DOCSLIB.ORG

One-Thousand Leagues Beneath an Extraterrestrial Sea Titan Submarines, Boats, and Dropsondes: Concepts and Technologies

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
One-Thousand Leagues Beneath an Extraterrestrial Sea Titan Submarines, Boats, and Dropsondes: Concepts and Technologies One-Thousand Leagues Beneath an Extraterrestrial Sea Titan Submarines, Boats, and Dropsondes: Concepts and Technologies Steven Oleson (NASA GRC), Ralph Lorenz (JHU/ APL), Michael Paul (JHU/APL), Jason Hartwig (NASA GRC), Justin Walsh (PSU/ARL) Compass Team NASA John H. Glenn Research Center, JHU/APL, PSU/ARL, Washington State U., New York University 1 FISO Telecon July 22, 2020 1 Titan Submarine Team Customer: NASA NIAC, Phases I & II, 2015-2018 • Concept PIs: Steve Oleson (NASA/GRC), Ralph Lorenz (JHU/APL), Michael Paul (JHU/APL), Jason Hartwig (NASA/GRC), Justin Walsh (PSU/ARL) • COMPASS Design Team – Lead - Steve Oleson – Science– Ralph Lorenz (APL) – System Integration, Conops, Launch vehicle – J Michael Newman – Mission – Steve McCarty – GN&C - Mike Martini – Hydrodynamics and Propulsion – Iskender Sahin (NYU), Shane Carberry Morgan (NYU), James Fittje – Mechanical Systems –John Gyekenyesi – Thermal - Tony Colozza – EDL – Evan Roelke (Georgia Tech) – Power - Paul Schmitz – C&DH, Software – Amee Bogner – Communications – Robert Jones – Configuration - Tom Packard – Cost – Tom Parkey, Elizabeth Turnbull • University Support – Washington State - Cryogenic Testing: Ian Richardson 2 2 Titan’s Seas Hundreds of lakes in the north, plus 3 seas : Kraken Mare, Ligeia Mare and Punga Mare (~1000km, 400km, ~200km across respectively). Only one large lake in the south, Ontario Lacus. 3 How Deep Are Ability of Cassini the Seas? radio waves to penetrate seas From Cassini Data: hints as use of RF for submerged Communications! ! Kraken and Ligeia in the north are the best Submersible Targets 4 When to Go: Seasons on Titan • If we want light to image the shore AND direct Earth Communica9ons Best to arrive in summer! (2045) • We can push to spring IF we have an orBiter for relay and suBmerge during ‘night’ (2040) • Trips to Saturn take 7 years or more so we need to launch early to mid 2030s 5 Earth vs. Titan Submarine Parameter Sea Horse UUV Titan Submarine Sea Material Water Liquid Ethane & Methane Density ~1000 kg/m^3 ~650 kg/m^3 / 450 kg/m^3 Temp ~0° to 30°C -178°C Viscosity 1000 uPa-s 200-4000 uPa-s Depth 1000s m 200 m sensed (design max set to 1000 m) Pressure by depth Every 10 m ~1 additional Bar Every 115m ~1 additional Bar Gravity 1 g 0.14g Size ~8m x 1m diameter with internal ballast tanks ~ 6m x .62m with external ballast tanks Mass ~4700 kg ~1200 kg Max Depth 1000 m (100 Bar pressure) 1000 m (~12 Bar pressure) Max Range 550km 5000 km Endurance 72 hours 1 year Speed 2 m/s 1 m/s (max) Power Battery Isotope (860W EOL) Navigation GPS (surfaced) & IMU Sun Sensor, Earth Tracking & IMU Communications Surfaced satellite ~ 800 km Surfaced Direct to Earth ~ 1.5 Billion km Payload Mass ~ 90 kg 6 6 Science • Titan is a target for the Must Do Ocean Worlds Explora9on Science Program Floor • Titan’s seas, while liquid methane Based, are a key part of a weather system like ours Added Science for Desired • Sampling Beneath the sea Baseline (especially the BoNom) could (intensive reveal sediment from Titan inves9ga9on of itself seabed) 7 7 Phase I Sub Concept: Big and Fast! • Autonomous Science Sonar, " Propulsion: Four motors for 1 m/s submerged and 1 m/s surfaced speeds in situ exploration, sampling of bottom sediment • Surface shore imaging and 90 day journey weather Kraken-1 • Two 430W • X-Band Comms direct to Earth Radioisotope Power (~800 bps during 16 hr DSN passes each Systems ~ 6 m long, ~ 1400 kg day surfaced) ~50 Mb per day " Thermal: Interior RPS heated, 3cm aerogel insulation, 300 W/m^2 thru skin, outer systems cryo capable (-178°C) " Navigation: IMU, sun direction, earth tracking, liquid velocity doppler, sonar scanning Power/Size/Mass/Aeroshell: Driven by DTE communications and 1 m/s speed Atlas 5 series using (efficient long narrow shape) and " Closed Ne system with an X-37 derived metal bellows ballast lifting body Science mass/hover needs, needs new tanks submerging and 8 aeroshell hovering down to 1000 m at pressures ~ 10 bar 8 Phase II Titan Turtle: Orbiter Supported " Propulsion: Four motors for • Autonomous Science 180 day Journey around/ 0.3 m/s submerged and 0.2 m/ Sonar, in situ exploration, beneath smaller Ligea Mare s surfaced speeds and sampling of bottom hovering sediment • Surface shore imaging and weather • Thermal: Internal RTG waste heat, 2.5cm aerogel insulation, Single 90W 300 W/m^2 thru skin ~ 2 m long, ~ 500 kg eMMRTG " Navigation using IMU, Orbiter UHF-Band Comms (~100 kbps during five, 30 minute tracking, sonar scanning 1500 km orbiter passes each day surfaced: ~ 1Gb/ SOA 4.5 m day) Aeroshell Providing orbiter relay (even when submerged!) and slowing speed to 0.2 m/s (delivered by " Pressure vessel with external, speed allows reducing mass by 3X and still orbiter) closed He system ballast tanks to providing same science investigations, allow for submerging and hovering smaller shape allows use of SOA 4.5m up to 200 m at pressures < 5 bar aeroshell 9 Phase II: Titan Boat with Dropsondes • Autonomous Science " Propulsion: Four motors for 0.1 m/s Sonar, in situ exploration w surfaced speeds 360 day Journey dropsondes around/beneath • Surface shore imaging and Single 90W EOL Kraken 1 and 2 weather eMMRTG • Boat with large radome to house phased (extended into array antenna and ensure self-righting after Ligeia) landing • Internal systems (including comms/ dropsondes) warmed by RTG waste • X-Band Comms heat, 1.5cm aerogel insulation, 200 W/ (~800 bps during m^2 thru skin) eight hour direct to " Navigation using IMU, sonar scanning, Earth ~ 3 m long, ~ 600 kg earth daily: ~ 30Mb/ SOA 4.5 m day) Aeroshell (delivered by Backing off to just Floor Science goals with cruisedeck) Boat/Dropsonde combination removes need • Battery Powered for ballast system, dropsondes use RF comm Dropsonde senses link to boat, Boat DTE communications allows stand-alone system, still allows use of P, T, Turbidity, SOA 4.5m aeroshell bottom image 10 Titan Submarines Side by Side Titan Design Sea(s) Science Size/ Power Speed/ Class Comms Ballast EDL Explored mass Submerged System FracCon Kraken I & II Desired Science ~ 6m Two, 500 W 1 m/s, 1/3 of Flagship DTE, ~ 50 Mb Ne Gas New, long Suite: ~ 100 kg, long, SMrling Mme submerged per day, with aeroshell surface, sea, BoDom ~1500 Radioisotope isolated insitu sampling, kg Generators metallic 90 day primary bellows Mission Ligeia Mare Desired Science: ~ ~ 2m Single, ~ 0.2 m/s, ½ Mme Works with Relayed Consumabl SOA 4.5 m 100 kg, surface, sea, long, 100W submerged OrBiter, part through e He gas aeroshell boDom insitu ~500 kg eMMRTG of Flagship? orbiter while with sampling, 180 day submerged, ~ conformal primary mission 1Gb per day Ballast tanks Kraken I & II Floor Science Suite: ~ ~ 3 m Single, ~ 0.1 m/s, only New DTE, ~ 30 Mb None SOA 4.5 m and Ligeia 80 kg with drop long, 100W dropsondes FronMers? per day aeroshell Mare if sondes, ~600 kg eMMRTG submerged accessable surface, sea, BoDom (Dropsondes science, BaDery ~ 30 Mb per day, 360 powered, day primary mission short duraMon) 11 Major Risks and Mitigations • Accuracy of Sea data/consistency from Cassini – MiMgaMon: • Develop potenMal sea mixtures and test • Design SuBmersiBles that minimize interacMons with seas (Consumable He or variable volume Ballast systems, dropsondes) • Propulsor operaMon in cryogenic sea – Analyses nearing compleMon to assess pressure drop effervescence impact on propulsion • Ballast Design/operaMon – MiMgaMon: Limit suBmersion to drop sondes or Test in relevant mixtures – Use of orBiter or Boat removes need to surface for comms/navigaMon • Thermal interacMon Between vehicle and sea (Liquid Methane/Ethane absorBs LARGE quanMMes of N2 – and Titan has a dense N2 atmosphere) – Thermally induced Effervescence: TesMng/Modeling show that when using RPS internally with Boat or suBmersiBle 300 Wth/m^2 will NOT create large amounts of BuBBles • CommunicaMons (cryogenic exposure to antennas, transmission through sea) – Cassini RF showed at least three of the seas radio transparent • NavigaMon (Sun/earth/BoDom tracking or navigaMon from orBiter) – Surface: Periodic updates using sun sensing, earth tracking should Be sufficient with IMU – SuBsurface: • IF available: Updates using RF tracking through orBiter or surface relay with IMU • If no RF sources available use BoDom tracking and surface periodically 12 Bubble Incipience Data - Bubble incipience data taken at WSU - Hot plate submerged in various bubbly mixtures - Sub waste heat flux is ~380 W/m2 - Bubble Incipience data taken shows we have a margin of safety of ~3 on thermal side. - Need to run subscale propulsor tests to rule out pressure-driven effervescence Heat Flux at N Sea Data CH C H 2 Pressure Heater Surface Bubble 4 2 6 [mol Temp. Point [mol %] [mol %] [bar] Temp. [K] Incipience [W/ %] [K] m2] 1 87.1 0.0 12.9 1.546 96.2 101.4 10830 2 87.7 0.0 12.3 1.65 93.5 100.2 13029 3 82.5 0.0 17.5 1.782 95.9 99.6 3257 4 72.3 0.0 27.7 4.53 97.0 104.1 17915 5 0.0 97.3 2.7 1.73 103.6 118.7 28810 6 0.0 94.6 5.4 4.41 92.5 107.2 24559 7 50.6 44.2 5.2 1.85 97.8 108.7 18729 8 57.5 37.2 5.3 1.561 92.7 107.8 26448 9 47.6 30.9 21.5 3.21 91.9 97.8 11074 10 24.9 48.3 26.8 3.44 91.9 94.2 2475 11 27.0 61.4 11.6 3.85 91.8 98.8 10244 12 30.2 63.9 5.9 2.133 93.6 111.6 31758 1 13 3 <7 TRL by Design Item Phase I Stand-alone Sub Phase II Orbiter Supported Phase II Ship/Dropsondes Vehicle Level 2-3 2-3 2-3 Science Instruments 3-4 External Cryogenic Science 3-4 External Cryogenic Science 3-4 External Cryogenic Science Instruments Instruments Instruments AD&CS 4 (suBmerged navigaMon using 4 (external sensors,
Load more

Recommended publications
  • Cassini Update
    Cassini Update Dr. Linda Spilker Cassini Project Scientist Outer Planets Assessment Group 22 February 2017 Sols%ce Mission Inclina%on Profile equator Saturn wrt Inclination 22 February 2017 LJS-3 Year 3 Key Flybys Since Aug. 2016 OPAG T124 – Titan flyby (1584 km) • November 13, 2016 • LAST Radio Science flyby • One of only two (cf. T106) ideal bistatic observations capturing Titan’s Northern Seas • First and only bistatic observation of Punga Mare • Western Kraken Mare not explored by RSS before T125 – Titan flyby (3158 km) • November 29, 2016 • LAST Optical Remote Sensing targeted flyby • VIMS high-resolution map of the North Pole looking for variations at and around the seas and lakes. • CIRS last opportunity for vertical profile determination of gases (e.g. water, aerosols) • UVIS limb viewing opportunity at the highest spatial resolution available outside of occultations 22 February 2017 4 Interior of Hexagon Turning “Less Blue” • Bluish to golden haze results from increased production of photochemical hazes as north pole approaches summer solstice. • Hexagon acts as a barrier that prevents haze particles outside hexagon from migrating inward. • 5 Refracting Atmosphere Saturn's• 22unlit February rings appear 2017 to bend as they pass behind the planet’s darkened limb due• 6 to refraction by Saturn's upper atmosphere. (Resolution 5 km/pixel) Dione Harbors A Subsurface Ocean Researchers at the Royal Observatory of Belgium reanalyzed Cassini RSS gravity data• 7 of Dione and predict a crust 100 km thick with a global ocean 10’s of km deep. Titan’s Summer Clouds Pose a Mystery Why would clouds on Titan be visible in VIMS images, but not in ISS images? ISS ISS VIMS High, thin cirrus clouds that are optically thicker than Titan’s atmospheric haze at longer VIMS wavelengths,• 22 February but optically 2017 thinner than the haze at shorter ISS wavelengths, could be• 8 detected by VIMS while simultaneously lost in the haze to ISS.
    [Show full text]
  • Transient Broad Specular Reflections from Titan's North Pole
    Lunar and Planetary Science XLVIII (2017) 1519.pdf TRANSIENT BROAD SPECULAR REFLECTIONS FROM TITAN’S NORTH POLE Rajani Dhingra1, J. W. Barnes1, R. H. Brown2, B J. Buratti3, C. Sotin3, P. D. Nicholson4, K. H. Baines5, R. N. Clark6, J. M. Soderblom7, Ralph Jaumann8, Sebastien Rodriguez9 and Stéphane Le Mouélic10 1Dept. of Physics, University of Idaho, ID,USA, [email protected], 2Dept. of Planetary Sciences, University of Arizona, AZ, USA, 3JPL, Caltech, CA, USA, 4Cornell University, Astronomy Dept., NY, USA, 5Space Science & Engineering Center, University of Wisconsin- Madison, 1225 West Dayton St., WI, USA, 6Planetary Science Institute, Arizona, USA, 7Dept. of Earth, Atmospheric and Planetary Sciences, MIT, Cambridge, USA, 8Deutsches Zentrum für Luft- und Raumfahrt, 12489, Germany, 9Laboratoire AIM, Centre d’etude de Saclay, DAPNIA/Sap, Centre de lorme des Merisiers, 91191 Gif/Yvette, France, 10Laboratoire de Planetologie et Geodynamique, CNRS UMR6112, Universite de Nantes, France. Introduction: The recent Cassini VIMS (Visual and Infrared Mapping Spectrometer) T120 observation of Titan show extensive north polar surface features which might correspond to a broad, off-specular reflec- tion from a wet, rough, solid surface. The observation appears similar in spectral nature to previous specular reflection observations and also has the appropriate geometry. Figure 1 illustrates the geometry of specular reflection from Jingpo Lacus [1], waves from Punga Mare [2] and T120 observation of broad off-specular reflection from land surfaces. We observe specular reflections apart from the observation of broad specular reflection and extensive clouds in the T120 flyby. Our initial mapping shows that the off-specular re- flections occur only over land surfaces.
    [Show full text]
  • 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.
    [Show full text]
  • 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.
    [Show full text]
  • The Exploration of Titan with an Orbiter and a Lake Probe
    Planetary and Space Science ∎ (∎∎∎∎) ∎∎∎–∎∎∎ Contents lists available at ScienceDirect Planetary and Space Science journal homepage: www.elsevier.com/locate/pss The exploration of Titan with an orbiter and a lake probe Giuseppe Mitri a,n, Athena Coustenis b, Gilbert Fanchini c, Alex G. Hayes d, Luciano Iess e, Krishan Khurana f, Jean-Pierre Lebreton g, Rosaly M. Lopes h, Ralph D. Lorenz i, Rachele Meriggiola e, Maria Luisa Moriconi j, Roberto Orosei k, Christophe Sotin h, Ellen Stofan l, Gabriel Tobie a,m, Tetsuya Tokano n, Federico Tosi o a Université de Nantes, LPGNantes, UMR 6112, 2 rue de la Houssinière, F-44322 Nantes, France b Laboratoire d’Etudes Spatiales et d’Instrumentation en Astrophysique (LESIA), Observatoire de Paris, CNRS, UPMC University Paris 06, University Paris-Diderot, Meudon, France c Smart Structures Solutions S.r.l., Rome, Italy d Center for Radiophysics and Space Research, Cornell University, Ithaca, NY 14853, United States e Dipartimento di Ingegneria Meccanica e Aerospaziale, Università La Sapienza, 00184 Rome, Italy f Institute of Geophysics and Planetary Physics, Department of Earth and Space Sciences, Los Angeles, CA, United States g LPC2E-CNRS & LESIA-Obs., Paris, France h Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, United States i Johns Hopkins University, Applied Physics Laboratory, Laurel, MD, United States j Istituto di Scienze dell‘Atmosfera e del Clima (ISAC), Consiglio Nazionale delle Ricerche (CNR), Rome, Italy k Istituto di Radioastronomia (IRA), Istituto Nazionale
    [Show full text]
  • Secrets from Titan's Seas
    Land O’Lakes Secrets from Titan’s seas By probing “magic islands” These images show Titan, from left to right, in October and December 2005 and January and seafloors, astronomers are 2006. The view from December is roughly the opposite side learning more than ever about of the moon from the October and January flybys, but careful inspection of Titan’s polar regions the lakes and seas on Saturn’s shows how dynamic and variable the polar weather can be. NASA/JPL/ largest moon. by Alexander G. Hayes UNIVERSITY OF ARIZONA IMAGINE YOURSELF standing at the shoreline and organic material like plastic shavings or Styrofoam beads. On of a picturesque freshwater lake, surrounded by soft grass and leafy closer inspection, the lake holds not water, but a liquid not unlike trees. Perhaps you are enjoying a peaceful lakefront vacation. In the natural gas. And you’d better be holding your breath because the calm water, you see the mirror-like reflection of a cloudy sky just surrounding air has no oxygen. before it begins to rain. Now, let the surrounding vegetation disap- If you can picture all of this, welcome to the surface of Saturn’s pear, leaving behind a landscape you might more reasonably expect largest moon, Titan. to see in the rocky deserts of the southwestern United States. The Titan is the only extraterrestrial body known to support standing temperature is dropping too, all the way down to a bone-chilling bodies of liquid on its surface and the only moon with a dense atmo- –295° F (92 kelvins).
    [Show full text]
  • Titan Submarine
    NASA/TM—2015-218831 Phase I Final Report: Titan Submarine Steven R. Oleson Glenn Research Center, Cleveland, Ohio Ralph D. Lorenz Johns Hopkins University, Applied Physics Laboratory, Laurel, Maryland Michael V. Paul The Pennsylvania State University, Applied Research Laboratory, State College, Pennsylvania July 2015 NASA STI Program . in Profile Since its founding, NASA has been dedicated • CONTRACTOR REPORT. Scientific and to the advancement of aeronautics and space science. technical findings by NASA-sponsored The NASA Scientific and Technical Information (STI) contractors and grantees. Program plays a key part in helping NASA maintain this important role. • CONFERENCE PUBLICATION. Collected papers from scientific and technical conferences, symposia, seminars, or other The NASA STI Program operates under the auspices meetings sponsored or co-sponsored by NASA. of the Agency Chief Information Officer. It collects, organizes, provides for archiving, and disseminates • SPECIAL PUBLICATION. Scientific, NASA’s STI. The NASA STI Program provides access technical, or historical information from to the NASA Technical Report Server—Registered NASA programs, projects, and missions, often (NTRS Reg) and NASA Technical Report Server— concerned with subjects having substantial Public (NTRS) thus providing one of the largest public interest. collections of aeronautical and space science STI in the world. Results are published in both non-NASA • TECHNICAL TRANSLATION. English- channels and by NASA in the NASA STI Report language translations of foreign scientific and Series, which includes the following report types: technical material pertinent to NASA’s mission. • TECHNICAL PUBLICATION. Reports of For more information about the NASA STI completed research or a major significant phase program, see the following: of research that present the results of NASA programs and include extensive data or theoretical • Access the NASA STI program home page at analysis.
    [Show full text]
  • 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.
    [Show full text]
  • Titan Submarine: Exploring the Depths of Kraken Mare
    Titan Submarine: Exploring The Depths of Kraken Mare Steven R. Oleson1 NASA Glenn Research Center, Cleveland, Ohio 44135 Ralph D. Lorenz2 Johns Hopkins University, Applied Physics Laboratory, Laurel, Maryland 20723 Michael V. Paul3 The Pennsylvania State University, Applied Research Laboratory, State College, Pennsylvania 16804 The conceptual design of a submarine for Saturn’s moon Titan was a funded NASA’s Innovative Advanced Concepts (NIAC) Phase I for 2014. The effort investigated what science a submarine for Titan’s liquid hydrocarbon ~93 K (–180 °C) seas might accomplish and what that submarine might look like. Focusing on a flagship class science system (~100 kg) it was found that a submersible platform can accomplish extensive and exciting science both above and below the surface of the Kraken Mare The submerged science includes mapping using side looking sonar, imaging and spectroscopy of the sea at all depths, as well as sampling of the sea’s bottom and shallow shoreline. While surfaced the submarine will not only sense weather conditions (including the interaction between the liquid and atmosphere) but also image the shoreline, as much as 2 km inland. This imaging requirement pushed the landing date to Titan’s next summer period (~2047) to allow for continuous lighted conditions, as well as direct-to-Earth (DTE) communication, avoiding the need for a separate relay orbiter spacecraft. Submerged and surfaced investigation are key to understanding both the hydrological cycle of Titan as well as gather hints to how life may have begun on Earth using liquid/sediment/chemical interactions. An estimated 25 Mb of data per day would be generated by the various science packages.
    [Show full text]
  • The Bathymetry of Moray Sinus at Titan's Kraken Mare
    The bathymetry of Moray Sinus at Titan’s Kraken Mare Valerio Poggiali, Alexander G. Hayes, Marco Mastrogiuseppe, Alice Le Gall, D. Lalich, I. Gomez-Leal, Jonathan Lunine To cite this version: Valerio Poggiali, Alexander G. Hayes, Marco Mastrogiuseppe, Alice Le Gall, D. Lalich, et al.. The bathymetry of Moray Sinus at Titan’s Kraken Mare. Journal of Geophysical Research. Planets, Wiley-Blackwell, 2020, 125 (12), pp.e2020JE006558. 10.1029/2020JE006558. insu-03003839 HAL Id: insu-03003839 https://hal-insu.archives-ouvertes.fr/insu-03003839 Submitted on 4 Dec 2020 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. RESEARCH ARTICLE The Bathymetry of Moray Sinus at Titan s Kraken Mare 10.1029/2020JE006558 V. Poggiali1 , A. G. Hayes1,2 , M. Mastrogiuseppe3 , A. Le Gall4,5 ' , D. Lalich1 , 1 1,2 Key Points: I. Gómez-Leal , and J. I. Lunine • Moray Sinus is an estuary located at 1Cornell Center for Astrophysics and Planetary Science, Cornell University, Ithaca, NY, USA, 2Astronomy Department, the northern end of Titan s Kraken 3 Mare ' Cornell University, Ithaca, NY, USA, Dipartimento di Ingegneria Dell'Informazione, Elettronica e Telecomunicazioni, 4 • Analysis of Cassini s radar altimeter Università di Roma La Sapienza, Rome, Italy, LATMOS/IPSL, UVSQ Université Paris-Saclay, Sorbonne Université, data shows that the' near-shore local CNRS, Paris, France, 5Institut Universitaire de France (IUF), Paris, France seafloor is up to 85 m deep in Moray Sinus estuary • The composition of the sea, inferred Moray Sinus is an estuary located at the northern end of Titan s Kraken Mare.
    [Show full text]
  • CASSINI TOST T109 SEGMENT Rev 212 Handoff Package
    CASSINI TOST T109 SEGMENT Rev 212 Handoff Package Segment Boundary 2015-042T23:51:00 – 2015-045T03:51:00 17 June 2014 J. Pitesky Science Highlights Notes & Liens This document has been reviewed and determined not to contain export controlled technical data Science Highlights TOST rev 212 DOY 043 (Feb 11) – Inbound to Titan, VIMS will image the South Pole to witness the evolution of the South Polar vortex. It will then make a mosaic of the sub-Saturn tropical zone that include dunes fields and plateaus. It will also look for clouds at northern mid- latitudes. Then, the VIMS will use the push-broom mode to take a high resolution swath across the polar cap North of 60 deg. This path will cross Punga Mare and possibly Kivu Lacus, looking for compositional differences in the faculae and the dunes. , VIMS will first look for specular reflection on the northeastern tip of Kraken Mare and across the straitthat links Kraken and Ligeia. It will then acquire a few high-resolution images of the lakes before handing off to CIRS. Just after closest approach, CIRS performs limb sounding in the far-infrared at 50N to extend spatial coverage of gas and aerosol vertical distributions. ISS will ride along with VIMS, UVIS, and CIRS to image Titan's surface and atmosphere over the equatorial sub-Saturnian hemisphere, including northern Tsegihi and eastern Aztlan. DOY 044 (Feb 12) – CIRS performs limb sounding in the far-infrared at 50N to extend spatial coverage of gas and aerosol vertical distributions. – ISS will ride along with VIMS, UVIS, and CIRS to image Titan's surface and atmosphere at high phase angle.
    [Show full text]
  • Cassini RADAR Users Guide Second Edition
    Cassini RADAR Users Guide Second Edition S.D. Wall, R.L. Kirk, B.W. Stiles, A. Hayes, K. Mitchell, R.D. Lorenz, M. Janssen, B. Bills, V. Poggiali, A. Schoenfeld, and the Cassini RADAR Science Team JPL D-102030 September 2019 The authors wish to thank Ellen Stofan, Yanhua Anderson, Rudy Boehmer, Trina Ray, and Reta Bebe for their assistance in producing this document, and especially Charles Elachi, whose guidance and support have led us in this amazingly successful experiment. We also thank Claire Marie-Peterson for helpful comments and superb editing. This publication was prepared for the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. Reference herein to any specific commercial product, process, or service by trade name, trademark, manufacturer, or otherwise, does not constitute or imply its endorsement by the United States Government or the Jet Propulsion Laboratory, California Institute of Technology. This guide is dedicated to the memory of Bill Johnson and Steve Ostro. They were fundamental to the success of the Cassini RADAR, and we miss them not only as colleagues, but as friends. Cassini RADAR Users Guide Contents Preface to the Second Edition .................................................................................................................... 1 1 Introduction ............................................................................................................................................... 2 2 The Cassini Spacecraft
    [Show full text]