this white paper, we present a cross-section of important scientific questions that remain partially or completely unanswered, ranging from Titan exosphere to the deep interior, and we detail which instrumentation and mission scenarios should be used to answer them. Our intention is to formulate the science goals for the next generation of planetary missions to Titan in order to prepare the future exploration of the moon. The ESA L-class mission concept that we propose is composed of a Titan orbiter and at least an in situ element (lake lander and/or drone(s))., White Paper submission to the call for ESA Voyage 2050 long-term plan

Published
2019

38. Comparison of Molecular Complexity Between Chondrites, Martian Meteorite and Lunar Soils

Author

Orthous-Daunay, F. -R, Wolters, C., Flandinet, L., Vuitton, V., Beck, P., Bonal, L., Isa, J., Moynier, F., Voisin, D., Moran, S., Horst, S., Gregoire Danger, Vinogradoff, V., Piani, L., Bekaert, D. V., Tissandier, L., Isono, Y., Tachibana, S., Naraoka, H., Remusat, L., Thissen, R., 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), McDonnell Center for Space Sciences, Washington University in St Louis, Laboratoire de glaciologie et géophysique de l'environnement (LGGE), Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS), School of Electrical and Computer Engineering - Georgia Insitute of Technology (ECE GeorgiaTech), Georgia Institute of Technology [Atlanta], Physique des interactions ioniques et moléculaires (PIIM), Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS), Centre de Recherches Pétrographiques et Géochimiques (CRPG), Université de Lorraine (UL)-Centre National de la Recherche Scientifique (CNRS), Department of Natural History Sciences, Hokkaido University, Laboratoire de minéralogie du Muséum National d'Histoire Naturelle (LMMNHN), Muséum national d'Histoire naturelle (MNHN)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Chimie Physique D'Orsay (LCPO), and Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS)

Subjects
[PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP]
Abstract

International audience; We compare typical polymerization patterns found in chondritic organic mixtures and the features found in martian meteorites and lunar soils.

Published
2019

39. Preparing sample return from Ryugu and Bennu asteroids with micrometeorites from the Concordia collection

Author

Duprat, J, Engrand, C, Dartois, E, Mathurin, J, Bernard, S, Le Guillou, C, Leroux, H, Vuitton, V, Orthous-Daunay, F.-R, Auge, B, Guerin, B, Rojas, J, Centre de Sciences Nucléaires et de Sciences de la Matière (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), Institut des Sciences Moléculaires d'Orsay (ISMO), Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Chimie Physique D'Orsay (LCPO), Université Paris-Sud - Paris 11 (UP11)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Institut de minéralogie, de physique des matériaux et de cosmochimie (IMPMC), Muséum national d'Histoire naturelle (MNHN)-Institut de recherche pour le développement [IRD] : UR206-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Unité Matériaux et Transformations - UMR 8207 (UMET), Centrale Lille-Institut de Chimie du CNRS (INC)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, Institut de Chimie du CNRS (INC)-Institut National de la Recherche Agronomique (INRA)-Centre National de la Recherche Scientifique (CNRS)-Université de Lille-Ecole Nationale Supérieure de Chimie de Lille (ENSCL), and Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)

Subjects
asteroid, interplanetary organic matter, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], micrometeorites, Solar System, space sample return mission
Abstract

International audience; Hayabusa 2 and OSIRIS-REx space missions will give a unique access to study the composition of carbonaceous asteroids. A key issue will be the comparison of the organic and mineral compounds from these near-Earth active carbonaceous asteroids with that of carbonaceous chondrites, carbon-rich interplanetary dust particles and cometary samples (81P/Wild2 or in-situ analyses from 67P/CG). The comparison of Ryugu and Bennu samples with chondritic micrometeorites and with extremely carbon-rich interplanetary dust particles such as the Ultra-Carbonaceous MicroMeteorites (UCAMMs) will provide a unique tool to assess their possible links with cometary organics. Analytical methods applied to study micrometeorites from Concordia collection (Antarctica) and the most recent results obtained will be summarised. A particular emphasis will be put on the dedicated experimental protocols that we developed to analyse such micrometeorite fragments and study their mineral-organic association at scales relevant to their intimate association, ranging from tens of nanometers to a few microns.

Published
2019

41. Liquid Chromatography Orbitrap Mass Spectrometry Study of Synthetic and Chondritic Organic Mixtures

Author

Wolters, C., Vuitton, V., Orthous-Daunay, F.-R., Flandinet, L., He, C., Moran, S., Horst, S., Bekaert, D., Tissandier, L., Marty, B., Piani, L., Vuitton, Véronique, 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), School of Electrical and Computer Engineering - Georgia Insitute of Technology (ECE GeorgiaTech), Georgia Institute of Technology [Atlanta], Centre de Recherches Pétrographiques et Géochimiques (CRPG), Université de Lorraine (UL)-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), 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 Grenoble Alpes [2016-2019] (UGA [2016-2019])-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 Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), and Institut national des sciences de l'Univers (INSU - CNRS)-Université de Lorraine (UL)-Centre National de la Recherche Scientifique (CNRS)

Subjects
[PHYS.ASTR.EP] Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP]
Abstract

International audience; Liquid chromatography Orbitrap mass spectrometry is used to compare extraterrestrial and synthetic organic matter. This analytical workflow brings information on the origin of the soluble organic matter present in carbonaceous chondrites.

Published
2019

42. Enrichment of heavy nitrogen in Titan's HC3N detected using ALMA

Author

Cordiner, M., Nixon, C. A., Charnley, S. B., Teanby, N. A., Molter, E. M., Kisiel, Z., Vuitton, V., NASA Goddard Space Flight Center (GSFC), School of Earth Sciences [Bristol], University of Bristol [Bristol], Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), 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 Grenoble Alpes [2016-2019] (UGA [2016-2019])-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 Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), 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), and Vuitton, Véronique

Subjects
[PHYS.ASTR.EP] Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], PLANETARY SCIENCES: SOLAR SYSTEM OBJECTS, 5210 Planetary atmospheres, PLANETARY SCIENCES: FLUID PLANETSDE: 6281 Titan, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], and hazes, clouds, PLANETARY SCIENCES: ASTROBIOLOGYDE: 5749 Origin and evolution, PLANETARY SCIENCES: ASTROBIOLOGYDE: 5215 Origin of life
Abstract

International audience; Trace isotopic ratios contain unique information on the chemical histories of atmospheric gases. From the combined efforts of previous ground and space-based sub-mm and infrared observations, Titan's atmospheric HCN has been found to be substantially enriched in 15N compared with the bulk N2 reservoir. This is theorized to occur as a consequence of isotope-selective photodissociation of N2 in the upper atmosphere, giving rise to an enhanced abundance of atomic 15N that subsequently becomes incorporated into HCN. Here, we present the first maps of cyanoacetylene isotopologues in Titan's atmosphere, including H13CCCN and HCCC15N, detected in the 0.9 mm band using the Atacama Large Millimeter/submillimeter array (ALMA) around the time of Titan's (southern winter) solstice in May 2017 (see Figure 1). The HC3N emission is found to be strongly enhanced over the south pole (by a factor of 5.7 compared to the north pole), consistent with rapid photochemical loss of HC3N from the summer hemisphere combined with production and transport to the winter pole since the previous (2015) ALMA observations. The H13CCCN/HCCC15N flux ratio is consistent with an HC3N/HCCC15N ratio of 67 ± 14, which is significantly enriched in 15N compared with the main molecular nitrogen reservoir (which has a 14N/15N ratio of 167). This confirms the importance of photochemistry in determining the nitrogen isotopic ratio in Titan's organic inventory. In this presentation I will discuss the impact of these results on our understanding of the origin of Titan's N2, the evolution of its atmospheric 14N/15N ratio, and on our knowledge of the detailed photochemical processes occurring in nitrogen-rich planetary atmospheres.

Published
2018

45. Identification of organic molecules with a laboratory prototype based on the Laser Ablation-CosmOrbitrap

Author

Selliez, L., primary, Briois, C., additional, Carrasco, N., additional, Thirkell, L., additional, Thissen, R., additional, Ito, M., additional, Orthous-Daunay, F.-R., additional, Chalumeau, G., additional, Colin, F., additional, Cottin, H., additional, Engrand, C., additional, Flandinet, L., additional, Fray, N., additional, Gaubicher, B., additional, Grand, N., additional, Lebreton, J.-P., additional, Makarov, A., additional, Ruocco, S., additional, Szopa, C., additional, Vuitton, V., additional, and Zapf, P., additional

Published
2019
Full Text
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47. Haze Production in the Atmospheres of super-Earths and mini-Neptunes: Insights from the Lab

Author

H��rst, Sarah M., He, Chao, Lewis, Nikole K., Kempton, Eliza M. -R., Marley, Mark S., Morley, Caroline V., Moses, Julianne I., Valenti, Jeff A., and Vuitton, V��ronique

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), FOS: Physical sciences, Astrophysics - Earth and Planetary Astrophysics
Abstract

Numerous solar system atmospheres possess aerosols including the characteristic organic hazes of Titan and Pluto. Haze particles substantially impact atmospheric temperatures structures and may provide organic material to the surface of a world, thereby affecting its habitability. Observations of exoplanet atmospheres suggest the presence of aerosols, especially in cooler (, 16 pages, 3 figures, 1 table, submitted to Nature Astronomy

Published
2018

50. Explorer of Enceladus and Titan (E2T): Investigating Ocean Worlds' Evolution and Habitability in the Saturn System

Author

Mitri, G., Postberg, F., Soderblom, J. M., Tobie, G., Tortora, P., Wurz, P., Barnes, J. W., Carrasco, N., Coustenis, A., Ferri, F., Hayes, A., Hillier, J., Kempf, S., Lebreton, J. P., Lorenz, R. D., OROSEI, ROBERTO, Petropoulos, A. E. E., Reh, K. R., Schmidt, J., Sotin, C., Srama, R., Vuitton, V., Yen, C. W., ITA, USA, GBR, FRA, DEU, FIN, and CHE

Abstract

The NASA-ESA-ASI Cassini-Huygens mission has revealed Titan and Enceladus to be two of the most enigmatic worlds in the Solar System. Titan, with its organically rich and dynamic atmosphere and geology, and Enceladus, with its active plume of water vapor and ice including trace amounts of organics, salts, and silica nano-particles, both harboring subsurface oceans, are prime environments to investigate the conditions for the emergence of life and the habitability potential of ocean worlds, as well as the origin and evolution of complex planetary systems. The Explorer of Enceladus and Titan (E2T) is a space mission concept dedicated to investigating the evolution and habitability of these Saturnian satellites and is proposed in response to ESA's M5 Cosmic Vision Call, as a medium-class mission led by ESA in collaboration with NASA. E2T has a focused state-of-the-art payload that will provide in-situ chemical analysis, and high-resolution imaging from multiple flybys of Enceladus and Titan using a solar-electric powered spacecraft in orbit around Saturn. With significant improvements in mass range and resolution, as compared with Cassini instrumentation, the Ion and Neutral Gas Mass Spectrometer (INMS) and the Enceladus Icy Jet Analyzer (ENIJA) time-of-flight mass spectrometers will provide the data needed to decipher the subtle details of the aqueous environment of Enceladus from plume sampling and of the complex pre-biotic chemistry occurring in Titan's atmosphere. The Titan Imaging and Geology, Enceladus Reconnaissance (TIGER) mid-wave infrared camera will map thermal emission from Enceladus' tiger stripes at meter scales and investigate Titan's geology and compositional variability at decameter scales.

Published
2016

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