Secrets from Titan's Seas
Total Page:16
File Type:pdf, Size:1020Kb
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. -
Titan North Pole
. Melrhir Lacuna . Ngami Lacuna . Cardiel Lacus . Jerid Lacuna . Racetrack Lacuna . Uyuni Lacuna Vänern Freeman. Lanao . Lacus . Atacama Lacuna Lacus Lacus . Sevan Lacus Ohrid . Cayuga Lacus .Albano Lacus Lacus Logtak . .Junín Lacus . Lacus . Mweru Lacus . Prespa Lacus Eyre . Taupo Lacus . Van Lacus en Lacuna Suwa Lacus m Ypoa Lacus. lu . F Rukwa Lacus Winnipeg . Atitlán Lacus . Viedma Lacus . Rannoch Lacus Ihotry Lacus Lacus n .Phewa Lacus . o h . Chilwa Lacus i G Patos Maracaibo Lacus . Oneida Lacus Rombaken . Sinus Muzhwi Lacus Negra Lacus . Mývatn Lacus Sinus . Buada Lacus. Uvs Lacus Lagdo Lacus . Annecy Lacus . Dilolo Lacus Towada Lacus Dridzis Lacus . Vid Flumina Imogene Lacus . Arala Lacus Yessey Lacus Woytchugga Lacuna . Toba Lacus . .Olomega Lacus Zaza Lacus . Roca Lacus Müggel Buyan . Waikare Lacus . Insula Nicoya Rwegura Lacus . Quilotoa Lacus . Lacus . Tengiz Lacus Bralgu Ligeia Planctae Insulae Sinus Insulae Zub Lacus . Grasmere Lacus Puget XanthusSinus Flumen Hlawga Lacus . Mare Kokytos Flumina . Kutch Lacuna Mackay S Lithui Montes . a m Kivu Lacus Ginaz T Nakuru Lacuna Lacus Fogo Lacus . r . b e a tio v Niushe n i F Labyrinthus Wakasa z lum e i Letas Lacus na Sinus . Balaton Lacus Layrinthus F r e t u m . Karakul Lacus Ipyr Labyrinthus a Flu Xolotlán ay m . noh u en . a Lacus Sparrow Lacus p Moray A Okahu .Akema Lacus Sinus Sinus Trichonida .Brienz Lacus Meropis Insula . Lacus Qinghai Hawaiki . Insulae Onogoro Lacus Punga Insula Fundy Sinus Tumaco Synevyr Sinus . Mare Fagaloa Lacus Sinus Tunu s Saldanha u Sinus n Sinus i S a h c a v Trold Yojoa A . Lacus Neagh Kraken MareSinus Feia s Lacus u in Mayda S Lacus Insula Dingle Sinus Gamont Gen a Gabes Sinus . -
Appendix 1: Venus Missions
Appendix 1: Venus Missions Sputnik 7 (USSR) Launch 02/04/1961 First attempted Venus atmosphere craft; upper stage failed to leave Earth orbit Venera 1 (USSR) Launch 02/12/1961 First attempted flyby; contact lost en route Mariner 1 (US) Launch 07/22/1961 Attempted flyby; launch failure Sputnik 19 (USSR) Launch 08/25/1962 Attempted flyby, stranded in Earth orbit Mariner 2 (US) Launch 08/27/1962 First successful Venus flyby Sputnik 20 (USSR) Launch 09/01/1962 Attempted flyby, upper stage failure Sputnik 21 (USSR) Launch 09/12/1962 Attempted flyby, upper stage failure Cosmos 21 (USSR) Launch 11/11/1963 Possible Venera engineering test flight or attempted flyby Venera 1964A (USSR) Launch 02/19/1964 Attempted flyby, launch failure Venera 1964B (USSR) Launch 03/01/1964 Attempted flyby, launch failure Cosmos 27 (USSR) Launch 03/27/1964 Attempted flyby, upper stage failure Zond 1 (USSR) Launch 04/02/1964 Venus flyby, contact lost May 14; flyby July 14 Venera 2 (USSR) Launch 11/12/1965 Venus flyby, contact lost en route Venera 3 (USSR) Launch 11/16/1965 Venus lander, contact lost en route, first Venus impact March 1, 1966 Cosmos 96 (USSR) Launch 11/23/1965 Possible attempted landing, craft fragmented in Earth orbit Venera 1965A (USSR) Launch 11/23/1965 Flyby attempt (launch failure) Venera 4 (USSR) Launch 06/12/1967 Successful atmospheric probe, arrived at Venus 10/18/1967 Mariner 5 (US) Launch 06/14/1967 Successful flyby 10/19/1967 Cosmos 167 (USSR) Launch 06/17/1967 Attempted atmospheric probe, stranded in Earth orbit Venera 5 (USSR) Launch 01/05/1969 Returned atmospheric data for 53 min on 05/16/1969 M. -
Comparative Saturn-Versus-Jupiter Tether Operation
Journal of Geophysical Research: Space Physics Comparative Saturn-Versus-Jupiter Tether Operation J. R. Sanmartin1 ©, J. Pelaez1 ©, and I. Carrera-Calvo1 Abstract Saturn, Uranus, and Neptune, among the four Giant Outer planets, have magnetic field B about 20 times weaker than Jupiter. This could suggest, in principle, that planetary capture and operation using tethers, which involve B effects twice, might be much less effective at Saturn, in particular, than at Jupiter. It was recently found, however, that the very high Jovian B itself strongly limits conditions for tether use, maximum captured spacecraft-to-tether mass ratio only reaching to about 3.5. Further, it is here shown that planetary parameters and low magnetic field might make tether operation at Saturn more effective than at Jupiter. Operation analysis involves electron plasma density in a limited radial range, about 1-1.5 times Saturn radius, and is weakly requiring as regards density modeling. 1. Introduction All Giant Outer planets have magnetic field B and corotating plasma, allowing nonconventional exploration. Electrodynamic tethers, which are thermodynamic (dissipative) in character, can 1. provide propellantless drag both for deorbiting spacecraft in Low Earth Orbit at end of mission and for planetary spacecraft capture and operation down the gravitational well, and 2. generate accompanying, useful electrical power, or store it to later invert tether current (Sanmartin et al., 1993; Sanmartin & Estes, 1999). At Jupiter, tethers could be effective because its field B is high (Sanmartin et al., 2008). Tethers would allow a variety of science applications (Sanchez-Torres & Sanmartin, 2011). The Saturn field is 20 times smaller, however, and tether operation involves field B twice, which makes that thermodynamic character manifest: 1. -
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. -
(Preprint) AAS 18-416 PRELIMINARY INTERPLANETARY MISSION
(Preprint) AAS 18-416 PRELIMINARY INTERPLANETARY MISSION DESIGN AND NAVIGATION FOR THE DRAGONFLY NEW FRONTIERS MISSION CONCEPT Christopher J. Scott,∗ Martin T. Ozimek,∗ Douglas S. Adams,y Ralph D. Lorenz,z Shyam Bhaskaran,x Rodica Ionasescu,{ Mark Jesick,{ and Frank E. Laipert{ Dragonfly is one of two mission concepts selected in December 2017 to advance into Phase A of NASA’s New Frontiers competition. Dragonfly would address the Ocean Worlds mis- sion theme by investigating Titan’s habitability and prebiotic chemistry and searching for evidence of chemical biosignatures of past (or extant) life. A rotorcraft lander, Dragonfly would capitalize on Titan’s dense atmosphere to enable mobility and sample materials from a variety of geologic settings. This paper describes Dragonfly’s baseline mission design giv- ing a complete picture of the inherent tradespace and outlines the design process from launch to atmospheric entry. INTRODUCTION Hosting the moons Titan and Enceladus, the Saturnian system contains at least two unique destinations that have been classified as ocean worlds. Titan, the second largest moon in the solar system behind Ganymede and the only planetary satellite with a significant atmosphere, is larger than the planet Mercury at 5,150 km (3,200 miles) in diameter. Its atmosphere, approximately 10 times the column mass of Earth’s, is composed of 95% nitrogen, 5% methane, 0.1% hydrogen along with trace amounts of organics.1 Titan’s atmosphere may resemble that of the Earth before biological processes began modifying its composition. Similar to the hydrological cycle on Earth, Titan’s methane evaporates into clouds, rains, and flows over the surface to fill lakes and seas, and subsequently evaporates back into the atmosphere. -
Outer Planets Assessment Group (OPAG) View of Decadal Survey
Outer Solar System: Many Worlds to Explore Outer Planets Assessment Group (OPAG) View of Decadal Survey Progress May 2017 Alfred McEwen, OPAG Chair LPL, University of Arizona This presentation will address (relevant to OPAG): • 1. Most important new discoveries 2011-2017 – (V&V writing was completed in late 2010) • 2. Progress made in implementing Decadal advice – Flight investigations • Flagship Missions • New Frontiers – R&A and infrastructure – Technology • 3. Other issues relevant to the committee’s statement of task – Smallsats for Outer Planet Exploration – How to make the Discovery Program useful for Outer Planets – Europa Lander – Coordination with ESA JUICE mission – Adding Ocean Worlds to New Frontiers 4 – Future mission studies to prepare for next Decadal • 4. Summary grade recommendations on Decadal progress • 5. OPAG top recommendations to mid-term review 1. Most Important New Discoveries 2011-present • Jupiter system: – Europa plate tectonics (Prockter et al., 2014) – Europa cryovolcanism (Quick et al., 2017; Prockter et al., 2017) – Europa plumes (Roth et al., 2014; Sparks et al., 2017) – Confirmation of subsurface ocean in Ganymede (Saur et al., 2015) – Evidence for extensive melt in Io’s mantle (Khurana et al., 2011; Tyler et al., 2015) – Fabulous results from Juno (papers submitted) • Saturn System: – MUCH from Cassini—see upcoming slides • Uranus and Neptune systems: – Standard interior models do not fit observations; Uranus and Neptune may be quite different (Nettelmann et al. 2013) – Intense auroras seen at Uranus (Lamy et al., 2012, 2017) – Weather on Uranus and Neptune confined to a “thin” layer (<1,000 km) (Kaspi et al. 2013) – Ice Giant growing around nearby TW Hydra (Rapson et al., 2015) – Triton’s tidal heating and possible subsurface ocean (Gaeman et al., 2012; Nimmo and Spencer, 2015) • Pluto system—lots of results from New Horizons – The Pluto system is complex in the variety of its landscapes, activity, and range of surface ages. -
No Slide Title
Planetary Protection Planetary Protection at NASA: Overview and Status Catharine A. Conley, NASA Planetary Protection Officer 1 May, 2012 2012 NASA Planetary Science Goals Planetary Protection Goal 2: Expand scientific understanding of the Earth and the universe in which we live. 2.3 Ascertain the content, origin, and evolution of the solar system and the potential for life elsewhere. 2.3.1 Inventory solar system objects and identify the processes active in and among them. 2.3.2 Improve understanding of how the Sun's family of planets, satellites, and minor bodies originated and evolved. 2.3.3 Improve understanding of the processes that determine the history and future of habitability of environments on Mars and other solar system bodies. 2.3.4 Improve understanding of the origin and evolution of Earth's life and biosphere to determine if there is or ever has been life elsewhere in the universe. 2.3.5 Identify and characterize small bodies and the properties of planetary environments that pose a threat to terrestrial life or exploration or provide potentially exploitable resources. NASA Planetary Protection Policy Planetary Protection • The policy and its implementation requirements are embodied in NPD 8020.7G (NASA Administrator) – Planetary Protection Officer acts on behalf of the Aassociate Administrator for Science to maintain and enforce the policy – NASA obtains recommendations on planetary protection issues (requirements for specific bodies and mission types) from the National Research Council’s Space Studies Board – Advice on -
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 -
The Science Case for a Titan Flagship-Class Orbiter with Probes (White Paper for the NRC Decadal Survey for Planetary Science and Astrobiology) Conor A
The Science Case for a Titan Flagship-class Orbiter with Probes (White paper for the NRC Decadal Survey for Planetary Science and Astrobiology) Conor A. Nixon, James Abshire, Andrew Ashton, Jason W. Barnes, Nathalie Carrasco, Mathieu Choukroun, Athena Coustenis, Louis-Alexandre Couston, Niklas Edberg, Alexander Gagnon, et al. To cite this version: Conor A. Nixon, James Abshire, Andrew Ashton, Jason W. Barnes, Nathalie Carrasco, et al.. The Science Case for a Titan Flagship-class Orbiter with Probes (White paper for the NRC Decadal Survey for Planetary Science and Astrobiology). 2020. hal-03085250 HAL Id: hal-03085250 https://hal.archives-ouvertes.fr/hal-03085250 Preprint submitted on 21 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. The Science Case for a Titan Flagship-class Orbiter with Probes Authors: Conor A. Nixon, NASA Goddard Space Flight Center, USA Planetary Systems Laboratory, 8800 Greenbelt Road, Greenbelt, MD 20771 (301) 286-6757 [email protected] James Abshire, University oF Maryland, USA Andrew Ashton, Woods Hole Oceanographic Institution, USA Jason W. Barnes, University oF Idaho, USA Nathalie Carrasco, Université Paris-Saclay, France, Mathieu Choukroun, Jet Propulsion Laboratory, Caltech, USA Athena Coustenis, Paris Observatory, CNRS, PSL, France Louis-Alexandre Couston, British Antarctic Survey, UK Niklas Edberg, Swedish Institute oF Space Physics, Sweden Alexander Gagnon, University oF Washington, USA Jason D. -
Titan Mare Explorer (TIME): the First Exploration of an Extraterrestrial Sea
Titan Mare Explorer (TIME): The First Exploration of an Extraterrestrial Sea Fact Sheet: Page 1 of 2 Science Objectives and Anticipated Payload . Determine the chemistry of a Titan lake to constrain Titan’s methane cycle. Instrument: Mass Spectrometer 1 . Determine the depth of a Titan lake. Instrument: Sonar 2 . Characterize physical properties of lake liquids. Instrument: Physical Properties Package 3a . Determine how the local meteorology over the lakes ties to the global cycling of methane. Instrument: Meteorology Package 3b . Analyze the morphology of lake surfaces, and if possible, shorelines, in order to constrain the kinetics of lake liquids and better understand the origin and evolution of Titan lakes. Instrument: Descent 4 and Surface 5 Imagers Focused, high-priority Discovery Science 5 Lake Lander Mission Objectives 3b . First exploration of planetary sea beyond Earth . Flight demonstration of ASRG in two Liquid environments: deep space and non- Level terrestrial atmosphere 4 . Pioneer low-cost, outer planet 1 missions 3a 2 Relevance and Importance to NASA Planetary Objectives and the Decadal Survey Decadal Survey – Volatiles and Organics, The Stuff of Life . Directly measure the organic constituents on another planetary object Decadal Survey – Processes: How Planetary Systems Work . First active measurement of liquid cycle beyond Earth Direct Successor to Revolutionary Cassini Discoveries Titan Mare Explorer (TIME): The First Exploration of an Extraterrestrial Sea Fact Sheet: Page 2 of 2 Major Mission Characteristics 1. Launch: 21 day window opens 17 January 2015 using an Atlas 411. 2. Cruise: One DSM, one Earth flyby en route to Saturn. 3. Titan Entry: Cruise stage separates from lander shortly before Titan entry on 29 June 2022. -
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.