Cassini Sheds Light on Titan's Second Largest Lake, Ligeia Mare 11 March 2014

Total Page:16

File Type:pdf, Size:1020Kb

Cassini Sheds Light on Titan's Second Largest Lake, Ligeia Mare 11 March 2014 Cassini sheds light on Titan's second largest lake, Ligeia Mare 11 March 2014 Saturn's second largest moon, Titan, is known for its dense, planet-like atmosphere and large lakes most likely made of methane and ethane. It has been suggested that Titan's atmosphere and surface is a model of early Earth. Since the early 2000s, NASA's Cassini space probe has been unlocking secrets of the distant moon. The most recent Cassini flyby of Titan on 23 May 2013 reveals new observations of Ligeia Mare, Titan's second largest lake, and offers insight into weather patterns and the chemical makeup of the surrounding terrain. Zebker et al. used radar data to determine that the surface of the lake is flat, ruling out the presence of waves or wind in the region. Other measurements, consistent with previous observations, suggest that Ligeia Mare is most likely composed of liquid methane. They also find that the surrounding solid terrain is most likely made of solid organic material and not water ice. The authors suggest that these findings not only help scientists to better understand Titan's surface dynamics, but also reveal best practices for how to infer features from remotely sensed data. More information: Surface of Ligeia Mare, Titan, from Cassini altimeter and radiometer analysis, Geophysical Research Letters, DOI: 10.1002/2013GL058877 , 2013. Provided by American Geophysical Union APA citation: Cassini sheds light on Titan's second largest lake, Ligeia Mare (2014, March 11) retrieved 1 October 2021 from https://phys.org/news/2014-03-cassini-titan-largest-lake-ligeia.html This document is subject to copyright. Apart from any fair dealing for the purpose of private study or research, no part may be reproduced without the written permission. The content is provided for information purposes only. 1 / 1 Powered by TCPDF (www.tcpdf.org).
Recommended publications
  • Surface of Ligeia Mare, Titan, from Cassini Altimeter and Radiometer Analysis Howard Zebker, Alex Hayes, Mike Janssen, Alice Le Gall, Ralph Lorenz, Lauren Wye
    Surface of Ligeia Mare, Titan, from Cassini altimeter and radiometer analysis Howard Zebker, Alex Hayes, Mike Janssen, Alice Le Gall, Ralph Lorenz, Lauren Wye To cite this version: Howard Zebker, Alex Hayes, Mike Janssen, Alice Le Gall, Ralph Lorenz, et al.. Surface of Ligeia Mare, Titan, from Cassini altimeter and radiometer analysis. Geophysical Research Letters, American Geophysical Union, 2014, 41 (2), pp.308-313. 10.1002/2013GL058877. hal-00926152 HAL Id: hal-00926152 https://hal.archives-ouvertes.fr/hal-00926152 Submitted on 19 Jul 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. PUBLICATIONS Geophysical Research Letters RESEARCH LETTER Surface of Ligeia Mare, Titan, from Cassini 10.1002/2013GL058877 altimeter and radiometer analysis Key Points: Howard Zebker1, Alex Hayes2, Mike Janssen3, Alice Le Gall4, Ralph Lorenz5, and Lauren Wye6 • Ligeia Mare, like Ontario Lacus, is flat with no evidence of ocean waves or wind 1Departments of Geophysics and Electrical Engineering, Stanford University, Stanford, California, USA, 2Department of • The
    [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 a Moon with an Atmosphere
    TITAN A MOON WITH AN ATMOSPHERE Ashley Gilliam Earth 450 – Satellites of Jupiter and Saturn 4/29/13 SATURN HAS > 60 SATELLITES, WHY TITAN? Is the only satellite with a dense atmosphere Has a nitrogen-rich atmosphere resembles Earth’s Is the only world besides Earth with a liquid on its surface • Possible habitable world Based on its size… Titan " a planet in its o# $ght! R = 6371 km R = 2576 km R = 1737 km Ch$%iaan Huy&ns (1629-1695) DISCOVERY OF TITAN Around 1650, Huygens began building telescopes with his brother Constantijn On March 25, 1655 Huygens discovered Titan in an attempt to study Saturn’s rings Named the moon Saturni Luna (“Saturns Moon”) Not properly named until the mid-1800’s THE DISCOVERY OF TITAN’S ATMOSPHERE Not much more was learned about Titan until the early 20th century In 1903, Catalan astronomer José Comas Solà claimed to have observed limb darkening on Titan, which requires the presence of an atmosphere Gerard P. Kuiper (1905-1973) José Comas Solà (1868-1937) This was confirmed by Gerard Kuiper in 1944 Image Credit: Ralph Lorenz Voyager 1 Launched September 5, 1977 M"sions to Titan Pioneer 11 Launched April 6, 1973 Cassini-Huygens Images: NASA Launched October 15, 1997 Pioneer 11 Could not penetrate Titan’s Atmosphere! Image Credit: NASA Vo y a &r 1 Image Credit: NASA Vo y a &r 1 What did we learn about the Atmosphere? • Composition (N2, CH4, & H2) • Variation with latitude (homogeneously mixed) • Temperature profile Mesosphere • Pressure profile Stratosphere Troposphere Image Credit: Fulchignoni, et al., 2005 Image Credit: Conway et al.
    [Show full text]
  • The Titan Mare Explorer Mission (Time): a Discovery Mission to a Titan Sea
    EPSC Abstracts Vol. 6, EPSC-DPS2011-909-1, 2011 EPSC-DPS Joint Meeting 2011 c Author(s) 2011 The Titan Mare Explorer Mission (TiME): A Discovery mission to a Titan sea E.R. Stofan (1), J.I. Lunine (2), R.D. Lorenz (3), O. Aharonson (4), E. Bierhaus (5), J. Boldt (3), B. Clark (6), C. Griffith (7), A-M. Harri (8), E. Karkoschka (7), R. Kirk (9), P. Mahaffy (10), C. Newman (11), M. Ravine (12), M. Trainer (10), E. Turtle (3), H. Waite (13), M. Yelland (14) and J. Zarnecki (15) (1) Proxemy Research, Rectortown, VA 20140; (2) Dipartimento di Fisica, Università degli Studi di Roma “Tor Vergata", Rome, Italy; (3) Applied Physics Laboratory, Johns Hopkins University, Laurel MD 20723; (4) California Institute of Technology, Pasadena, CA 91125; (5) Lockheed Martin, Denver, CO; (6) Space Science Institute, Boulder CO 80301; (7) LPL, U. Arizona, Tucson, AZ 85721; (8) Finnish Meteorological Institute, Finland; (9) U.S.G.S. Flagstaff, AZ 86001; (10) NASA Goddard SFC, Greenbelt, MD 20771; (11) Ashima Research, Pasadena, CA 91106; (12) Malin Space Science Systems, San Diego, CA 92191; (13) SWRI, San Antonio, TX 78228; (14) NOC, Univ. Southampton, Southampton, UK SO14 3ZH; (15) PSSRI, The Open University, Milton Keynes, UK MK7 6B Abstract subsurface liquid hydrocarbon table, and are likely hold some combination of liquid methane and liquid The Titan Mare Explorer (TiME) is a Discovery class ethane. Titan’s seas probably contain dissolved mission to Titan, and would be the first in situ amounts of many other compounds, including exploration of an extraterrestrial sea.
    [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]
  • AVIATR—Aerial Vehicle for In-Situ and Airborne Titan Reconnaissance a Titan Airplane Mission Concept
    Exp Astron DOI 10.1007/s10686-011-9275-9 ORIGINAL ARTICLE AVIATR—Aerial Vehicle for In-situ and Airborne Titan Reconnaissance A Titan airplane mission concept Jason W. Barnes · Lawrence Lemke · Rick Foch · Christopher P. McKay · Ross A. Beyer · Jani Radebaugh · David H. Atkinson · Ralph D. Lorenz · Stéphane Le Mouélic · Sebastien Rodriguez · Jay Gundlach · Francesco Giannini · Sean Bain · F. Michael Flasar · Terry Hurford · Carrie M. Anderson · Jon Merrison · Máté Ádámkovics · Simon A. Kattenhorn · Jonathan Mitchell · Devon M. Burr · Anthony Colaprete · Emily Schaller · A. James Friedson · Kenneth S. Edgett · Angioletta Coradini · Alberto Adriani · Kunio M. Sayanagi · Michael J. Malaska · David Morabito · Kim Reh Received: 22 June 2011 / Accepted: 10 November 2011 © The Author(s) 2011. This article is published with open access at Springerlink.com J. W. Barnes (B) · D. H. Atkinson · S. A. Kattenhorn University of Idaho, Moscow, ID 83844-0903, USA e-mail: [email protected] L. Lemke · C. P. McKay · R. A. Beyer · A. Colaprete NASA Ames Research Center, Moffett Field, CA, USA R. Foch · Sean Bain Naval Research Laboratory, Washington, DC, USA R. A. Beyer Carl Sagan Center at the SETI Institute, Mountain View, CA, USA J. Radebaugh Brigham Young University, Provo, UT, USA R. D. Lorenz Johns Hopkins University Applied Physics Laboratory, Silver Spring, MD, USA S. Le Mouélic Laboratoire de Planétologie et Géodynamique, CNRS, UMR6112, Université de Nantes, Nantes, France S. Rodriguez Université de Paris Diderot, Paris, France Exp Astron Abstract We describe a mission concept for a stand-alone Titan airplane mission: Aerial Vehicle for In-situ and Airborne Titan Reconnaissance (AVI- ATR). With independent delivery and direct-to-Earth communications, AVI- ATR could contribute to Titan science either alone or as part of a sustained Titan Exploration Program.
    [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]
  • CASSINI TOST T109 SEGMENT Rev 210 Handoff Package
    CASSINI TOST T109 SEGMENT Rev 210 Handoff Package Segment Boundary 2014-344T03:30:00 – 2014-346T07:00:00 17 Apr 2014 J. Pitesky Science Highlights Notes & Liens This document has been reviewed and determined not to contain export controlled technical data Science Highlights (1 of 2) TOST rev 210 DOY 344 (Dec. 10): T107 is the second pass in the Solstice Mission where INMS and the navigation team will simultaneously measure Titan’s atmosphere. This is critical to understanding the differences in the calculated densities of INMS, Nav, AACS and UVIS. Navigation will determine Titan's atmospheric density by measuring the acceleration of drag on the spacecraft with Doppler shift observations during this NAV 10-point flyby. On the inbound wing, CIRS focuses on high spectral resolution observations in the far- infrared to determine the abundances of trace species. ISS will acquire a mosaic of mid- southern latitudes, including northern Tsegihi, on Titan's sub-Saturnian hemisphere. ISS will also ride along with CIRS and VIMS, to image Titan's surface and atmosphere at mid- southern latitudes on sub-Saturnian hemisphere . VIMS will ride along with CIRS and ISS and will acquire low resolution images (50 km/pixel) of the sub-Saturn hemisphere, observe the evolution of the South Pole vortex, and monitor cloud activity. T107 is a low altitude (980 km) dayside high inclination flyby similar to T106, T105 and T104 occurring in the midnight sector of Saturn’s magnetosphere. With closest approach near the terminator, Cassini will be able to study the draping and the diffusion of the external magnetic field within the ionosphere over the flank facing Saturn.
    [Show full text]
  • 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.
    [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]
  • Titan Mare Explorer
    TiME Titan Mare Explorer Titan Mare Explorer (TiME): Proxemy Research First Exploration of an Extraterrestrial Sea Ellen Stofan TiME Science . Discovery of lakes and seas in Titan’s northern hemisphere confirmed the expectation that liquid hydrocarbons exist . Detection of the presence of ethane in Ontario Lacus near the South Pole (Brown et al., 2008) . 2 distinct types of features- lakes and seas, likely 10’s, >100 m deep . Post-Cassini, major questions will remain on the chemistry of sea liquids, their role in the overall methane cycle, the origin of sea basins, and seasonal processes and variability TiME Proprietary Information/Competition Sensitive Titan’s methane cycle • Titan’s methane cycle is analogous to Earth’s hydrologic cycle, with meteorological working fluid existing in condensed phase on surface and within crust, cycling through the surface atmosphere system and transporting mass and energy TiME Proprietary Information/Competition Sensitive TiME Science Target •Target: Ligeia Mare (78°N, 250°W) –One of the largest seas identified to date on Titan, surface area ~100,000 km2 –Backup target- Kraken Mare TiME Proprietary Information/Competition Sensitive TiME Science Team .PI: Ellen Stofan (Proxemy Research) .Co-Is: .Jonathan Lunine (Univ. of Az.) - Deputy PI .Ralph Lorenz (APL)- Project Scientist .Oded Aharonson (CalTech) .Beau Bierhaus (LM) .Ben Clark (SSI) .Caitlin Griffith (Univ. Arizona) .Ari-Matti Harri (FMI) .Erich Karkoschka (Univ. Arizona) .Randy Kirk (USGS) .Paul Mahaffy (Goddard) .Claire Newman (Ashima Research) .Mike Ravine (MSSS) .Melissa Trainer (GSFC) .Elizabeth Turtle (APL) .Hunter Waite (SWRI) .Margaret Yelland (Univ. Southampton) .John Zarnecki (Open University) TiME Proprietary Information/Competition Sensitive TiME Science Goals and Objectives .
    [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]