Search

Your search keyword '"J. I. Lunine"' showing total 55 results
Start Over Author "J. I. Lunine"
55 results on '"J. I. Lunine"'

1. Science Goals and Mission Architecture of the Europa Lander Mission Concept

Author

K. P. Hand, C. B. Phillips, A. Murray, J. B. Garvin, E. H. Maize, R. G. Gibbs, G. Reeves, A. M. San Martin, G. H. Tan-Wang, J. Krajewski, K. Hurst, R. Crum, B. A. Kennedy, T. P. McElrath, J. C. Gallon, D. Sabahi, S. W. Thurman, B. Goldstein, P. Estabrook, S. W. Lee, J. A. Dooley, W. B. Brinckerhoff, K. S. Edgett, C. R. German, T. M. Hoehler, S. M. Hörst, J. I. Lunine, C. Paranicas, K. Nealson, D. E. Smith, A. S. Templeton, M. J. Russell, B. Schmidt, B. Christner, B. Ehlmann, A. Hayes, A. Rhoden, P. Willis, R. A. Yingst, K. Craft, M. E. Cameron, T. Nordheim, J. Pitesky, J. Scully, J. Hofgartner, S. W. Sell, K. J. Barltrop, J. Izraelevitz, E. J. Brandon, J. Seong, J.-P. Jones, J. Pasalic, K. J. Billings, J. P. Ruiz, R. V. Bugga, D. Graham, L. A. Arenas, D. Takeyama, M. Drummond, H. Aghazarian, A. J. Andersen, K. B. Andersen, E. W. Anderson, A. Babuscia, P. G. Backes, E. S. Bailey, D. Balentine, C. G. Ballard, D. F. Berisford, P. Bhandari, K. Blackwood, G. S. Bolotin, E. A. Bovre, J. Bowkett, K. T. Boykins, M. S. Bramble, T. M. Brice, P. Briggs, A. P. Brinkman, S. M. Brooks, B. B. Buffington, B. Burns, M. L. Cable, S. Campagnola, L. A. Cangahuala, G. A Carr, J. R. Casani, N. E. Chahat, B. K. Chamberlain-Simon, Y. Cheng, S. A. Chien, B. T. Cook, M. Cooper, M. DiNicola, B. Clement, Z. Dean, E. A. Cullimore, A. G. Curtis, J-P. de la Croix, P. Di Pasquale, E. M. Dodd, L. A. Dubord, J. A. Edlund, R. Ellyin, B. Emanuel, J. T. Foster, A. J. Ganino, G. J. Garner, M. T. Gibson, M. Gildner, K. J. Glazebrook, M. E. Greco, W. M. Green, S. J. Hatch, M. M. Hetzel, W. A. Hoey, A. E. Hofmann, R. Ionasescu, A. Jain, J. D. Jasper, J. R. Johannesen, G. K. Johnson, I. Jun, A. B. Katake, S. Y. Kim-Castet, D. I. Kim, W. Kim, E. F. Klonicki, B. Kobeissi, B. D. Kobie, J. Kochocki, M. Kokorowski, J. A. Kosberg, K. Kriechbaum, T. P. Kulkarni, R. L. Lam, D. F. Landau, M. A. Lattimore, S. L. Laubach, C. R. Lawler, G. Lim, J. Y Lin, T. E. Litwin, M. W. Lo, C. A. Logan, E. Maghasoudi, L. Mandrake, Y. Marchetti, E. Marteau, K. A. Maxwell, J. B. Mc Namee, O. Mcintyre, M. Meacham, J. P. Melko, J. Mueller, D. A. Muliere, A. Mysore, J. Nash, H. Ono, J. M. Parker, R. C. Perkins, A. E Petropoulos, A. Gaut, M. Y. Piette Gomez, R. P. Casillas, M. Preudhomme, G. Pyrzak, J. Rapinchuk, J. M. Ratliff, T. L. Ray, E. T. Roberts, K. Roffo, D. C. Roth, J. A. Russino, T. M. Schmidt, M. J. Schoppers, J. S. Senent, F. Serricchio, D. J. Sheldon, L. R. Shiraishi, J. Shirvanian, K. J. Siegel, G. Singh, A. R. Sirota, E. D. Skulsky, J. S. Stehly, N. J. Strange, S. U. Stevens, E. T. Sunada, S. P. Tepsuporn, L. P. C. Tosi, N. Trawny, I. Uchenik, V. Verma, R. A. Volpe, C. T. Wagner, D. Wang, R. G. Willson, J. L. Wolff, A. T. Wong, A. K. Zimmer, K. G. Sukhatme, K. A. Bago, Y. Chen, A. M. Deardorff, R. S. Kuch, C. Lim, M. L. Syvertson, G. A. Arakaki, A. Avila, K. J. DeBruin, A. Frick, J. R. Harris, M. C. Heverly, J. M. Kawata, S.-K. Kim, D. M. Kipp, J. Murphy, M. W. Smith, M. D. Spaulding, R. Thakker, N. Z. Warner, C. R. Yahnker, M. E. Young, T. Magner, D. Adams, P. Bedini, L. Mehr, C. Sheldon, S. Vernon, V. Bailey, M. Briere, M. Butler, A. Davis, S. Ensor, M. Gannon, A. Haapala-Chalk, T. Hartka, M. Holdridge, A. Hong, J. Hunt, J. Iskow, F. Kahler, K. Murray, D. Napolillo, M. Norkus, R. Pfisterer, J. Porter, D. Roth, P. Schwartz, L. Wolfarth, E. H. Cardiff, E. W. Grob, J. R. Adam, E. Betts, J. Norwood, M. M. Heller, T. Voskuilen, P. Sakievich, L. Gray, D. J. Hansen, K. W. Irick, J. C. Hewson, J. Lamb, S. C. Stacy, C. M. Brotherton, A. S Tappan, D. Benally, H. Thigpen, E. Ortiz, D. Sandoval, A. M. Ison, M. Warren, P. G. Stromberg, P. M. Thelen, B. Blasy, P. Nandy, A. W. Haddad, L. B. Trujillo, T. H. Wiseley, S. A. Bell, N. P. Teske, C. Post, L. Torres-Castro, C. Grosso, and M. Wasiolek

Published
2022
Full Text
View/download PDF

3. First Estimate of Wind Fields in the Jupiter Polar Regions From JIRAM‐Juno Images

Author

D. Grassi, A. Adriani, M. L. Moriconi, A. Mura, F. Tabataba‐Vakili, A. Ingersoll, G. Orton, C. Hansen, F. Altieri, G. Filacchione, G. Sindoni, B. M. Dinelli, F. Fabiano, S. J. Bolton, S. Levin, S. K. Atreya, J. I. Lunine, T. Momary, F. Tosi, A. Migliorini, G. Piccioni, R. Noschese, A. Cicchetti, C. Plainaki, A. Olivieri, D. Turrini, S. Stefani, R. Sordini, and M. Amoroso

Published
2018
Full Text
View/download PDF

4. Moonraker -- Enceladus Multiple Flyby Mission

Author

O. Mousis, A. Bouquet, Y. Langevin, N. André, H. Boithias, G. Durry, F. Faye, P. Hartogh, J. Helbert, L. Iess, S. Kempf, A. Masters, F. Postberg, J.-B. Renard, P. Vernazza, A. Vorburger, P. Wurz, D. H. Atkinson, S. Barabash, M. Berthomier, J. Brucato, M. Cable, J. Carter, S. Cazaux, A. Coustenis, G. Danger, V. Dehant, T. Fornaro, P. Garnier, T. Gautier, O. Groussin, L. Z. Hadid, J.-C. Ize, I. Kolmasova, J.-P. Lebreton, S. Le Maistre, E. Lellouch, J. I. Lunine, K. E. Mandt, Z. Martins, D. Mimoun, Q. Nenon, G. M. Muñoz Caro, P. Rannou, H. Rauer, P. Schmitt-Kopplin, A. Schneeberger, M. Simons, K. Stephan, T. Van Hoolst, J. Vaverka, M. Wieser, L. Wörner, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Physique des interactions ioniques et moléculaires (PIIM), Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS), UCL - SST/ELI/ELIC - Earth & Climate, Institut Universitaire de France (IUF), Ministère de l'Education nationale, de l’Enseignement supérieur et de la Recherche (M.E.N.E.S.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), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Airbus Defence and Space [Les Mureaux], ASTRIUM, Groupe de spectrométrie moléculaire et atmosphérique (GSMA), Université de Reims Champagne-Ardenne (URCA)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Max-Planck-Gesellschaft, DLR Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), Dipartimento di Ingegneria Meccanica e Aerospaziale [Roma La Sapienza] (DIMA), Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome] (UNIROMA), Laboratory for Atmospheric and Space Physics [Boulder] (LASP), University of Colorado [Boulder], Imperial College London, Institute of Geological Sciences [Berlin], Department of Earth Sciences [Berlin], Free University of Berlin (FU)-Free University of Berlin (FU), Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Physics Institute [Bern], University of Bern, Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Swedish Institute of Space Physics [Kiruna] (IRF), Laboratoire de Physique des Plasmas (LPP), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École polytechnique (X)-Sorbonne Université (SU)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto Nazionale di Astrofisica (INAF), Faculty of Aerospace Engineering [Delft], Delft University of Technology (TU Delft), Leiden Observatory [Leiden], Universiteit Leiden, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Royal Observatory of Belgium [Brussels] (ROB), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institute of Atmospheric Physics [Prague] (IAP), Czech Academy of Sciences [Prague] (CAS), Faculty of Mathematics and Physics [Praha/Prague], Charles University [Prague] (CU), Department of Astronomy [Ithaca], Cornell University [New York], Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), Centro de Quimica Estrutural (CQE), Instituto Superior Técnico, Universidade Técnica de Lisboa (IST), Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Max-Planck-Institut für Extraterrestrische Physik (MPE), Seismological Laboratory, California Institute of Technology, California Institute of Technology (CALTECH), and DLR In­sti­tute of Quan­tum Tech­nolo­gies

Subjects
530 Physics, ISOTOPOLOGUES, MU-M, FOS: Physical sciences, Saturnian satellites, Astronomy & Astrophysics, moon, Enceladus, [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, Earth and Planetary Sciences (miscellaneous), Interdisciplinary astronomy, INTERIOR STRUCTURE, ION, Habitable planets, Instrumentation and Methods for Astrophysics (astro-ph.IM), CALIBRATION, Earth and Planetary Astrophysics (astro-ph.EP), Science & Technology, SPECTROSCOPY, GRAVITY-FIELD, 520 Astronomy, 500 Naturwissenschaften und Mathematik::520 Astronomie::520 Astronomie und zugeordnete Wissenschaften, Astronomy and Astrophysics, CASSINI, Astrobiology, 620 Engineering, PLUME, Geophysics, Saturn, [SDU]Sciences of the Universe [physics], Space and Planetary Science, MASS-SPECTROMETER, Physical Sciences, Ocean planets, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

Enceladus, an icy moon of Saturn, possesses an internal water ocean and jets expelling ocean material into space. Cassini investigations indicated that the subsurface ocean could be a habitable environment having a complex interaction with the rocky core. Further investigation of the composition of the plume formed by the jets is necessary to fully understand the ocean, its potential habitability, and what it tells us about Enceladus' origin. Moonraker has been proposed as an ESA M-class mission designed to orbit Saturn and perform multiple flybys of Enceladus, focusing on traversals of the plume. The proposed Moonraker mission consists of an ESA-provided platform, with strong heritage from JUICE and Mars Sample Return, and carrying a suite of instruments dedicated to plume and surface analysis. The nominal Moonraker mission has a duration of 13.5 years. It includes a 23-flyby segment with 189 days allocated for the science phase, and can be expanded with additional segments if resources allow. The mission concept consists in investigating: i) the habitability conditions of present-day Enceladus and its internal ocean, ii) the mechanisms at play for the communication between the internal ocean and the surface of the South Polar Terrain, and iii) the formation conditions of the moon. Moonraker, thanks to state-of-the-art instruments representing a significant improvement over Cassini's payload, would quantify the abundance of key species in the plume, isotopic ratios, and physical parameters of the plume and the surface. Such a mission would pave the way for a possible future landed mission., Accepted for publication in The Planetary Science Journal

Published
2022

5. Jupiter's inhomogeneous envelope

Author

Y. Miguel, M. Bazot, T. Guillot, S. Howard, E. Galanti, Y. Kaspi, W. B. Hubbard, B. Militzer, R. Helled, S. K. Atreya, J. E. P. Connerney, D. Durante, L. Kulowski, J. I. Lunine, D. Stevenson, and S. Bolton

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), composition, Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics, Juppiter, planets and satellites: interiors, gaseous planets, formation, composition, formation, planets and satellites, planets and satellites, FOS: Physical sciences, Astronomy and Astrophysics, gaseous planets, planets and satellites, interiors, planets and satellites, interiors, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Physics::Space Physics, Astrophysics::Earth and Planetary Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics - Earth and Planetary Astrophysics
Abstract

While Jupiter's massive gas envelope consists mainly of hydrogen and helium, the key to understanding Jupiter's formation and evolution lies in the distribution of the remaining (heavy) elements. Before the Juno mission, the lack of high-precision gravity harmonics precluded the use of statistical analyses in a robust determination of the heavy-elements distribution in Jupiter's envelope. In this paper, we assemble the most comprehensive and diverse collection of Jupiter interior models to date and use it to study the distribution of heavy elements in the planet's envelope. We apply a Bayesian statistical approach to our interior model calculations, reproducing the Juno gravitational and atmospheric measurements and constraints from the deep zonal flows. Our results show that the gravity constraints lead to a deep entropy of Jupiter corresponding to a 1 bar temperature 5-15 K higher than traditionally assumed. We also find that uncertainties in the equation of state are crucial when determining the amount of heavy elements in Jupiter's interior. Our models put an upper limit to the inner compact core of Jupiter of 7 Earth masses, independently on the structure model (with or without dilute core) and the equation of state considered. Furthermore, we robustly demonstrate that Jupiter's envelope is inhomogenous, with a heavy-element enrichment in the interior relative to the outer envelope. This implies that heavy element enrichment continued through the gas accretion phase, with important implications for the formation of giant planets in our solar system and beyond., Accepted for publication in A&A

Published
2022

6. Titan Stratospheric Haze Bands Observed in Cassini VIMS as Tracers of Meridional Circulation

Author

N. W. Kutsop, A. G. Hayes, P. M. Corlies, S. Le Mouélic, J. I. Lunine, C. A. Nixon, P. Rannou, S. Rodriguez, M. T. Roman, C. Sotin, and T. Tokano

Subjects
Geophysics, Space and Planetary Science, Earth and Planetary Sciences (miscellaneous), Astronomy and Astrophysics
Abstract

We analyzed Cassini data to derive the nature and evolution of circumglobal annuli observed in the stratosphere of Titan, Saturn's largest moon. The annuli were observed between 2004 and 2017 in data acquired by the Visual and Infrared Mapping Spectrometer on board the Cassini spacecraft. We observed a north polar annulus, an equatorial annulus, and several secondary annuli. Pre-Cassini telescopic observations by the Hubble Space Telescope and Keck reported an atmospheric feature consistent with the presence of a south polar annulus between 1999 and 2001, although this feature was not observed by Cassini. Relative to the atmosphere near the annuli, they appear dark at 300–500 nm and bright in methane absorption channels such as the ones at 900 and 1150 nm. The stratosphere seems to rotate around the north pole. Alternatively, it seems to rotate about a point offset from solid-body rotation axis by a few degrees; this point in turn rotates around the solid-body rotation axis.

Published
2022

8. Characterization of the white ovals on Jupiter extquotesingles southern hemisphere using the first data by the Juno/JIRAM instrument

Author

G. Sindoni, D. Grassi, A. Adriani, A. Mura, M. L. Moriconi, B. M. Dinelli, G. Filacchione, F. Tosi, G. Piccioni, A. Migliorini, F. Altieri, F. Fabiano, D. Turrini, R. Noschese, A. Cicchetti, S. Stefani, S. J. Bolton, J. E. P. Connerney, S. K. Atreya, F. Bagenal, C. Hansen, A. Ingersoll, M. Janssen, S. M. Levin, J. I. Lunine, G. Orton, A. Olivieri, M. Amoroso, G. Sindoni, D. Grassi, A. Adriani, A. Mura, M. L. Moriconi, B. M. Dinelli, G. Filacchione, F. Tosi, G. Piccioni, A. Migliorini, F. Altieri, F. Fabiano, D. Turrini, R. Noschese, A. Cicchetti, S. Stefani, S. J. Bolton, J. E. P. Connerney, S. K. Atreya, F. Bagenal, C. Hansen, A. Ingersoll, M. Janssen, S. M. Levin, J. I. Lunine, G. Orton, A. Olivieri, and M. Amoroso

Subjects
Jupiter troposphere white ovals Juno Jiram
Abstract

Throughout the first orbit of the NASA Juno mission around Jupiter, the Jupiter InfraRed Auroral Mapper (JIRAM) targeted the northern and southern polar regions several times. The analyses of the acquired images and spectra confirmed a significant presence of methane (CH 4 ) near both poles through its 3.3 μm emission overlapping the H 3+ auroral feature at 3.31 μm. Neither acetylene (C 2 H 2 ) nor ethane (C 2 H 6 ) have been observed so far. The analysis method, developed for the retrieval of H 3+ temperature and abundances and applied to the JIRAM-measured spectra, has enabled an estimate of the effective temperature for methane peak emission and the distribution of its spectral contribution in the polar regions. The enhanced methane inside the auroral oval regions in the two hemispheres at different longitude suggests an excitation mechanism driven by energized particle precipitation from the magnetosphere.

Published
2017

11. Future Exploration of Enceladus and Other Saturnian Moons

Author

G. Mitri, A. Coustenis, J. I. Lunine, F. Tosi, G. Tobie, Lunar and Planetary Laboratory [Tucson] (LPL), University of Arizona, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Laboratoire de Planétologie et Géodynamique [UMR 6112] (LPG), Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), International Research School of Planetary Sciences [Pescara] (IRSPS), Università degli studi 'G. d'Annunzio' Chieti-Pescara [Chieti-Pescara] (Ud'A), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), and Istituto Nazionale di Astrofisica (INAF)

Subjects
020209 energy, 0103 physical sciences, 0202 electrical engineering, electronic engineering, information engineering, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Environmental science, 02 engineering and technology, Saturnian, Enceladus, 010303 astronomy & astrophysics, 01 natural sciences, ComputingMilieux_MISCELLANEOUS, Astrobiology
Abstract

International audience

Published
2018

12. MWR: Microwave Radiometer for the Juno Mission to Jupiter

Author

M. A. Janssen, J. E. Oswald, S. T. Brown, S. Gulkis, S. M. Levin, S. J. Bolton, M. D. Allison, S. K. Atreya, D. Gautier, A. P. Ingersoll, J. I. Lunine, G. S. Orton, T. C. Owen, P. G. Steffes, V. Adumitroaie, A. Bellotti, L. A. Jewell, C. Li, L. Li, S. Misra, F. A. Oyafuso, D. Santos-Costa, E. Sarkissian, R. Williamson, J. K. Arballo, A. Kitiyakara, A. Ulloa-Severino, J. C. Chen, F. W. Maiwald, A. S. Sahakian, P. J. Pingree, K. A. Lee, A. S. Mazer, R. Redick, R. E. Hodges, R. C. Hughes, G. Bedrosian, D. E. Dawson, W. A. Hatch, D. S. Russell, N. F. Chamberlain, M. S. Zawadski, B. Khayatian, B. R. Franklin, H. A. Conley, J. G. Kempenaar, M. S. Loo, E. T. Sunada, V. Vorperion, and C. C. Wang

Published
2017

13. Planetary System Imaging and Spectroscopy from Earth and Space

Author

J. R. P. Angel, N. J. Woolf, and J. I. Lunine

Subjects
Physics, Astronomy, Earth (chemistry), Astrophysics::Earth and Planetary Astrophysics, Planetary system, Space (mathematics), Spectroscopy, Astrobiology
Abstract

We describe the two main techniques by which planetary systems may be imaged, and by which spectra of the planets may be obtained. There is a discussion of how planetary systems will appear, and of the extreme differences in brightness between stars and their planets Coronography is an extension of Lyot's technique by addition of adaptive optics. Nulling is an interferometric technique originally proposed by Bracewell. Differences between the techniques are emphasized. The paper concludes with a discussion of the problem of training people to develop these technically difficult tasks.

Published
2004

14. Moist convective clouds in Titan's atmosphere

Author

J. I. Lunine and M. Awal

Subjects
Convection, Buoyancy, Atmospheric models, engineering.material, Atmospheric sciences, Physics::Fluid Dynamics, Troposphere, symbols.namesake, Geophysics, Flow velocity, Drag, symbols, engineering, General Earth and Planetary Sciences, Environmental science, Natural satellite, Astrophysics::Earth and Planetary Astrophysics, Titan (rocket family), Physics::Atmospheric and Oceanic Physics
Abstract

We examine moist convection as a plausible mechanism for driving large vertical motions and mixing in the troposphere of Titan. The model used here is based on that of Stoker [1986] for Jupiter — a one dimensional diagnostic model of cumulus clouds developed to calculate cloud temperature and vertical velocity profiles - incorporating an improved treatment of the drag effect of condensate on the buoyancy of the plumes. We find that under conditions plausible for the near surface of Titan, moist convection can occur with vertical velocity in excess of 1–13 m/s but that such plumes occupy only a very small fraction of the surface area of Titan. Nonetheless, we also find that such plumes may be the primary means of moving methane and other trace species from the surface into Titan's upper troposphere.

Published
1994

15. Carbon-rich giant planets: spectra, thermal inversions and formation conditions

Author

Madhusdhan O. Mousis J. I. Lunine T. V. Johnson, N., Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) (UTINAM), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), and Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC)

Subjects
ComputingMilieux_MISCELLANEOUS
Abstract

International audience

Published
2011

16. Impact regimes and post-formation sequestration processes: implications for the origin of heavy noble gases in terrestrial planets

Author

Mousis J. I. Lunine J.-M. Petit S. Picaud B. Schmitt D. Marquer J. Horner C. Thomas, O., Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) (UTINAM), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), Université de Franche-Comté (UFC), and Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)

Subjects
ComputingMilieux_MISCELLANEOUS
Abstract

International audience

Published
2010

17. Composition of the lakes of Titan

Author

Mousis D. Cordier J. I. Lunine P. Lavvas V. Vuitton, O., Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) (UTINAM), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), M. Heydari-Malayeri, C. Reylé, and R. Samadi

Subjects
ComputingMilieux_MISCELLANEOUS
Abstract

International audience

Published
2009

18. Isotopic evolution of the major constituents of Titan's atmosphere based on Cassini data

Author

E. Mandt J. H. Waite W. Lewis B. Magee J. Bell J. I. Lunine O. Mousis D. Cordier, K., Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) (UTINAM), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), and Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC)

Subjects
ComputingMilieux_MISCELLANEOUS
Abstract

International audience

Published
2009

19. Is Serpentinization the Source of Titan's Atmospheric Methane?

Author

Mousis J. I. Lunine M. Pasek D. Cordier J. H. Waite K. E. Mandt W. S. Lewis M.-J. Nguyen, O., Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) (UTINAM), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), and Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC)

Subjects
ComputingMilieux_MISCELLANEOUS
Abstract

International audience

Published
2009

20. Higher-order hydrocarbons, 40Ar, and deuterium in the plume of Saturn's icy moon Enceladus

Author

H. Waite T. Brockwell C.R. Glein W. S. Lewis J. I. Lunine B. Magee W. B. Mckinnon O. Mousis M. J. Nguyen B. Teolis J. Westlake D. T. Young Members Of The Inms Team, J., Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) (UTINAM), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), and Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC)

Subjects
ComputingMilieux_MISCELLANEOUS
Abstract

International audience

Published
2009

21. Formation conditions of Enceladus and origin of its methane reservoir

Author

Mousis J. I. Lunine J. H. Waite, O., Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) (UTINAM), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), M. Heydari-Malayeri, C. Reylé, and R. Samadi

Subjects
ComputingMilieux_MISCELLANEOUS
Abstract

International audience

Published
2009

22. A primordial origin for the atmospheric methane of Titan

Author

Mousis J. I. Lunine M. Pasek D. Cordier J. H. Waite K. E. Mandt, O., Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) (UTINAM), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), and Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC)

Subjects
ComputingMilieux_MISCELLANEOUS
Abstract

International audience

Published
2009

23. An estimate of the chemical composition of Titan's lakes

Author

Cordier O. Mousis J. I. Lunine P. Lavvas V. Vuitton, D., Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) (UTINAM), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), and Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC)

Subjects
ComputingMilieux_MISCELLANEOUS
Abstract

International audience

Published
2009

24. JIRAM, the Image Spectrometer in the Near Infrared on Board the Juno Mission to Jupiter

Author

Adriani, A. 1, A. Coradini 1, G. Filacchione 2, J. I. Lunine 3, A. Bini 4, C. Pasqui 4, L. Calamai 4, F. Colosimo 1, B. M. Dinelli 5, D. Grassi 1, G. Magni 2, M. L. Moriconi 5, and R. Orosei 2

Subjects
Physics, medicine.medical_specialty, Spectroscopy, Near-Infrared, Spectrometer, Extraterrestrial Environment, Atmosphere, Astronomy, Water, Space Flight, Agricultural and Biological Sciences (miscellaneous), Jovian, law.invention, Spectral imaging, Telescope, Jupiter, Exploration of Jupiter, Space and Planetary Science, law, medicine, Radiance, Spectral resolution, Remote sensing
Abstract

The Jovian InfraRed Auroral Mapper (JIRAM) has been accepted by NASA for inclusion in the New Frontiers mission “Juno,” which will launch in August 2011. JIRAM will explore the dynamics and the chemistry of Jupiter's auroral regions by high-contrast imaging and spectroscopy. It will also analyze jovian hot spots to determine their vertical structure and infer possible mechanisms for their formation. JIRAM will sound the jovian meteorological layer to map moist convection and determine water abundance and other constituents at depths that correspond to several bars pressure. JIRAM is equipped with a single telescope that accommodates both an infrared camera and a spectrometer to facilitate a large observational flexibility in obtaining simultaneous images in the L and M bands with the spectral radiance over the central zone of the images. Moreover, JIRAM will be able to perform spectral imaging of the planet in the 2.0–5.0 ¼m interval of wavelengths with a spectral resolution better than 10 nm. Instrument design, modes, and observation strategy will be optimized for operations onboard a spinning satellite in polar orbit around Jupiter. The JIRAM heritage comes from Italian-made, visual-infrared imaging spectrometers dedicated to planetary exploration, such as VIMS-V on Cassini, VIRTIS on Rosetta and Venus Express, and VIR-MS on the Dawn mission. Astrobiology 8, 613–622

Published
2008
Full Text
View/download PDF

25. New Debris Disks Around Nearby Main Sequence Stars: Impact on The Direct Detection of Planets

Author

C. A. Beichman, G. Bryden, K. R. Stapelfeldt, T. N. Gautier, K. Grogan, M. Shao, T. Velusamy, S. M. Lawler, M. Blaylock, G. H. Rieke, J. I. Lunine, D. A. Fischer, G. W. Marcy, J. S. Greaves, M. C. Wyatt, W. S. Holland, and W. R. F. Dent

Subjects
Physics, Photosphere, Zodiacal light, Metallicity, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Terrestrial Planet Finder, Stars, Space and Planetary Science, Planet, Asteroid belt, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Main sequence, Astrophysics::Galaxy Astrophysics
Abstract

Using the MIPS instrument on the Spitzer telescope, we have searched for infrared excesses around a sample of 82 stars, mostly F, G, and K main-sequence field stars, along with a small number of nearby M stars. These stars were selected for their suitability for future observations by a variety of planet-finding techniques. These observations provide information on the asteroidal and cometary material orbiting these stars - data that can be correlated with any planets that may eventually be found. We have found significant excess 70um emission toward 12 stars. Combined with an earlier study, we find an overall 70um excess detection rate of $13 \pm 3$% for mature cool stars. Unlike the trend for planets to be found preferentially toward stars with high metallicity, the incidence of debris disks is uncorrelated with metallicity. By newly identifying 4 of these stars as having weak 24um excesses (fluxes $\sim$10% above the stellar photosphere), we confirm a trend found in earlier studies wherein a weak 24um excess is associated with a strong 70um excess. Interestingly, we find no evidence for debris disks around 23 stars cooler than K1, a result that is bolstered by a lack of excess around any of the 38 K1-M6 stars in 2 companion surveys. One motivation for this study is the fact that strong zodiacal emission can make it hard or impossible to detect planets directly with future observatories like the {\it Terrestrial Planet Finder (TPF)}. The observations reported here exclude a few stars with very high levels of emission, $>$1,000 times the emission of our zodiacal cloud, from direct planet searches. For the remainder of the sample, we set relatively high limits on dust emission from asteroid belt counterparts.

Published
2006

26. Interiors of Rhea and Enceladus

Author

Rappaport, N. J., Iess, Luciano, Tortora, P., J. I, Lunine, Armstrong, J. W., Asmar, S. W., Somenzi, L., and Zingoni, F.

Published
2006

27. Radar: The Cassini Titan Radar Mapper

Author

C. Elachi, M. D. Allison, L. Borgarelli, P. Encrenaz, E. Im, M. A. Janssen, W. T. K. Johnson, R. L. Kirk, R. D. Lorenz, J. I. Lunine, D. O. Muhleman, S. J. Ostro, G. Picardi, F. Posa, C. G. Rapley, L. E. Roth, R. Seu, L. A. Soderblom, S. Vetrella, S. D. Wall, C. A. Wood, and H. A. Zebker

Published
2005

29. Modeling the Infrared Emission from the HR 4796A Disk

Author

J. I. Lunine and Aigen Li

Subjects
Physics, education.field_of_study, Infrared, Astrophysics (astro-ph), Carbon dust, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Silicate, Protoplanetary nebula, chemistry.chemical_compound, chemistry, Space and Planetary Science, Volume fraction, Spectral energy distribution, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, education, Astrophysics::Galaxy Astrophysics
Abstract

We model the spectral energy distribution (SED) from the mid-infrared to submillimeter of the ring-like disk of HR 4796A, the dustiest A-type star. We consider dust made either of coagulated but otherwise unaltered protostellar interstellar grains, or grains that are highly-processed in a protostellar/protoplanetary nebula with silicate dust annealed and carbon dust oxidized. Both types of dust are successful in reproducing the observed SED, provided that the grains are highly fluffy, with a vacuum volume fraction of \~90%. We find no evidence for the existence of a hot ``zodiacal dust'' component a few AU from the star, which was suggested by previous workers to account for the 10 micron-wavelength emission., published in The Astrophysical Journal, vol. 590, pp. 368--378; 26 pages; 9 figures

Published
2003

30. Geologic settings for aqueous organic synthesis on Titan revisited

Author

R D, Lorenz, J I, Lunine, and C P, McKay

Subjects
Carbon Monoxide, Extraterrestrial Environment, Photochemistry, Ultraviolet Rays, Jupiter, Exobiology, Water
Abstract

The photochemistry in Titan's cold reducing atmosphere is an evolutionary dead end. However, the hydrocarbons and nitriles deposited from the atmosphere can undergo aqueous synthesis into prebiotic molecules in ephemeral settings such as impact melt sheets. We re-examine the longevity of aqueous solutions on Titan, noting that recent measurements of the thermal conductivity of ammonia-rich ices suggest that the melt pockets may be longer-lived than previously thought. We propose an important role in surface organic reactions for ultraviolet sunlight transported to the surface as chemical energy stored in acetylene and released by polymerization at Titan's surface.

Published
2001

31. Challenges and approaches to the robotic detection of enantioenrichment on Saturn's moon, Titan

Author

C J, Welch and J I, Lunine

Abstract

Saturn's moon, Titan, is one of the most interesting locations for organic chemistry in the solar system. As a possible follow up to the Cassini-Huygens mission, which will conduct the first in situ analysis of the Titan atmosphere in 2004, studies are underway for missions to explore in detail the chemical composition of Titan's atmosphere, surface, and oceans. In order to seek out and explore complex chemical systems that may represent steps on the pathway to life, instruments for detection of enantioenrichment should be included on such a mission. The formidable challenges of robotic measurement of enantioenrichment on Titan are summarized, and experimental approaches to this problem are reviewed. In addition, some speculations are offered concerning locations on Titan where complex fractionation of organic materials may have occurred.

Published
2001

32. Titan and the origin of life on Earth

Author

T, Owen, F, Raulin, C P, McKay, J I, Lunine, and J P, Lebreton

Subjects
Evolution, Chemical, Saturn, Atmosphere, Earth, Planet, Nitrogen, Ice, Origin of Life, Water, Spacecraft, Methane
Abstract

The relevance of Titan to the study of pre-biotic chemistry and the origin of life on Earth will be addressed by an interdisciplinary group of Cassini/Huygens scientists using the different, but synergistic data sets obtained by NASA's Cassini Orbiter and ESA's Huygens Probe. Titan's special importance lies in the primitive chemically-reducing nature of its atmosphere Cassini/ Huygens instruments will determine what compounds form in this environment, and the results will be compared with models for pre-biological chemical evolution on Earth.

Published
2001

33. Physics and chemistry of the solar nebula

Author

J I, Lunine

Subjects
Cold Temperature, Physical Phenomena, Chemistry, Cosmic Dust, Chemical Phenomena, Astronomy, Physics, Gases, Solar System, Models, Theoretical
Abstract

The solar system is thought to have begun in a flattened disk of gas and dust referred to traditionally as the solar nebula. Such a construct seems to be a natural product of the collapse of dense parts of giant molecular clouds, the vast star-forming regions that pepper the Milky Way and other galaxies. Gravitational, magnetic and thermal forces within the solar nebula forced a gradual evolution of mass toward the center (where the sun formed) and angular momentum (borne by a small fraction of the mass) toward the outer more distant regions of the disk. This evolution was accompanied by heating and a strong temperature contrast from the hot, inner regions to the cold, more remote parts of the disk. The resulting chemistry in the disk determined the initial distribution of organic matter in the planets; most of the reduced carbon species, in condensed form, were located beyond the asteroid belt (the 'outer' solar system). The Earth could have received much of its inventory of pre-biological material from comets and other icy fragments of the process of planetary formation in the outer solar system.

Published
1997

34. A Statistical Approach to Planetesimal Condensate Composition beyond the Snowline Based on the Carbon-to-oxygen Ratio.

Author

G. S. Pekmezci, T. V. Johnson, J. I. Lunine, and O. Mousis

Subjects
SPACE sciences, SOLAR system, CHEMISTRY, PLANETESIMALS, ICE
Abstract

The ratio between carbon and oxygen is regarded as an important driver of circumstellar and planetary chemistry, which can be used as a parameter to estimate the fractionation among refractory and volatile portions of a planet. From this motivation, nearly 500 stars including some with planets discovered around them are investigated. The relation between the C/O ratio and fractions of icy and refractory species is traced for planetesimals expected to form in their protostellar disks. It is found that low C/O ratios lead to planets rich in ice, but poor in organic and other refractory materials. With increasing C/O ratios, the ice fraction diminishes, where organics increase and other refractory materials dominate. Apart from that, the carbon portion incorporated in the solid phase and the redox state of the environment are altered to analyze their influence on bulk formation for generated planets. Under zero solid carbon contribution, ice formation decreases and refractory formation increases with increasing C/O ratio. When the carbon contribution is considered to be entirely in the solid phase, refractory materials are not significantly affected by the increasing C/O ratio while ice may even disappear. For reducing conditions, the C/O ratio is not an obstacle for ice formation no matter how high it is. Under oxidizing conditions, however, water is not found where the C/O ratio is greater than 0.8. Bulk densities are also calculated according to alternative scenarios along with compositional distributions, and results are compared to solar system objects. This study, therefore, exemplifies how a simple correlation can be drawn between stellar chemistry, redox state, and planetesimal composition. [ABSTRACT FROM AUTHOR]

Published
2019
Full Text
View/download PDF

40. Synthesis of Molecular Oxygen via Irradiation of Ice Grains in the Protosolar Nebula.

Author

O. Mousis, T. Ronnet, J. I. Lunine, R. Maggiolo, P. Wurz, G. Danger, and A. Bouquet

Subjects
NEBULAE, COMETS, COSMIC abundances, SPACE vehicles, CENTROID
Abstract

Molecular oxygen has been detected in the coma of comet 67P/Churyumov–Gerasimenko with a mean abundance of 3.80 ± 0.85% by the ROSINA mass spectrometer on board the Rosetta spacecraft. To account for the presence of this species in comet 67P/Churyumov–Gerasimenko, it has been shown that the radiolysis of ice grain precursors of comets is a viable mechanism in low-density environments, such as molecular clouds. Here, we investigate the alternative possibility that the icy grains present in the midplane of the protosolar nebula were irradiated during their vertical transport between the midplane and the upper layers over a large number of cycles, as a result of turbulent mixing. Consequently, these grains spent a non-negligible fraction of their lifetime in the disk’s upper regions, where the irradiation by cosmic rays was strong. To do so, we used a coupled disk-transport-irradiation model to calculate the time evolution of the molecular oxygen abundance radiolytically produced in ice grains. Our computations show that, even if a significant fraction of the icy particles has followed a back and forth cycle toward the upper layers of the disk over tens of millions of years, a timespan far exceeding the formation timescale of comet 67P/Churyumov–Gerasimenko, the amount of produced molecular oxygen is at least two orders of magnitude lower than the Rosetta observations. We conclude that the most likely scenario remains the formation of molecular oxygen in low-density environments, such as the presolar cloud, prior to the genesis of the protosolar nebula. [ABSTRACT FROM AUTHOR]

Published
2018
Full Text
View/download PDF

41. Acetylene on Titan

Author

J I, Lunine, D J, Stevenson, and Y L, Yung

Subjects
Multidisciplinary
Published
1984

42. Correction to 'The vertical distribution of ozone in the mesosphere and lower thermosphere' by M. Allen, J. I. Lunine, and Y. L. Yung

Author

J. I. Lunine, Yuk L. Yung, and M. Allen

Subjects
Atmospheric Science, Ozone, Ecology, Distribution (number theory), Meteorology, Paleontology, Soil Science, Forestry, Aquatic Science, Oceanography, Atmospheric sciences, chemistry.chemical_compound, Geophysics, chemistry, Space and Planetary Science, Geochemistry and Petrology, Mesopause, Earth and Planetary Sciences (miscellaneous), Environmental science, Thermosphere, Earth-Surface Processes, Water Science and Technology
Published
1984

44. Stability of Sulphur Dimers (S2) in Cometary Ices.

Author

O. Mousis, T. Ronnet, O. Ozgurel, F. Pauzat, A. Markovits, Y. Ellinger, J. I. Lunine, and A. Luspay-Kuti

Subjects
SPACE biology, COMETS, SULFUR, INTERSTELLAR medium, HYDROGEN sulfide
Abstract

S2 has been observed for decades in comets, including comet 67P/Churyumov–Gerasimenko. Despite the fact that this molecule appears ubiquitous in these bodies, the nature of its source remains unknown. In this study, we assume that S2 is formed by irradiation (photolysis and/or radiolysis) of S-bearing molecules embedded in the icy grain precursors of comets and that the cosmic ray flux simultaneously creates voids in ices within which the produced molecules can accumulate. We investigate the stability of S2 molecules in such cavities, assuming that the surrounding ice is made of H2S or H2O. We show that the stabilization energy of S2 molecules in such voids is close to that of the H2O ice binding energy, implying that they can only leave the icy matrix when this latter sublimates. Because S2 has a short lifetime in the vapor phase, we derive that its formation in grains via irradiation must occur only in low-density environments such as the ISM or the upper layers of the protosolar nebula, where the local temperature is extremely low. In the first case, comets would have agglomerated from icy grains that remained pristine when entering the nebula. In the second case, comets would have agglomerated from icy grains condensed in the protosolar nebula and that would have been efficiently irradiated during their turbulent transport toward the upper layers of the disk. Both scenarios are found consistent with the presence of molecular oxygen in comets. [ABSTRACT FROM AUTHOR]

Published
2017
Full Text
View/download PDF

48. Radar: The Cassini Titan Radar Mapper

Author

Steven J. Ostro, Randolph L. Kirk, Laurence A. Soderblom, L. Borgarelli, Giovanni Picardi, M. A. Janssen, Duane O. Muhleman, Pierre Encrenaz, Francesco Posa, L.E. Roth, Charles A. Wood, Chris Rapley, Michael Allison, Ralph D. Lorenz, Jonathan I. Lunine, William T. K. Johnson, Charles Elachi, Howard A. Zebker, Eastwood Im, Roberto Seu, S. Vetrella, S. D. Wall, C., Elachi, M. D., Allison, L., Borgarelli, E., Encrenaz, E., Im, M. A., Janssen, W. T. K., Johnson, R. L., Kirk, R. D., Lorenz, J. I., Lunine, D. O., Muhleman, S. J., Ostro, G., Picardi, F., Posa, C. G., Rapley, L. E., Roth, R., Seu, L. A., Soderblom, Vetrella, Sergio, S. D., Wall, C. A., Wood, H. A., Zebker, Jet Propulsion Laboratory, California Institute of Technology (JPL), Goddard Institute for Space Studies, National Aeronautics and Space Administration New York, Alenia Aerospazio, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Instrumentation et télédétection, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique et Atmosphères = Laboratory for Studies of Radiation and Matter in Astrophysics and Atmospheres (LERMA), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), US Geological Survey, Flagstaff, Lunar and Planetary Laboratory [University of Arizona] (LPL), University of Arizona, Geological and Planetary Sciences, California Institute of Technology, Pasadena, Universitá La Sapienza, Dipartimento Interateneo di Fisica, Politecnico di Bari, British Antarctic Survey, Natural Environment Research Council, Facoltá di Ingegneria, University of North Dakota, and Stanford University

Subjects
Radar altimeter, Titan moon, Astronomy and Astrophysics, Scatterometer, Space-based radar, law.invention, Radar engineering details, Radar astronomy, Space and Planetary Science, law, Radar imaging, 3D radar, Cassini, Radar, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Remote sensing
Abstract

International audience; The Cassini RADAR instrument is a multimode 13.8 GHz multiple-beam sensor that can operate as a synthetic-aperture radar (SAR) imager, altimeter, scatterometer, and radiometer. The principal objective of the RADAR is to map the surface of Titan. This will be done in the imaging, scatterometer, and radiometer modes. The RADAR altimeter data will provide information on relative elevations in selected areas. Surfaces of the Saturn's icy satellites will be explored utilizing the RADAR radiometer and scatterometer modes. Saturn's atmosphere and rings will be probed in the radiometer mode only. The instrument is a joint development by JPL/NASA and ASI. The RADAR design features significant autonomy and data compression capabilities. It is expected that the instrument will detect surfaces with backscatter coefficient as low as -40 dB.

Published
2004

49. The Gravity Field and Interior Structure of Enceladus

Author

Douglas J. Hemingway, Francis Nimmo, M. Ducci, Luciano Iess, Robert A. Jacobson, Sami W. Asmar, Jonathan I. Lunine, Paolo Tortora, Marzia Parisi, John W. Armstrong, David J. Stevenson, L. Ie, D. J. Stevenson, M. Parisi, D. Hemingway, R.A. Jacobson, J. I. Lunine, F. Nimmo, J. W. Armstrong, S. W. Asmar, M. Ducci, and P. Tortora

Subjects
SATURN, Multidisciplinary, Extraterrestrial Environment, planetary interiors, ICE, Water, Mineralogy, GRAVITATION, Astrophysics, Radius, Moment of inertia, enceladus, planetary geodesy, law.invention, Gravitational field, Negative mass, law, Saturn, Quadrupole, Spacecraft, Hydrostatic equilibrium, Enceladus
Abstract

Inside Enceladus Saturn's moon Enceladus has often been the focus of flybys of the Cassini spacecraft. Although small—Enceladus is roughly 10 times smaller than Saturn's largest moon, Titan—Enceladus has shown hints of having a complex internal structure rich in liquid water. Iess et al. (p. 78 ) used long-range data collected by the Cassini spacecraft to construct a gravity model of Enceladus. The resulting gravity field indicates the presence of a large mass anomaly at its south pole. Calculations of the moment of inertia and hydrostatic equilibrium from the gravity data suggest the presence of a large, regional subsurface ocean 30 to 40 km deep.

Published
2014

50. Can Cassini detect a subsurface ocean in Titan from gravity measurements?

Author

Paolo Tortora, Jonathan I. Lunine, Sami W. Asmar, Mauro Di Benedetto, Luciano Iess, P. Racioppa, John W. Armstrong, John Wahr, Nicole J. Rappaport, N. J. Rappaport, L. Ie, J. Wahr, J. I. Lunine, J. W. Armstrong, S. W. Asmar, P. Tortora, and M. Di Benedetto and P. Racioppa

Subjects
Gravity (chemistry), Lead (sea ice), Astronomy and Astrophysics, Geophysics, Viscoelasticity, DOPPLER TRACKING OF SPACECRAFT, symbols.namesake, Space and Planetary Science, TITAN GRAVITY FIELD, symbols, RADIO SCIENCE EXPERIMENTS, Satellite, Love number, Titan (rocket family), Geology, Remote sensing, Radio Science, SATELLITE INTERNAL OCEANS
Abstract

Recent models of Titan's interior predict that the satellite contains an ocean of water and ammonia under an icy layer. Direct evidence for the presence of an ocean can be provided on the Cassini mission only by radio science determination of Titan Love number k 2 . Simulations that use the five flybys T11, T22 T33, T45, and T68 (the latter two belonging to the extended mission) lead to the result that in the elastic case, where the Love number is real, k 2 will be determined with a one-sigma accuracy of 0.1. In the viscoelastic case, where k 2 is complex, the real and imaginary parts of k 2 will be determined with one sigma accuracies of 0.138 and 0.115, respectively. Ocean and oceanless models that include a viscoelastic rheology are built. In the viscoelastic case, there is a 93% probability to correctly predict the presence or absence of an ocean; this probability improves to 97% in the elastic case.

Published
2008

Catalog

Books, media, physical & digital resources
See catalog results