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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]. -
Callisto: a Guide to the Origin of the Jupiter System
A PAPER SUBMITTED TO THE DECADAL SURVEY ON PLANETARY SCIENCE AND ASTROBIOLOGY Callisto: A Guide to the Origin of the Jupiter System David E Smith 617-803-3377 Department of Earth, Atmospheric and PLanetary Sciences Massachusetts Institute of Technology, Cambridge MA 02139 [email protected] Co-authors: Francis Nimmo, UCSC, [email protected] Krishan Khurana, UCLA, [email protected] Catherine L. Johnson, PSI, [email protected] Mark Wieczorek, OCA, Fr, [email protected] Maria T. Zuber, MIT, [email protected] Carol Paty, University of Oregon, [email protected] Antonio Genova, Univ Rome, It, [email protected] Erwan Mazarico, NASA GSFC, [email protected] Louise Prockter, LPI, [email protected] Gregory A. Neumann, NASA GSFC Emeritus, [email protected] John E. Connerney, Adnet Systems Inc., [email protected] Edward B. Bierhaus, LMCO, [email protected] Sander J. Goossens, UMBC, [email protected] MichaeL K. Barker, NASA GSFC, [email protected] Peter B. James, Baylor, [email protected] James Head, Brown, [email protected] Jason Soderblom, MIT, [email protected] July 14, 2020 Introduction Among the GaLiLean moons of Jupiter, it is outermost CaLListo that appears to most fulLy preserve the record of its ancient past. With a surface aLmost devoid of signs of internaL geologic activity, and hints from spacecraft data that its interior has an ocean whiLe being only partiaLLy differentiated, CaLListo is the most paradoxicaL of the giant rock-ice worlds. How can a body with such a primordiaL surface harbor an ocean? If the interior was warm enough to form an ocean, how could a mixed rock and ice interior remain stable? What do the striking differences between geologicaLLy unmodified CaLListo and its sibling moon Ganymede teLL us about the formation of the GaLiLean moons and the primordiaL conditions at the time of the formation of CaLListo and the accretion of giant planet systems? The answers can be provided by a CaLListo orbitaL mission. -
Saturn — from the Outside In
Saturn — From the Outside In Saturn — From the Outside In Questions, Answers, and Cool Things to Think About Discovering Saturn:The Real Lord of the Rings Saturn — From the Outside In Although no one has ever traveled ing from Saturn’s interior. As gases in from Saturn’s atmosphere to its core, Saturn’s interior warm up, they rise scientists do have an understanding until they reach a level where the tem- of what’s there, based on their knowl- perature is cold enough to freeze them edge of natural forces, chemistry, and into particles of solid ice. Icy ammonia mathematical models. If you were able forms the outermost layer of clouds, to go deep into Saturn, here’s what you which look yellow because ammonia re- trapped in the ammonia ice particles, First, you would enter Saturn’s up- add shades of brown and other col- per atmosphere, which has super-fast ors to the clouds. Methane and water winds. In fact, winds near Saturn’s freeze at higher temperatures, so they equator (the fat middle) can reach turn to ice farther down, below the am- speeds of 1,100 miles per hour. That is monia clouds. Hydrogen and helium rise almost four times as fast as the fast- even higher than the ammonia without est hurricane winds on Earth! These freezing at all. They remain gases above winds get their energy from heat ris- the cloud tops. Saturn — From the Outside In Warm gases are continually rising in Earth’s Layers Saturn’s atmosphere, while icy particles are continually falling back down to the lower depths, where they warm up, turn to gas and rise again. -
Dwarf Planet Ceres
Dwarf Planet Ceres drishtiias.com/printpdf/dwarf-planet-ceres Why in News As per the data collected by NASA’s Dawn spacecraft, dwarf planet Ceres reportedly has salty water underground. Dawn (2007-18) was a mission to the two most massive bodies in the main asteroid belt - Vesta and Ceres. Key Points 1/3 Latest Findings: The scientists have given Ceres the status of an “ocean world” as it has a big reservoir of salty water underneath its frigid surface. This has led to an increased interest of scientists that the dwarf planet was maybe habitable or has the potential to be. Ocean Worlds is a term for ‘Water in the Solar System and Beyond’. The salty water originated in a brine reservoir spread hundreds of miles and about 40 km beneath the surface of the Ceres. Further, there is an evidence that Ceres remains geologically active with cryovolcanism - volcanoes oozing icy material. Instead of molten rock, cryovolcanoes or salty-mud volcanoes release frigid, salty water sometimes mixed with mud. Subsurface Oceans on other Celestial Bodies: Jupiter’s moon Europa, Saturn’s moon Enceladus, Neptune’s moon Triton, and the dwarf planet Pluto. This provides scientists a means to understand the history of the solar system. Ceres: It is the largest object in the asteroid belt between Mars and Jupiter. It was the first member of the asteroid belt to be discovered when Giuseppe Piazzi spotted it in 1801. It is the only dwarf planet located in the inner solar system (includes planets Mercury, Venus, Earth and Mars). Scientists classified it as a dwarf planet in 2006. -
Titan and the Moons of Saturn Telesto Titan
The Icy Moons and the Extended Habitable Zone Europa Interior Models Other Types of Habitable Zones Water requires heat and pressure to remain stable as a liquid Extended Habitable Zones • You do not need sunlight. • You do need liquid water • You do need an energy source. Saturn and its Satellites • Saturn is nearly twice as far from the Sun as Jupiter • Saturn gets ~30% of Jupiter’s sunlight: It is commensurately colder Prometheus • Saturn has 82 known satellites (plus the rings) • 7 major • 27 regular • 4 Trojan • 55 irregular • Others in rings Titan • Titan is nearly as large as Ganymede Titan and the Moons of Saturn Telesto Titan Prometheus Dione Titan Janus Pandora Enceladus Mimas Rhea Pan • . • . Titan The second-largest moon in the Solar System The only moon with a substantial atmosphere 90% N2 + CH4, Ar, C2H6, C3H8, C2H2, HCN, CO2 Equilibrium Temperatures 2 1/4 Recall that TEQ ~ (L*/d ) Planet Distance (au) TEQ (K) Mercury 0.38 400 Venus 0.72 291 Earth 1.00 247 Mars 1.52 200 Jupiter 5.20 108 Saturn 9.53 80 Uranus 19.2 56 Neptune 30.1 45 The Atmosphere of Titan Pressure: 1.5 bars Temperature: 95 K Condensation sequence: • Jovian Moons: H2O ice • Saturnian Moons: NH3, CH4 2NH3 + sunlight è N2 + 3H2 CH4 + sunlight è CH, CH2 Implications of Methane Free CH4 requires replenishment • Liquid methane on the surface? Hazy atmosphere/clouds may suggest methane/ ethane precipitation. The freezing points of CH4 and C2H6 are 91 and 92K, respectively. (Titan has a mean temperature of 95K) (Liquid natural gas anyone?) This atmosphere may resemble the primordial terrestrial atmosphere. -
Enceladus, Moon of Saturn
National Aeronautics and and Space Space Administration Administration Enceladus, Moon of Saturn www.nasa.gov Enceladus (pronounced en-SELL-ah-dus) is an icy moon of Saturn with remarkable activity near its south pole. Covered in water ice that reflects sunlight like freshly fallen snow, Enceladus reflects almost 100 percent of the sunlight that strikes it. Because the moon reflects so much sunlight, the surface temperature is extremely cold, about –330 degrees F (–201 degrees C). The surface of Enceladus displays fissures, plains, corrugated terrain and a variety of other features. Enceladus may be heated by a tidal mechanism similar to that which provides the heat for volca- An artist’s concept of Saturn’s rings and some of the icy moons. The ring particles are composed primarily of water ice and range in size from microns to tens of meters. In 2004, the Cassini spacecraft passed through the gap between the F and G rings to begin orbiting Saturn. noes on Jupiter’s moon Io. A dramatic plume of jets sprays water ice and gas out from the interior at ring material, coating itself continually in a mantle Space Agency. The Jet Propulsion Laboratory, a many locations along the famed “tiger stripes” at of fresh, white ice. division of the California Institute of Technology, the south pole. Cassini mission data have provided manages the mission for NASA. evidence for at least 100 distinct geysers erupting Saturn’s Rings For images and information about the Cassini on Enceladus. All of this activity, plus clues hidden Saturn’s rings form an enormous, complex struc- mission, visit — http://saturn.jpl.nasa.gov/ in the moon’s gravity, indicates that the moon’s ture. -
The Solar System Cause Impact Craters
ASTRONOMY 161 Introduction to Solar System Astronomy Class 12 Solar System Survey Monday, February 5 Key Concepts (1) The terrestrial planets are made primarily of rock and metal. (2) The Jovian planets are made primarily of hydrogen and helium. (3) Moons (a.k.a. satellites) orbit the planets; some moons are large. (4) Asteroids, meteoroids, comets, and Kuiper Belt objects orbit the Sun. (5) Collision between objects in the Solar System cause impact craters. Family portrait of the Solar System: Mercury, Venus, Earth, Mars, Jupiter, Saturn, Uranus, Neptune, (Eris, Ceres, Pluto): My Very Excellent Mother Just Served Us Nine (Extra Cheese Pizzas). The Solar System: List of Ingredients Ingredient Percent of total mass Sun 99.8% Jupiter 0.1% other planets 0.05% everything else 0.05% The Sun dominates the Solar System Jupiter dominates the planets Object Mass Object Mass 1) Sun 330,000 2) Jupiter 320 10) Ganymede 0.025 3) Saturn 95 11) Titan 0.023 4) Neptune 17 12) Callisto 0.018 5) Uranus 15 13) Io 0.015 6) Earth 1.0 14) Moon 0.012 7) Venus 0.82 15) Europa 0.008 8) Mars 0.11 16) Triton 0.004 9) Mercury 0.055 17) Pluto 0.002 A few words about the Sun. The Sun is a large sphere of gas (mostly H, He – hydrogen and helium). The Sun shines because it is hot (T = 5,800 K). The Sun remains hot because it is powered by fusion of hydrogen to helium (H-bomb). (1) The terrestrial planets are made primarily of rock and metal. -
Final Report of the Opgt/Mjs Plasma Wave Science Team
1 September 1972 FINAL REPORT OF THE OPGT/MJS PLASMA WAVE SCIENCE TEAM Prepared by F. L. Scarf, Team Leader for National Aeronautical and Space Administration Washington, D.C. 205*t6 Contract NASW 2228 Space Sciences Department TRW Systems Group One Space Park Redondo Beach, California 902?8 4 Page 1 1. TEAM ORGANIZATION AND MEMBERSHIP The Plasma Wave Team Leader is Dr. F. L. Scarf of TRW Systems, and the official team members are Dr. D. A. Gurnett (University of Iowa), Dr. R. A. Helliwell (Stanford University), Dr. R. E. Holzer (UCLA), Dr. P. J. Kellogg (University of Minnesota), Dr. E. J. Smith (JPL), and Dr. E. Ungstrup (Danish Space Research Institute). Mr. A. M. A. Frandsen of JPL serves as Team Member and Experiment Representative. In addition, the Plasma Wave Team solicited the continuing support and assistance of several other outstanding scientists, and we have designated these participants as Team Associates; the Associates are Dr. N. M. Brice (Cornell University), Dr. D. Cartwright (University of Minnesota), Dr. R. W. Fredricks (TRW), Dr. H. B. Liemohn (Boeing), Dr. C. F. Kennel (UCLA), and Dr. R. Thome (UCLA) . 2. GENERAL TEAM ACTIVITIES FEBRUARY 1972-AUGUST 31, 1972 (See the mid-year report for a summary of the earlier work) During this period Dr. Scarf attended all SSG Meetings except the last one, where Dr. E. J. Smith represented the Plasma Wave Team. There were a number of Team Meetings and several additional .conferences at JPL concerning EMI and other potential spacecraft problems. The major development during this interval involved the decision not to go ahead with the Grand Tour. -
THE PENNY MOON and QUARTER EARTH School Adapted from a Physics Forum Activity At
~ LPI EDUCATION/PUBLIC OUTREACH SCIENCE ACTIVITIES ~ Ages: 5th grade – high THE PENNY MOON AND QUARTER EARTH school Adapted from a Physics Forum activity at: http://www.phvsicsforums.com/ Duration: 10 minutes OVERVIEW — The students will use a penny and a quarter to model the Moon’s rotation on its axis and Materials: revolution around the Earth, and demonstrate that the Moon keeps the same face toward One penny and one the Earth. quarter per pair of students OBJECTIVE — Overhead projector, or The students will: elmo, or video Demonstrate the motion of the Moon’s rotation and revolution. projector Compare what we would see of the Moon if it did not rotate to what we see when its period of rotation is the same as its orbital period. Projected image of student overhead BEFORE YOU START: Do not introduce this topic along with the reason for lunar phases; students may become confused and assume that the Moon’s rotation is related to its phases. Prepare to show the student overhead projected for the class to see. ACTIVITY — 1. Ask your students to describe which parts of the Moon they see. Does the Moon turn? Can we see its far side? Allow time for your students to discuss this and share their opinions. 2. Hand out the pennies and quarters so that each pair of students has both. Tell the students that they will be creating a model of the Earth and Moon. Which object is Earth? [the quarter] Which one is the Moon? [the penny] 3. Turn on the projected student overhead. -
The Sun's Dynamic Atmosphere
Lecture 16 The Sun’s Dynamic Atmosphere Jiong Qiu, MSU Physics Department Guiding Questions 1. What is the temperature and density structure of the Sun’s atmosphere? Does the atmosphere cool off farther away from the Sun’s center? 2. What intrinsic properties of the Sun are reflected in the photospheric observations of limb darkening and granulation? 3. What are major observational signatures in the dynamic chromosphere? 4. What might cause the heating of the upper atmosphere? Can Sound waves heat the upper atmosphere of the Sun? 5. Where does the solar wind come from? 15.1 Introduction The Sun’s atmosphere is composed of three major layers, the photosphere, chromosphere, and corona. The different layers have different temperatures, densities, and distinctive features, and are observed at different wavelengths. Structure of the Sun 15.2 Photosphere The photosphere is the thin (~500 km) bottom layer in the Sun’s atmosphere, where the atmosphere is optically thin, so that photons make their way out and travel unimpeded. Ex.1: the mean free path of photons in the photosphere and the radiative zone. The photosphere is seen in visible light continuum (so- called white light). Observable features on the photosphere include: • Limb darkening: from the disk center to the limb, the brightness fades. • Sun spots: dark areas of magnetic field concentration in low-mid latitudes. • Granulation: convection cells appearing as light patches divided by dark boundaries. Q: does the full moon exhibit limb darkening? Limb Darkening: limb darkening phenomenon indicates that temperature decreases with altitude in the photosphere. Modeling the limb darkening profile tells us the structure of the stellar atmosphere. -
Our Atmosphere Greece Sicily Athens
National Aeronautics and Space Administration Sardinia Italy Turkey Our Atmosphere Greece Sicily Athens he atmosphere is a life-giving blanket of air that surrounds our Crete T Tunisia Earth; it is composed of gases that protect us from the Sun’s intense ultraviolet Gulf of Gables radiation, allowing life to flourish. Greenhouse gases like carbon dioxide, Mediterranean Sea ozone, and methane are steadily increasing from year to year. These gases trap infrared radiation (heat) emitted from Earth’s surface and atmosphere, Gulf of causing the atmosphere to warm. Conversely, clouds as well as many tiny Sidra suspended liquid or solid particles in the air such as dust, smoke, and Egypt Libya pollution—called aerosols—reflect the Sun’s radiative energy, which leads N to cooling. This delicate balance of incoming and reflected solar radiation 200 km and emitted infrared energy is critical in maintaining the Earth’s climate Turkey Greece and sustaining life. Research using computer models and satellite data from NASA’s Earth Sicily Observing System enhances our understanding of the physical processes Athens affecting trends in temperature, humidity, clouds, and aerosols and helps us assess the impact of a changing atmosphere on the global climate. Crete Tunisia Gulf of Gables Mediterranean Sea September 17, 1979 Gulf of Sidra October 6, 1986 September 20, 1993 Egypt Libya September 10, 2000 Aerosol Index low high September 24, 2006 On August 26, 2007, wildfires in southern Greece stretched along the southwest coast of the Peloponnese producing Total Ozone (Dobson Units) plumes of smoke that drifted across the Mediterranean Sea as far as Libya along Africa’s north coast. -
Jacques Tiziou Space Collection
Jacques Tiziou Space Collection Isaac Middleton and Melissa A. N. Keiser 2019 National Air and Space Museum Archives 14390 Air & Space Museum Parkway Chantilly, VA 20151 [email protected] https://airandspace.si.edu/archives Table of Contents Collection Overview ........................................................................................................ 1 Administrative Information .............................................................................................. 1 Biographical / Historical.................................................................................................... 1 Scope and Contents........................................................................................................ 2 Arrangement..................................................................................................................... 2 Names and Subjects ...................................................................................................... 2 Container Listing ............................................................................................................. 4 Series : Files, (bulk 1960-2011)............................................................................... 4 Series : Photography, (bulk 1960-2011)................................................................. 25 Jacques Tiziou Space Collection NASM.2018.0078 Collection Overview Repository: National Air and Space Museum Archives Title: Jacques Tiziou Space Collection Identifier: NASM.2018.0078 Date: (bulk 1960s through