Exploring the Surface Liquid and Lake Regions of Titan with Laboratory
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The Spectral Nature of Titan's Major Geomorphological Units
PUBLICATIONS Journal of Geophysical Research: Planets RESEARCH ARTICLE The Spectral Nature of Titan’s Major Geomorphological 10.1002/2017JE005477 Units: Constraints on Surface Composition Key Points: A. Solomonidou1,2,3 , A. Coustenis3, R. M. C. Lopes4 , M. J. Malaska4 , S. Rodriguez5, • ’ The spectral nature of some of Titan s 3 1 6 6 4 7 4 4 major geomorphological units at P. Drossart , C. Elachi , B. Schmitt , S. Philippe , M. Janssen , M. Hirtzig , S. Wall , C. Sotin , 4 2 8 9 10 11 12 midlatitudes is described using a K. Lawrence , N. Altobelli , E. Bratsolis , J. Radebaugh , K. Stephan , R. H. Brown , S. Le Mouélic , radiative transfer code A. Le Gall13, E. V. Villanueva4, J. F. Brossier10 , A. A. Bloom4 , O. Witasse14 , C. Matsoukas15, and • Three main categories of albedo 16 govern Titan’s low-midlatitude surface A. Schoenfeld regions, and its surface composition 1 2 has a latitudinal dependence California Institute of Technology, Pasadena, CA, USA, European Space Astronomy Centre, European Space Agency, Madrid, 3 • The surface albedo differences and Spain, LESIA-Observatoire de Paris, Paris Sciences and Letters Research University, CNRS, Sorbonne Université, Université similarities among the RoIs set Paris-Diderot, Meudon, France, 4Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA, 5Institut de constraints on possible formation Physique du Globe de Paris, CNRS-UMR 7154, Université Paris-Diderot, USPC, Paris, France, 6Institut de Planétologie et and/or evolution processes d’Astrophysique de Grenoble, Université Grenoble Alpes, CNRS, Grenoble, France, 7Fondation “La main à la pâte”, Montrouge, France, 8Department of Physics, University of Athens, Athens, Greece, 9Department of Geological Sciences, Brigham Young University, Provo, UT, USA, 10Institute of Planetary Research, DLR, Berlin, Germany, 11Lunar and Planetary Laboratory, University Correspondence to: of Arizona, Tucson, AZ, USA, 12Laboratoire de Planétologie et Géodynamique, CNRS UMR 6112, Université de Nantes, Nantes, A. -
The Lakes and Seas of Titan • Explore Related Articles • Search Keywords Alexander G
EA44CH04-Hayes ARI 17 May 2016 14:59 ANNUAL REVIEWS Further Click here to view this article's online features: • Download figures as PPT slides • Navigate linked references • Download citations The Lakes and Seas of Titan • Explore related articles • Search keywords Alexander G. Hayes Department of Astronomy and Cornell Center for Astrophysics and Planetary Science, Cornell University, Ithaca, New York 14853; email: [email protected] Annu. Rev. Earth Planet. Sci. 2016. 44:57–83 Keywords First published online as a Review in Advance on Cassini, Saturn, icy satellites, hydrology, hydrocarbons, climate April 27, 2016 The Annual Review of Earth and Planetary Sciences is Abstract online at earth.annualreviews.org Analogous to Earth’s water cycle, Titan’s methane-based hydrologic cycle This article’s doi: supports standing bodies of liquid and drives processes that result in common 10.1146/annurev-earth-060115-012247 Annu. Rev. Earth Planet. Sci. 2016.44:57-83. Downloaded from annualreviews.org morphologic features including dunes, channels, lakes, and seas. Like lakes Access provided by University of Chicago Libraries on 03/07/17. For personal use only. Copyright c 2016 by Annual Reviews. on Earth and early Mars, Titan’s lakes and seas preserve a record of its All rights reserved climate and surface evolution. Unlike on Earth, the volume of liquid exposed on Titan’s surface is only a small fraction of the atmospheric reservoir. The volume and bulk composition of the seas can constrain the age and nature of atmospheric methane, as well as its interaction with surface reservoirs. Similarly, the morphology of lacustrine basins chronicles the history of the polar landscape over multiple temporal and spatial scales. -
Titan's Cold Case Files
Titan’s cold case files - Outstanding questions after Cassini-Huygens C.A. Nixon, R.D. Lorenz, R.K. Achterberg, A. Buch, P. Coll, R.N. Clark, R. Courtin, A. Hayes, L. Iess, R.E. Johnson, et al. To cite this version: C.A. Nixon, R.D. Lorenz, R.K. Achterberg, A. Buch, P. Coll, et al.. Titan’s cold case files - Out- standing questions after Cassini-Huygens. Planetary and Space Science, Elsevier, 2018, 155, pp.50-72. 10.1016/j.pss.2018.02.009. insu-03318440 HAL Id: insu-03318440 https://hal-insu.archives-ouvertes.fr/insu-03318440 Submitted on 10 Aug 2021 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. Distributed under a Creative Commons Attribution| 4.0 International License Planetary and Space Science 155 (2018) 50–72 Contents lists available at ScienceDirect Planetary and Space Science journal homepage: www.elsevier.com/locate/pss Titan's cold case files - Outstanding questions after Cassini-Huygens C.A. Nixon a,*, R.D. Lorenz b, R.K. Achterberg c, A. Buch d, P. Coll e, R.N. Clark f, R. Courtin g, A. Hayes h, L. Iess i, R.E. -
Wave Constraints for Titan’S Jingpo Lacus and Kraken Mare
Icarus 211 (2011) 722–731 Contents lists available at ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus Wave constraints for Titan’s Jingpo Lacus and Kraken Mare from VIMS specular reflection lightcurves ⇑ Jason W. Barnes a, , Jason M. Soderblom b, Robert H. Brown b, Laurence A. Soderblom c, Katrin Stephan d, Ralf Jaumann d, Stéphane Le Mouélic e, Sebastien Rodriguez f, Christophe Sotin g, Bonnie J. Buratti g, Kevin H. Baines g, Roger N. Clark h, Philip D. Nicholson i a Department of Physics, University of Idaho, Moscow, ID 83844-0903, United States b Department of Planetary Sciences, University of Arizona, Tucson, AZ 85721, United States c United States Geological Survey, Flagstaff, AZ 86001, United States d DLR, Institute of Planetary Research, Rutherfordstrasse 2, D-12489 Berlin, Germany e Laboratoire de Planétologie et Géodynamique, CNRS UMR6112, Université de Nantes, France f Laboratoire AIM, Centre d’ètude de Saclay, DAPNIA/Sap, Centre de l’Orme des M erisiers, bât. 709, 91191 Gif/Yvette Cedex, France g Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, United States h United States Geological Survey, Denver, CO 80225, United States i Department of Astronomy, Cornell University, Ithaca, NY 14853, United States article info abstract Article history: Stephan et al. (Stephan, K. et al. [2010]. Geophys. Res. Lett. 37, 7104–+.) first saw the glint of sunlight Received 15 April 2010 specularly reflected off of Titan’s lakes. We develop a quantitative model for analyzing the photometric Revised 18 September 2010 lightcurve generated during a flyby in which the specularly reflected light flux depends on the fraction of Accepted 28 September 2010 the solar specular footprint that is covered by liquid. -
Composition, Seasonal Change and Bathymetry of Ligeia Mare, Titan, Derived from Its Microwave Thermal Emission Alice Le Gall, M.J
Composition, seasonal change and bathymetry of Ligeia Mare, Titan, derived from its microwave thermal emission Alice Le Gall, M.J. Malaska, R.D. Lorenz, M.A. Janssen, T. Tokano, A.G. Hayes, M. Mastrogiuseppe, J.I. Lunine, G. Veyssière, P. Encrenaz, et al. To cite this version: Alice Le Gall, M.J. Malaska, R.D. Lorenz, M.A. Janssen, T. Tokano, et al.. Composition, seasonal change and bathymetry of Ligeia Mare, Titan, derived from its microwave thermal emission. Journal of Geophysical Research. Planets, Wiley-Blackwell, 2016, 121 (2), pp.233-251. 10.1002/2015JE004920. hal-01259869 HAL Id: hal-01259869 https://hal.archives-ouvertes.fr/hal-01259869 Submitted on 8 Mar 2016 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. PUBLICATIONS Journal of Geophysical Research: Planets RESEARCH ARTICLE Composition, seasonal change, and bathymetry 10.1002/2015JE004920 of Ligeia Mare, Titan, derived from its Key Points: microwave thermal emission • Radiometry observations of Ligeia Mare support a liquid composition A. Le Gall1, M. J. Malaska2, R. D. Lorenz3, M. A. Janssen2, T. Tokano4, A. G. Hayes5, M. Mastrogiuseppe5, dominated by methane 5 6 7 8 • The seafloor of Ligeia Mare probably J. -
Production and Global Transport of Titan's Sand Particles
Barnes et al. Planetary Science (2015) 4:1 DOI 10.1186/s13535-015-0004-y ORIGINAL RESEARCH Open Access Production and global transport of Titan’s sand particles Jason W Barnes1*,RalphDLorenz2, Jani Radebaugh3, Alexander G Hayes4,KarlArnold3 and Clayton Chandler3 *Correspondence: [email protected] Abstract 1Department of Physics, University Previous authors have suggested that Titan’s individual sand particles form by either of Idaho, Moscow, Idaho, 83844-0903 USA sintering or by lithification and erosion. We suggest two new mechanisms for the Full list of author information is production of Titan’s organic sand particles that would occur within bodies of liquid: available at the end of the article flocculation and evaporitic precipitation. Such production mechanisms would suggest discrete sand sources in dry lakebeds. We search for such sources, but find no convincing candidates with the present Cassini Visual and Infrared Mapping Spectrometer coverage. As a result we propose that Titan’s equatorial dunes may represent a single, global sand sea with west-to-east transport providing sources and sinks for sand in each interconnected basin. The sand might then be transported around Xanadu by fast-moving Barchan dune chains and/or fluvial transport in transient riverbeds. A river at the Xanadu/Shangri-La border could explain the sharp edge of the sand sea there, much like the Kuiseb River stops the Namib Sand Sea in southwest Africa on Earth. Future missions could use the composition of Titan’s sands to constrain the global hydrocarbon cycle. We chose to follow an unconventional format with respect to our choice of section head- ings compared to more conventional practice because the multifaceted nature of our work did not naturally lend itself to a logical progression within the precribed system. -
THE SURFACE AGE of TITAN. Introduction
View metadata, citation and similar papers at core.ac.uk brought to you by CORE provided by Institute of Transport Research:Publications 40th Lunar and Planetary Science Conference (2009) 1641.pdf THE SURFACE AGE OF TITAN. Ralf Jaumann1,2,* and Gerhard Neukum2. 1DLR, Institute of Planetary Research. Rutherfordstrasse 2, 12489 Berlin, Germany; 2Dept. of Earth Sciences, Inst. of Geosciences, Freie Universität Berlin, Germany; Email address: [email protected] Introduction: Since its arrival at the Saturnian system, Titan’s surface with a slight increase on the trailing site the Cassini spacecraft has made about 100 Titan fly- (Fig.1). This observation appears to coincide with the bys. The surface of Titan has been revealed almost impactor model of Korycansky and Zahnle (2005) [10] globally by the Cassini observations in the infrared and who suggest that the leading hemisphere should have a regionally to about 25% in radar wavelengths [1,2,3] crater frequency about 5 times higher than the trailing as well as locally by the Huygens optical instruments side assuming Titan has been in synchronous rotation [4]. Extended dune fields, lakes, distinct landscapes of throughout its history. However, this observation may volcanic and tectonic origin, dendritic erosion patterns change in the course of the mission with increasing and deposited erosional remnants exhibit a high-resolution coverage which is so far poorer on the geologically active surface indicating significant leading site. The cumulative crater frequency is shown endogenic and exogenic processes leading to dynamic in Fig. 2 for both the confirmed five craters and the surface alteration. Consequently, impact craters are total of the putative craters. -
Regional Geomorphology and History of Titan's Xanadu Province
Icarus 211 (2011) 672–685 Contents lists available at ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus Regional geomorphology and history of Titan’s Xanadu province J. Radebaugh a,, R.D. Lorenz b, S.D. Wall c, R.L. Kirk d, C.A. Wood e, J.I. Lunine f, E.R. Stofan g, R.M.C. Lopes c, P. Valora a, T.G. Farr c, A. Hayes h, B. Stiles c, G. Mitri c, H. Zebker i, M. Janssen c, L. Wye i, A. LeGall c, K.L. Mitchell c, F. Paganelli g, R.D. West c, E.L. Schaller j, The Cassini Radar Team a Department of Geological Sciences, Brigham Young University, S-389 ESC Provo, UT 84602, United States b Johns Hopkins Applied Physics Laboratory, Laurel, MD 20723, United States c Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, United States d US Geological Survey, Branch of Astrogeology, Flagstaff, AZ 86001, United States e Wheeling Jesuit University, Wheeling, WV 26003, United States f Department of Physics, University of Rome ‘‘Tor Vergata”, Rome 00133, Italy g Proxemy Research, P.O. Box 338, Rectortown, VA 20140, USA h Department of Geological Sciences, California Institute of Technology, Pasadena, CA 91125, USA i Department of Electrical Engineering, Stanford University, 350 Serra Mall, Stanford, CA 94305, USA j Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721, USA article info abstract Article history: Titan’s enigmatic Xanadu province has been seen in some detail with instruments from the Cassini space- Received 20 March 2009 craft. -
Titan's Meteorology Over the Cassini Mission: Evidence for Extensive
Titan’s Meteorology Over the Cassini Mission: Evidence for Extensive Subsurface Methane Reservoirs E. Turtle, J. Perry, J. Barbara, A. del Genio, S. Rodriguez, Stéphane Le Mouélic, C. Sotin, J. M. Lora, S. Faulk, P. Corlies, et al. To cite this version: E. Turtle, J. Perry, J. Barbara, A. del Genio, S. Rodriguez, et al.. Titan’s Meteorology Over the Cassini Mission: Evidence for Extensive Subsurface Methane Reservoirs. Geophysical Research Letters, Amer- ican Geophysical Union, 2018, 45 (11), pp.5320-5328. 10.1029/2018GL078170. hal-02373164 HAL Id: hal-02373164 https://hal.archives-ouvertes.fr/hal-02373164 Submitted on 8 Jul 2021 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. Copyright Geophysical Research Letters RESEARCH LETTER Titan’s Meteorology Over the Cassini Mission: 10.1029/2018GL078170 Evidence for Extensive Subsurface Special Section: Methane Reservoirs Cassini's Final Year: Science Highlights and Discoveries E. P. Turtle1 , J. E. Perry2 , J. M. Barbara3 , A. D. Del Genio4 , S. Rodriguez5 , S. Le Mouélic6, C. Sotin7 , J. M. Lora8 , S. Faulk8 , P. Corlies9 , J. Kelland10 , S. M. MacKenzie1 , 7 2 9 7 7 7 Key Points: R. A. West , A. -
Solubility, Sea Properties, Effervescence and Ballast Design
SOLUBILITY, SEA PROPERTIES, EFFERVESCENCE AND BALLAST DESIGN FOR AN EXTRATERRESTRIAL SUBMARINE by PETER MEYERHOFER Submitted in partial fulfillment of the requirements for the degree of Master of Science Mechanical Engineering CASE WESTERN RESERVE UNIVERSITY January 2019 CASE WESTERN RESERVE UNIVERSITY SCHOOL OF GRADUATE STUDIES We hereby approve the thesis of Peter Meyerhofer candidate for the degree of Master of Science. Committee Chair Prof. Yasuhiro Kamotani Committee Member Prof. Paul Barnhart Committee Member Prof. Joseph Prahl Date of Defense October 24th, 2017 *We also certify that written approval has been obtained for any proprietary material contained therein. 1 Table of Contents 1 Introduction ........................................................................................................ 14 2 Literature Review ............................................................................................... 18 3 Solubility Model ................................................................................................. 21 3.1 Background ................................................................................................. 21 3.2 Analysis and Filtering ................................................................................. 26 3.3 Analytical Model ........................................................................................ 30 3.3.1 Functional Form .................................................................................. 30 3.3.2 Curve Fit to Data ................................................................................ -
Formation Et Développement Des Lacs De Titan : Interprétation Géomorphologique D’Ontario Lacus Et Analogues Terrestres Thomas Cornet
Formation et Développement des Lacs de Titan : Interprétation Géomorphologique d’Ontario Lacus et Analogues Terrestres Thomas Cornet To cite this version: Thomas Cornet. Formation et Développement des Lacs de Titan : Interprétation Géomorphologique d’Ontario Lacus et Analogues Terrestres. Planétologie. Ecole Centrale de Nantes (ECN), 2012. Français. NNT : 498 - 254. tel-00807255v2 HAL Id: tel-00807255 https://tel.archives-ouvertes.fr/tel-00807255v2 Submitted on 28 Nov 2013 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. Ecole Centrale de Nantes ÉCOLE DOCTORALE SCIENCES POUR L’INGENIEUR, GEOSCIENCES, ARCHITECTURE Année 2012 N° B.U. : Thèse de DOCTORAT Spécialité : ASTRONOMIE - ASTROPHYSIQUE Présentée et soutenue publiquement par : THOMAS CORNET le mardi 11 Décembre 2012 à l’Université de Nantes, UFR Sciences et Techniques TITRE FORMATION ET DEVELOPPEMENT DES LACS DE TITAN : INTERPRETATION GEOMORPHOLOGIQUE D’ONTARIO LACUS ET ANALOGUES TERRESTRES JURY Président : M. MANGOLD Nicolas Directeur de Recherche CNRS au LPGNantes Rapporteurs : M. COSTARD François Directeur de Recherche CNRS à l’IDES M. DELACOURT Christophe Professeur des Universités à l’Université de Bretagne Occidentale Examinateurs : M. BOURGEOIS Olivier Maître de Conférences HDR à l’Université de Nantes M. GUILLOCHEAU François Professeur des Universités à l’Université de Rennes I M. -
Implications for Titan's Surface Properties
Icarus 208 (2010) 366–384 Contents lists available at ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus Correlations between VIMS and RADAR data over the surface of Titan: Implications for Titan’s surface properties F. Tosi a,*, R. Orosei a, R. Seu b, A. Coradini a, J.I. Lunine a,c, G. Filacchione d, A.I. Gavrishin e, F. Capaccioni d, P. Cerroni d, A. Adriani a, M.L. Moriconi f, A. Negrão g, E. Flamini h, R.H. Brown i, L.C. Wye j, M. Janssen k, R.D. West k, J.W. Barnes l, S.D. Wall k, R.N. Clark m, D.P. Cruikshank n, T.B. McCord o, P.D. Nicholson p, J.M. Soderblom i, The Cassini VIMS and RADAR Teams a INAF-IFSI Istituto di Fisica dello Spazio Interplanetario, Via del Fosso del Cavaliere, 100, I-00133 Roma, Italy b Università degli Studi di Roma ‘‘La Sapienza”, Facoltà di Ingegneria, Dipartimento INFOCOM, Via Eudossiana 18, I-00184 Roma, Italy c Università degli Studi di Roma ‘‘Tor Vergata”, Dipartimento di Fisica, Via della Ricerca Scientifica 1, I-00133 Roma, Italy d INAF-IASF Istituto di Astrofisica Spaziale e Fisica Cosmica, Via del Fosso del Cavaliere 100, I-00133 Roma, Italy e South-Russian State Technical University, Prosveschenia 132, Novocherkassk 346428, Russia f CNR-ISAC Istituto di Scienze dell’Atmosfera e del Clima, Via del Fosso del Cavaliere 100, I-00133 Roma, Italy g Escola Superior de Tecnologia e Gestão do Instituto Politécnico de Leiria (ESTG-IPL), Campus 2 Morro do Lena – Alto do Vieiro, 2411-901 Leiria, Portugal h Agenzia Spaziale Italiana, Viale Liegi 26, I-00198 Roma, Italy i Lunar and Planetary Lab and Steward Observatory, University of Arizona, 1629 E.