Titan As an Analog of Earth's Past and Future
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The Geology of the Rocky Bodies Inside Enceladus, Europa, Titan, and Ganymede
49th Lunar and Planetary Science Conference 2018 (LPI Contrib. No. 2083) 2905.pdf THE GEOLOGY OF THE ROCKY BODIES INSIDE ENCELADUS, EUROPA, TITAN, AND GANYMEDE. Paul K. Byrne1, Paul V. Regensburger1, Christian Klimczak2, DelWayne R. Bohnenstiehl1, Steven A. Hauck, II3, Andrew J. Dombard4, and Douglas J. Hemingway5, 1Planetary Research Group, Department of Marine, Earth, and Atmospheric Sciences, North Carolina State University, Raleigh, NC 27695, USA ([email protected]), 2Department of Geology, University of Georgia, Athens, GA 30602, USA, 3Department of Earth, Environmental, and Planetary Sciences, Case Western Reserve University, Cleveland, OH 44106, USA, 4Department of Earth and Environmental Sciences, University of Illinois at Chicago, Chicago, IL 60607, USA, 5Department of Earth & Planetary Science, University of California Berkeley, Berkeley, CA 94720, USA. Introduction: The icy satellites of Jupiter and horizontal stresses, respectively, Pp is pore fluid Saturn have been the subjects of substantial geological pressure (found from (3)), and μ is the coefficient of study. Much of this work has focused on their outer friction [12]. Finally, because equations (4) and (5) shells [e.g., 1–3], because that is the part most readily assess failure in the brittle domain, we also considered amenable to analysis. Yet many of these satellites ductile deformation with the relation n –E/RT feature known or suspected subsurface oceans [e.g., 4– ε̇ = C1σ exp , (6) 6], likely situated atop rocky interiors [e.g., 7], and where ε̇ is strain rate, C1 is a constant, σ is deviatoric several are of considerable astrobiological significance. stress, n is the stress exponent, E is activation energy, R For example, chemical reactions at the rock–water is the universal gas constant, and T is temperature [13]. -
Cassini RADAR Images at Hotei Arcus and Western Xanadu, Titan: Evidence for Geologically Recent Cryovolcanic Activity S
GEOPHYSICAL RESEARCH LETTERS, VOL. 36, L04203, doi:10.1029/2008GL036415, 2009 Click Here for Full Article Cassini RADAR images at Hotei Arcus and western Xanadu, Titan: Evidence for geologically recent cryovolcanic activity S. D. Wall,1 R. M. Lopes,1 E. R. Stofan,2 C. A. Wood,3 J. L. Radebaugh,4 S. M. Ho¨rst,5 B. W. Stiles,1 R. M. Nelson,1 L. W. Kamp,1 M. A. Janssen,1 R. D. Lorenz,6 J. I. Lunine,5 T. G. Farr,1 G. Mitri,1 P. Paillou,7 F. Paganelli,2 and K. L. Mitchell1 Received 21 October 2008; revised 5 January 2009; accepted 8 January 2009; published 24 February 2009. [1] Images obtained by the Cassini Titan Radar Mapper retention age comparable with Earth or Venus (500 Myr) (RADAR) reveal lobate, flowlike features in the Hotei [Lorenz et al., 2007]). Arcus region that embay and cover surrounding terrains and [4] Most putative cryovolcanic features are located at mid channels. We conclude that they are cryovolcanic lava flows to high northern latitudes [Elachi et al., 2005; Lopes et al., younger than surrounding terrain, although we cannot reject 2007]. They are characterized by lobate boundaries and the sedimentary alternative. Their appearance is grossly relatively uniform radar properties, with flow features similar to another region in western Xanadu and unlike most brighter than their surroundings. Cryovolcanic flows are of the other volcanic regions on Titan. Both regions quite limited in area compared to the more extensive dune correspond to those identified by Cassini’s Visual and fields [Radebaugh et al., 2008] or lakes [Hayes et al., Infrared Mapping Spectrometer (VIMS) as having variable 2008]. -
A 5-Micron-Bright Spot on Titan: Evidence for Surface Diversity
R EPORTS coated SiN lines corresponds to voids at SiN- surface imaging in physical sciences, engi- 19. R. E. Geer, O. V. Kolosov, G. A. D. Briggs, G. S. polymer interfaces (i.e., voiding underneath the neered systems, and biology. Shekhawat, J. Appl. Phys. 91, 4549 (2002). 20. O. Kolosov, R. M. Castell, C. D. Marsh, G. A. D. Briggs, contact). The contrast is due to the distinct Phys. Rev. Lett. 81, 1046 (1998). viscoelastic response from the specimen acous- References and Notes 21. D. C. Hurley, K. Shen, N. M. Jennett, J. A. Turner, J. tic wave from the voids. Interestingly, a notable 1. H. N. Lin, Appl. Phys. Lett. 74, 2785 (1999). Appl. Phys. 94, 2347 (2003). 2. M. R. VanLandingham et al., in Interfacial Engineering 22. O. Hirotsugu, T. Jiayong, T. Toyokazu, H. Masahiko, hardening of the polymer in the trench and its for Optimized Properties,C.L.Briant,C.B.Carter, Appl. Phys. Lett. 83, 464 (2003). sidewall is also evident in the phase image, E. L. Hall, Eds., vol. 458 of Materials Research Society 23. L. Muthuswami, R. E. Geer, Appl. Phys. Lett. 84, 5082 which results from thermal annealing and pos- Proceedings (Materials Research Society, Pittsburgh, (2004). PA, 1997), pp. 313–318. 24. M. T. Cuberes, H. E. Assender, G. A. D. Briggs, O. V. sibly poor adhesion with SOD. Because it is 3. M. R. VanLandingham et al., J. Adhesion 64, 31 (1997). Kolosov, J. Phys. D 33, 2347 (2000). nondestructive, SNFUH may be an ideal tool- 4. B. Bhushan, L. Huiwen, Nanotechnology 15,1785 25. -
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 -
National Reconnaissance Office Review and Redaction Guide
NRO Approved for Release 16 Dec 2010 —Tep-nm.T7ymqtmthitmemf- (u) National Reconnaissance Office Review and Redaction Guide For Automatic Declassification Of 25-Year-Old Information Version 1.0 2008 Edition Approved: Scott F. Large Director DECL ON: 25x1, 20590201 DRV FROM: NRO Classification Guide 6.0, 20 May 2005 NRO Approved for Release 16 Dec 2010 (U) Table of Contents (U) Preface (U) Background 1 (U) General Methodology 2 (U) File Series Exemptions 4 (U) Continued Exemption from Declassification 4 1. (U) Reveal Information that Involves the Application of Intelligence Sources and Methods (25X1) 6 1.1 (U) Document Administration 7 1.2 (U) About the National Reconnaissance Program (NRP) 10 1.2.1 (U) Fact of Satellite Reconnaissance 10 1.2.2 (U) National Reconnaissance Program Information 12 1.2.3 (U) Organizational Relationships 16 1.2.3.1. (U) SAF/SS 16 1.2.3.2. (U) SAF/SP (Program A) 18 1.2.3.3. (U) CIA (Program B) 18 1.2.3.4. (U) Navy (Program C) 19 1.2.3.5. (U) CIA/Air Force (Program D) 19 1.2.3.6. (U) Defense Recon Support Program (DRSP/DSRP) 19 1.3 (U) Satellite Imagery (IMINT) Systems 21 1.3.1 (U) Imagery System Information 21 1.3.2 (U) Non-Operational IMINT Systems 25 1.3.3 (U) Current and Future IMINT Operational Systems 32 1.3.4 (U) Meteorological Forecasting 33 1.3.5 (U) IMINT System Ground Operations 34 1.4 (U) Signals Intelligence (SIGINT) Systems 36 1.4.1 (U) Signals Intelligence System Information 36 1.4.2 (U) Non-Operational SIGINT Systems 38 1.4.3 (U) Current and Future SIGINT Operational Systems 40 1.4.4 (U) SIGINT -
Cassini Reveals Earth-Like Land on Titan 20 July 2006
Cassini Reveals Earth-like Land on Titan 20 July 2006 at the University of Arizona, Tucson. "Surprisingly, this cold, faraway region has geological features remarkably like Earth." Titan is a place of twilight, dimmed by a haze of hydrocarbons surrounding it. Cassini's radar instrument can see through the haze by bouncing radio signals off the surface and timing their return. In the radar images bright regions indicate rough or scattering material, while a dark region might be smoother or more absorbing material, possibly liquid. Xanadu was first discovered by NASA's Hubble Space Telescope in 1994 as a striking bright spot This radar image shows a network of river channels at seen in infrared imaging. When Cassini's radar Xanadu, the continent-sized region on Saturn's moon system viewed Xanadu on April 30, 2006, it found a Titan. Image credit: NASA/JPL surface modified by winds, rain, and the flow of liquids. At Titan's frigid temperatures, the liquid cannot be water; it is almost certainly methane or ethane. New radar images from NASA's Cassini spacecraft revealed geological features similar to Earth on "Although Titan gets far less sunlight and is much Xanadu, an Australia-sized, bright region on smaller and colder than Earth, Xanadu is no longer Saturn's moon Titan. just a mere bright spot, but a land where rivers flow down to a sunless sea," Lunine said. These radar images, from a strip more than 2,796 miles long, show Xanadu is surrounded by darker Observations by the European Space Agency's terrain, reminiscent of a free-standing landmass. -
Simon Porter , Will Grundy
Post-Capture Evolution of Potentially Habitable Exomoons Simon Porter1,2, Will Grundy1 1Lowell Observatory, Flagstaff, Arizona 2School of Earth and Space Exploration, Arizona State University [email protected] and spin vector were initially pointed at random di- Table 1: Relative fraction of end states for fully Abstract !"# $%& " '(" !"# $%& # '(# rections on the sky. The exoplanets had a ran- evolved exomoon systems dom obliquity < 5 deg and was at a stellarcentric The satellites of extrasolar planets (exomoons) Star Planet Moon Survived Retrograde Separated Impacted distance such that the equilibrium temperature was have been recently proposed as astrobiological tar- Earth 43% 52% 21% 35% equal to Earth. The simulations were run until they Jupiter Mars 44% 45% 18% 37% gets. Triton has been proposed to have been cap- 5 either reached an eccentricity below 10 or the pe- Titan 42% 47% 21% 36% tured through a momentum-exchange reaction [1], − Sun Earth 52% 44% 17% 30% riapse went below the Roche limit (impact) or the and it is possible that a similar event could allow Neptune Mars 44% 45% 18% 36% apoapse exceeded the Hill radius. Stars used were Titan 45% 47% 19% 35% a giant planet to capture a formerly binary terres- Earth 65% 47% 3% 31% the Sun (G2), a main-sequence F0 (1.7 MSun), trial planet or planetesimal. We therefore attempt to Jupiter Mars 59% 46% 4% 35% and a main-sequence M0 (0.47 MSun). Exoplan- Titan 61% 48% 3% 34% model the dynamical evolution of a terrestrial planet !"# $%& " !"# $%& " ' F0 ets used had the mass of either Jupiter or Neptune, Earth 77% 44% 4% 18% captured into orbit around a giant planet in the hab- and exomoons with the mass of Earth, Mars, and Neptune Mars 67% 44% 4% 28% itable zone of a star. -
Saturn Satellites As Seen by Cassini Mission
Saturn satellites as seen by Cassini Mission A. Coradini (1), F. Capaccioni (2), P. Cerroni(2), G. Filacchione(2), G. Magni,(2) R. Orosei(1), F. Tosi(1) and D. Turrini (1) (1)IFSI- Istituto di Fisica dello Spazio Interplanetario INAF Via fosso del Cavaliere 100- 00133 Roma (2)IASF- Istituto di Astrofisica Spaziale e Fisica Cosmica INAF Via fosso del Cavaliere 100- 00133 Roma Paper to be included in the special issue for Elba workshop Table of content SATURN SATELLITES AS SEEN BY CASSINI MISSION ....................................................................... 1 TABLE OF CONTENT .................................................................................................................................. 2 Abstract ....................................................................................................................................................................... 3 Introduction ................................................................................................................................................................ 3 The Cassini Mission payload and data ......................................................................................................................... 4 Satellites origin and bulk characteristics ...................................................................................................................... 6 Phoebe ............................................................................................................................................................................... -
Titan Fact Sheet Titan Is a Large Moon Orbiting the Planet Saturn, About
Titan Fact Sheet Titan is a large moon orbiting the planet Saturn, about 866 million miles from the sun. The surface of Titan is hidden by the thick, hazy atmosphere, but in the past few years spacecraft have managed to collect images and other data that tell us about what lies beneath the haze. They found something that’s common on Earth but very unusual in the rest of the solar system: lakes and seas! Besides Earth, Titan is the only body in our solar system with enough liquid on its surface to fill lakes and seas. Titan’s lakes and seas are filled mainly with thick tar-like substances, such as methane and ethane. Titan also has methane gas in its atmosphere, just as Earth has water vapor in its atmosphere. Titan has summer and winter seasons when its surface becomes warmer and colder. However, because it is so far from the sun, even in summer Titan is very cold. Its average surface temperature is about -179 degrees Celsius or -290 degrees Fahrenheit. Titan Fact Sheet Titan is a large moon orbiting the planet Saturn, about 866 million miles from the sun. The surface of Titan is hidden by the thick, hazy atmosphere, but in the past few years spacecraft have managed to collect images and other data that tell us about what lies beneath the haze. They found something that’s common on Earth but very unusual in the rest of the solar system: lakes and seas! Besides Earth, Titan is the only body in our solar system with enough liquid on its surface to fill lakes and seas. -
The Cassini-Huygens Mission Overview
SpaceOps 2006 Conference AIAA 2006-5502 The Cassini-Huygens Mission Overview N. Vandermey and B. G. Paczkowski Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109 The Cassini-Huygens Program is an international science mission to the Saturnian system. Three space agencies and seventeen nations contributed to building the Cassini spacecraft and Huygens probe. The Cassini orbiter is managed and operated by NASA's Jet Propulsion Laboratory. The Huygens probe was built and operated by the European Space Agency. The mission design for Cassini-Huygens calls for a four-year orbital survey of Saturn, its rings, magnetosphere, and satellites, and the descent into Titan’s atmosphere of the Huygens probe. The Cassini orbiter tour consists of 76 orbits around Saturn with 45 close Titan flybys and 8 targeted icy satellite flybys. The Cassini orbiter spacecraft carries twelve scientific instruments that are performing a wide range of observations on a multitude of designated targets. The Huygens probe carried six additional instruments that provided in-situ sampling of the atmosphere and surface of Titan. The multi-national nature of this mission poses significant challenges in the area of flight operations. This paper will provide an overview of the mission, spacecraft, organization and flight operations environment used for the Cassini-Huygens Mission. It will address the operational complexities of the spacecraft and the science instruments and the approach used by Cassini- Huygens to address these issues. I. The Mission Saturn has fascinated observers for over 300 years. The only planet whose rings were visible from Earth with primitive telescopes, it was not until the age of robotic spacecraft that questions about the Saturnian system’s composition could be answered. -
Cassini-Huygens
High Ambitions for an Outstanding Planetary Mission: Cassini-Huygens Composite image of Titan in ultraviolet and infrared wavelengths taken by Cassini’s imaging science subsystem on 26 October. Red and green colours show areas where atmospheric methane absorbs light and reveal a brighter (redder) northern hemisphere. Blue colours show the high atmosphere and detached hazes (Courtesy of JPL /Univ. of Arizona) Cassini-Huygens Jean-Pierre Lebreton1, Claudio Sollazzo2, Thierry Blancquaert13, Olivier Witasse1 and the Huygens Mission Team 1 ESA Directorate of Scientific Programmes, ESTEC, Noordwijk, The Netherlands 2 ESA Directorate of Operations and Infrastructure, ESOC, Darmstadt, Germany 3 ESA Directorate of Technical and Quality Management, ESTEC, Noordwijk, The Netherlands Earl Maize, Dennis Matson, Robert Mitchell, Linda Spilker Jet Propulsion Laboratory (NASA/JPL), Pasadena, California Enrico Flamini Italian Space Agency (ASI), Rome, Italy Monica Talevi Science Programme Communication Service, ESA Directorate of Scientific Programmes, ESTEC, Noordwijk, The Netherlands assini-Huygens, named after the two celebrated scientists, is the joint NASA/ESA/ASI mission to Saturn Cand its giant moon Titan. It is designed to shed light on many of the unsolved mysteries arising from previous observations and to pursue the detailed exploration of the gas giants after Galileo’s successful mission at Jupiter. The exploration of the Saturnian planetary system, the most complex in our Solar System, will help us to make significant progress in our understanding -
On the Detection of Exomoons in Photometric Time Series
On the Detection of Exomoons in Photometric Time Series Dissertation zur Erlangung des mathematisch-naturwissenschaftlichen Doktorgrades “Doctor rerum naturalium” der Georg-August-Universität Göttingen im Promotionsprogramm PROPHYS der Georg-August University School of Science (GAUSS) vorgelegt von Kai Oliver Rodenbeck aus Göttingen, Deutschland Göttingen, 2019 Betreuungsausschuss Prof. Dr. Laurent Gizon Max-Planck-Institut für Sonnensystemforschung, Göttingen, Deutschland und Institut für Astrophysik, Georg-August-Universität, Göttingen, Deutschland Prof. Dr. Stefan Dreizler Institut für Astrophysik, Georg-August-Universität, Göttingen, Deutschland Dr. Warrick H. Ball School of Physics and Astronomy, University of Birmingham, UK vormals Institut für Astrophysik, Georg-August-Universität, Göttingen, Deutschland Mitglieder der Prüfungskommision Referent: Prof. Dr. Laurent Gizon Max-Planck-Institut für Sonnensystemforschung, Göttingen, Deutschland und Institut für Astrophysik, Georg-August-Universität, Göttingen, Deutschland Korreferent: Prof. Dr. Stefan Dreizler Institut für Astrophysik, Georg-August-Universität, Göttingen, Deutschland Weitere Mitglieder der Prüfungskommission: Prof. Dr. Ulrich Christensen Max-Planck-Institut für Sonnensystemforschung, Göttingen, Deutschland Dr.ir. Saskia Hekker Max-Planck-Institut für Sonnensystemforschung, Göttingen, Deutschland Dr. René Heller Max-Planck-Institut für Sonnensystemforschung, Göttingen, Deutschland Prof. Dr. Wolfram Kollatschny Institut für Astrophysik, Georg-August-Universität, Göttingen,