Voyage to Europa!

Total Page:16

File Type:pdf, Size:1020Kb

Voyage to Europa! Voyage to Europa! 1. Introduction: Is there life on one of Jupiter's moons? The Setting The Challenge Heads Up! 2. Activities: Getting the Images Imaging Jupiter and it's Moons Scope it Out Reflecting on your Images Which moon is Europa? Using the Images to Investigate Jupiter and Europa Preparing for the Trip: How far is Jupiter? Go Figure A Base Camp on Jupiter? What is the scale of my image? How large is Jupiter? How large is Europa? How much does Jupiter weigh? How dense is Jupiter? How strong is Jupiter's gravity? Mission assessment: Jupiter as a base camp? Search for Life on Europa What is Europa Like? Does Europa have an Atmosphere? What is Europa's Environment? Can We Communice to Earth from Europa? Artificial Gravity? Try this/Tabletop Experiment: Mysterious motion experiment An Ocean on Europa? Try this/Tabletop Experiment: Cooool Heat! Did you know/fun fact: whales Is there Life at the extremes? 3. Wrap-Up & Reference: Data Page Briefing Room Timeline Ideas you'll need From the Ground Up!: Jupiter v. 031301 -1- Harvard-Smithsonian Center for Astrophysics VOYAGE TO EUROPA 1. INTRODUCTION: Is there life on one of Jupiter's moons? Circling the giant planet, Jupiter, are several moons that may contain liquid water. One of those moons Ñ named Europa Ñ may even be covered by a vast ocean. In fact, according to recent evidence from a NASA space probe to Jupiter, this salt-water ocean may be 60 miles deep and as warm as the waters of Bermuda! If true, this would make Europa the likeliest place in our solar system to search for extra- terrestrial life. The problem: Europa's ocean is hidden under a thick layer of ice. THE CHALLENGE: You and your firm, Investigation Inc., have been asked by NASA to report on the prospects for sending an expedition to search for life beneath Europa's frozen surface. NASA will provide the spacecraft to get your crew to Jupiter, and will develop any technologies you may need. Your challenge is to: • Obtain images of the planet Jupiter and its four brightest moons, and identify your destination, Europa. • Evaluate the prospects for setting up a base camp on Jupiter. Use your images Ñ and your knowledge of physics Ñ to find out as much as you can about Jupiter. If you tried to land on Jupiter, would you hit a solid surface, or would you keep on falling and never be heard from again? If you could land on Jupiter, how much would you weigh? Would your body be able to support you? Would you be able to take off again? From the Ground Up!: Jupiter v. 031301 -2- Harvard-Smithsonian Center for Astrophysics • Evaluate the prospects for a base camp on Europa: Do you expect Europa to have an atmosphere? How much sunlight does Europa get compared to Earth? If you can only explore the surface while the sun is up, how long can you explore before you must get back to base camp? How cold do you expect it to be? How much will you weigh there, compared to Earth? • Evaluate the prospects for life under Europa's icy surface: The ocean on Europa could contain bizarre life forms Ñ or it could contain no life at all. Make a case for the likelihood of finding life on Europa. Consider these questions: Does life need an energy source Ñ and if so, what kinds of energy will do? Does life need light to exist? Does life need oxygen? In discussing these questions, you may wish to research and report on one or more of the following: -What kind of life lives near deep-sea volcanic vents on Earth? -What are the most extreme conditions on Earth, and what kinds of living things thrive under those conditions? This mission guide will take you step by step through the activities you'll need for your report. HEADS UP! Next time you find yourself under the stars, look for the planet Jupiter. When it's above the horizon, Jupiter is easy to spot, even in the city, because it often appears brighter than even the brightest stars. If the other planets or the Moon are also visible, you'll see that they all lie along a nearly straight path across the sky. If extended below the horizon, this line would also pass through the Sun. That's because the Sun, planets and their moons lie in nearly the same plane. When seen from a point within that plane, they appear to lie along a line. Try this dizzying feat: Look up at the sky and picture the plane that the planets lie in. You'll suddenly become aware that you're standing at an angle to that plane. When it comes to outer space, which direction is "up"?! From the Ground Up!: Jupiter v. 031301 -3- Harvard-Smithsonian Center for Astrophysics 2. ACTIVITIES Getting the Images IMAGING JUPITER AND ITS MOONS Your first challenge is to use the telescope to get good images of your destination: Jupiter and its moons. In this challenge, you'll investigate the motion of the moons by taking images about once an hour for four or five hours. Amazingly, there will be enough information in these images for you to determine several properties of Jupiter that you'll need to know for your mission Ñ such as Jupiter's size, density, and gravity. This information will help you in deciding whether to establish a base camp on Jupiter. 'SCOPE IT OUT Selecting the Target: Use the pull-down menu to select Jupiter. (The telescope's computer will automatically determine Jupiter's location in the sky for the time you selected. Jupiter does not have a permanent address Ñor RA and DEC Ñ in the sky, because it moves from night to night relative to the background stars. In fact, the word "planet" means "wanderer.") Camera: Use the MAIN camera, ZOOMED IN. (If some of the moons are out of the field of view, you can use ZOOMED OUT instead.) Filter: Try using the grey filter ("ND-40") to cut down on Jupiter's glare. Exposure time: Use a 10 second exposure if you are using the grey filter. Downloading Your Image: You should be able to see Jupiter and its moons clearly in the GIF-format image on the Web, without any image processing. Be sure to download both the image AND its Image Info file, because this contains the information about how and when you took the image. It's a good idea to also download the FITS file for each image as well for your records. (Click and HOLD on the underlined link, then select "Save As...SOURCE" and download. Printing the Image: The simplest way to compare your images is to print them. TIP: Use an image processing program to INVERT your image Ñ that is, to reverse black and white. Then when you print, Jupiter and its moons will appear black against a white background. That's much easier to measure, and you'll be saving your printer's ink as well! Making Measurements: You can make measurements directly from your computer monitor, or from printed images. For an image printed at 100% scale, 1 inch = 72 pixels. From the Ground Up!: Jupiter v. 031301 -4- Harvard-Smithsonian Center for Astrophysics REFLECTING ON YOUR IMAGES: Size of Jupiter. Why does Jupiter appear so small, compared to the Moon? Point of view. Why do we see the moons arranged on a more or less straight line? Forces and motion. What keeps the moons in orbit around Jupiter? Why don't they fly off into space? Speed of the moons. Which moons appear to have moved, from image to image? Why have some moons moved more than others? Getting the big picture. Jupiter and its moons look like a miniature "solar system." How does the plane of the moons compare to the plane of the solar system? Why might that be? From the Ground Up!: Jupiter v. 031301 -5- Harvard-Smithsonian Center for Astrophysics WHICH MOON IN YOUR IMAGE IS EUROPA? You'll probably see up to four of Jupiter's moons in your image. Can you figure out which moon is Europa? The moon closest to Jupiter in nature is called Io, followed by Europa, Ganymede and Callisto. But the moon that looks closest to Jupiter in your image need not be Io. That's because, from Earth, we're looking at the moons edge-on to the plane of their orbit. For example, the image at right shows how the moons might look if you were to look DOWN on the plane of their orbit. (The image shows the relative size of the orbits, to scale.) The edge-on view below it shows how this scene would appear through the telescope. Can you label which moon is which? When you look at your images, you won't have the benefit of a top-down view to compare them to. But can you think of a way to figure out which moon is which by following the moons through several images? If you could follow the moons for long enough, you could see the furthest distance that each one gets from Jupiter. That would tell which moon is which. A second way to tell the moons apart is to see which moon moves FASTEST -- i.e., moves the furthest in several successive images taken, say, an hour apart. The moons closest to Jupiter orbit the fastest, as predicted by Newton's laws of motion.
Recommended publications
  • Lab 7: Gravity and Jupiter's Moons
    Lab 7: Gravity and Jupiter's Moons Image of Galileo Spacecraft Gravity is the force that binds all astronomical structures. Clusters of galaxies are gravitationally bound into the largest structures in the Universe, Galactic Superclusters. The galaxies themselves are held together by gravity, as are all of the star systems within them. Our own Solar System is a collection of bodies gravitationally bound to our star, Sol. Cutting edge science requires the use of Einstein's General Theory of Relativity to explain gravity. But the interactions of the bodies in our Solar System were understood long before Einstein's time. In chapter two of Chaisson McMillan's Astronomy Today, you went over Kepler's Laws. These laws of gravity were made to describe the interactions in our Solar System. P2=a3/M Where 'P' is the orbital period in Earth years, the time for the body to make one full orbit. 'a' is the length of the orbit's semi-major axis, for nearly circular orbits the orbital radius. 'M' is the total mass of the system in units of Solar Masses. Jupiter System Montage picture from NASA ID = PIA01481 Jupiter has over 60 moons at the last count, most of which are asteroids and comets captured from Written by Meagan White and Paul Lewis Page 1 the Asteroid Belt. When Galileo viewed Jupiter through his early telescope, he noticed only four moons: Io, Europa, Ganymede, and Callisto. The Jupiter System can be thought of as a miniature Solar System, with Jupiter in place of the Sun, and the Galilean moons like planets.
    [Show full text]
  • 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].
    [Show full text]
  • Astronomy 330 HW 2 Presentations Outline
    Astronomy 330 HW 2 •! Stanley Swat This class (Lecture 12): http://www.ufohowto.com/ Life in the Solar System •! Lucas Guthrie Next Class: http://www.crystalinks.com/abduction.html Life in the Solar System HW 5 is due Wednesday Music: We Are All Made of Stars– Moby Presentations Outline •! Daniel Borup •! Life on Venus? Futurama •! Life on Mars? Life in the Solar System? Earth – Venus comparison •! We want to examine in more detail the backyard of humans. •! What we find may change our estimates of ne. Radius 0.95 Earth Surface gravity 0.91 Earth Venus is the hottest Mass 0.81 Earth planet, the closest in Distance from Sun 0.72 AU size to Earth, the closest Average Temp 475 C in distance to Earth, and Year 224.7 Earth days the planet with the Length of Day 116.8 Earth days longest day. Atmosphere 96% CO2 What We Used to Think Turns Out that Venus is Hell Venus must be hotter, as it is closer the Sun, but the cloud •! The surface is hot enough to melt lead cover must reflect back a large amount of the heat. •! There is a runaway greenhouse effect •! There is almost no water In 1918, a Swedish chemist and Nobel laureate concluded: •! There is sulfuric acid rain •! Everything on Venus is dripping wet. •! Most of the surface is no doubt covered with swamps. •! Not a place to visit for Spring Break. •! The constantly uniform climatic conditions result in an entire absence of adaptation to changing exterior conditions. •! Only low forms of life are therefore represented, mostly no doubt, belonging to the vegetable kingdom; and the organisms are nearly of the same kind all over the planet.
    [Show full text]
  • Mission to Jupiter
    This book attempts to convey the creativity, Project A History of the Galileo Jupiter: To Mission The Galileo mission to Jupiter explored leadership, and vision that were necessary for the an exciting new frontier, had a major impact mission’s success. It is a book about dedicated people on planetary science, and provided invaluable and their scientific and engineering achievements. lessons for the design of spacecraft. This The Galileo mission faced many significant problems. mission amassed so many scientific firsts and Some of the most brilliant accomplishments and key discoveries that it can truly be called one of “work-arounds” of the Galileo staff occurred the most impressive feats of exploration of the precisely when these challenges arose. Throughout 20th century. In the words of John Casani, the the mission, engineers and scientists found ways to original project manager of the mission, “Galileo keep the spacecraft operational from a distance of was a way of demonstrating . just what U.S. nearly half a billion miles, enabling one of the most technology was capable of doing.” An engineer impressive voyages of scientific discovery. on the Galileo team expressed more personal * * * * * sentiments when she said, “I had never been a Michael Meltzer is an environmental part of something with such great scope . To scientist who has been writing about science know that the whole world was watching and and technology for nearly 30 years. His books hoping with us that this would work. We were and articles have investigated topics that include doing something for all mankind.” designing solar houses, preventing pollution in When Galileo lifted off from Kennedy electroplating shops, catching salmon with sonar and Space Center on 18 October 1989, it began an radar, and developing a sensor for examining Space interplanetary voyage that took it to Venus, to Michael Meltzer Michael Shuttle engines.
    [Show full text]
  • Exomoon Habitability Constrained by Illumination and Tidal Heating
    submitted to Astrobiology: April 6, 2012 accepted by Astrobiology: September 8, 2012 published in Astrobiology: January 24, 2013 this updated draft: October 30, 2013 doi:10.1089/ast.2012.0859 Exomoon habitability constrained by illumination and tidal heating René HellerI , Rory BarnesII,III I Leibniz-Institute for Astrophysics Potsdam (AIP), An der Sternwarte 16, 14482 Potsdam, Germany, [email protected] II Astronomy Department, University of Washington, Box 951580, Seattle, WA 98195, [email protected] III NASA Astrobiology Institute – Virtual Planetary Laboratory Lead Team, USA Abstract The detection of moons orbiting extrasolar planets (“exomoons”) has now become feasible. Once they are discovered in the circumstellar habitable zone, questions about their habitability will emerge. Exomoons are likely to be tidally locked to their planet and hence experience days much shorter than their orbital period around the star and have seasons, all of which works in favor of habitability. These satellites can receive more illumination per area than their host planets, as the planet reflects stellar light and emits thermal photons. On the contrary, eclipses can significantly alter local climates on exomoons by reducing stellar illumination. In addition to radiative heating, tidal heating can be very large on exomoons, possibly even large enough for sterilization. We identify combinations of physical and orbital parameters for which radiative and tidal heating are strong enough to trigger a runaway greenhouse. By analogy with the circumstellar habitable zone, these constraints define a circumplanetary “habitable edge”. We apply our model to hypothetical moons around the recently discovered exoplanet Kepler-22b and the giant planet candidate KOI211.01 and describe, for the first time, the orbits of habitable exomoons.
    [Show full text]
  • Moons Phases and Tides
    Moon’s Phases and Tides Moon Phases Half of the Moon is always lit up by the sun. As the Moon orbits the Earth, we see different parts of the lighted area. From Earth, the lit portion we see of the moon waxes (grows) and wanes (shrinks). The revolution of the Moon around the Earth makes the Moon look as if it is changing shape in the sky The Moon passes through four major shapes during a cycle that repeats itself every 29.5 days. The phases always follow one another in the same order: New moon Waxing Crescent First quarter Waxing Gibbous Full moon Waning Gibbous Third (last) Quarter Waning Crescent • IF LIT FROM THE RIGHT, IT IS WAXING OR GROWING • IF DARKENING FROM THE RIGHT, IT IS WANING (SHRINKING) Tides • The Moon's gravitational pull on the Earth cause the seas and oceans to rise and fall in an endless cycle of low and high tides. • Much of the Earth's shoreline life depends on the tides. – Crabs, starfish, mussels, barnacles, etc. – Tides caused by the Moon • The Earth's tides are caused by the gravitational pull of the Moon. • The Earth bulges slightly both toward and away from the Moon. -As the Earth rotates daily, the bulges move across the Earth. • The moon pulls strongly on the water on the side of Earth closest to the moon, causing the water to bulge. • It also pulls less strongly on Earth and on the water on the far side of Earth, which results in tides. What causes tides? • Tides are the rise and fall of ocean water.
    [Show full text]
  • 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.
    [Show full text]
  • JUICE Red Book
    ESA/SRE(2014)1 September 2014 JUICE JUpiter ICy moons Explorer Exploring the emergence of habitable worlds around gas giants Definition Study Report European Space Agency 1 This page left intentionally blank 2 Mission Description Jupiter Icy Moons Explorer Key science goals The emergence of habitable worlds around gas giants Characterise Ganymede, Europa and Callisto as planetary objects and potential habitats Explore the Jupiter system as an archetype for gas giants Payload Ten instruments Laser Altimeter Radio Science Experiment Ice Penetrating Radar Visible-Infrared Hyperspectral Imaging Spectrometer Ultraviolet Imaging Spectrograph Imaging System Magnetometer Particle Package Submillimetre Wave Instrument Radio and Plasma Wave Instrument Overall mission profile 06/2022 - Launch by Ariane-5 ECA + EVEE Cruise 01/2030 - Jupiter orbit insertion Jupiter tour Transfer to Callisto (11 months) Europa phase: 2 Europa and 3 Callisto flybys (1 month) Jupiter High Latitude Phase: 9 Callisto flybys (9 months) Transfer to Ganymede (11 months) 09/2032 – Ganymede orbit insertion Ganymede tour Elliptical and high altitude circular phases (5 months) Low altitude (500 km) circular orbit (4 months) 06/2033 – End of nominal mission Spacecraft 3-axis stabilised Power: solar panels: ~900 W HGA: ~3 m, body fixed X and Ka bands Downlink ≥ 1.4 Gbit/day High Δv capability (2700 m/s) Radiation tolerance: 50 krad at equipment level Dry mass: ~1800 kg Ground TM stations ESTRAC network Key mission drivers Radiation tolerance and technology Power budget and solar arrays challenges Mass budget Responsibilities ESA: manufacturing, launch, operations of the spacecraft and data archiving PI Teams: science payload provision, operations, and data analysis 3 Foreword The JUICE (JUpiter ICy moon Explorer) mission, selected by ESA in May 2012 to be the first large mission within the Cosmic Vision Program 2015–2025, will provide the most comprehensive exploration to date of the Jovian system in all its complexity, with particular emphasis on Ganymede as a planetary body and potential habitat.
    [Show full text]
  • An Impacting Descent Probe for Europa and the Other Galilean Moons of Jupiter
    An Impacting Descent Probe for Europa and the other Galilean Moons of Jupiter P. Wurz1,*, D. Lasi1, N. Thomas1, D. Piazza1, A. Galli1, M. Jutzi1, S. Barabash2, M. Wieser2, W. Magnes3, H. Lammer3, U. Auster4, L.I. Gurvits5,6, and W. Hajdas7 1) Physikalisches Institut, University of Bern, Bern, Switzerland, 2) Swedish Institute of Space Physics, Kiruna, Sweden, 3) Space Research Institute, Austrian Academy of Sciences, Graz, Austria, 4) Institut f. Geophysik u. Extraterrestrische Physik, Technische Universität, Braunschweig, Germany, 5) Joint Institute for VLBI ERIC, Dwingelo, The Netherlands, 6) Department of Astrodynamics and Space Missions, Delft University of Technology, The Netherlands 7) Paul Scherrer Institute, Villigen, Switzerland. *) Corresponding author, [email protected], Tel.: +41 31 631 44 26, FAX: +41 31 631 44 05 1 Abstract We present a study of an impacting descent probe that increases the science return of spacecraft orbiting or passing an atmosphere-less planetary bodies of the solar system, such as the Galilean moons of Jupiter. The descent probe is a carry-on small spacecraft (< 100 kg), to be deployed by the mother spacecraft, that brings itself onto a collisional trajectory with the targeted planetary body in a simple manner. A possible science payload includes instruments for surface imaging, characterisation of the neutral exosphere, and magnetic field and plasma measurement near the target body down to very low-altitudes (~1 km), during the probe’s fast (~km/s) descent to the surface until impact. The science goals and the concept of operation are discussed with particular reference to Europa, including options for flying through water plumes and after-impact retrieval of very-low altitude science data.
    [Show full text]
  • 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.
    [Show full text]
  • EJSM-Laplace Why Are Ganymede and Europa Habitable Worlds ?
    Exploring icy satellites for their Astrobiological potential from an astronomical point of view Athena Coustenis LESIA, Paris-Meudon Observatory France Galileo Cassini-Huygens Quelques points de considération Aspects astrobiologiques: chimie organique, eau liquide (en surface ou à l’intérieur), sources d’énergie (activité interne), stabilité Les satellites de glace avec organiques : Titan, Encelade, Triton. avec une activité évidente : Encelade, Triton, Io, (Titan?) avec de l’eau liquide à l’intérieur (à confirmer): Europe, Ganymède, Encelade, Titan A l’exception de Titan, les satellites de glace avec des océans subsurfaciques possibles (Europe, Ganymède, Callisto) ou une activité cryovolcanique évidente (Encelade, Triton) résident à l’intérieur des magnétosphères des planètes géantes, mais les deux derniers ne sont pas dans la partie avec l’irradiation surfacique extrême et destructive pour les organiques. Quel est le potentiel astrobiologique de chacun de ces satellites? Exploring the Habitability of Icy Worlds: The Europa Jupiter System Mission (JUICE) The EJSM Science Study Team 2009 All rights reserved. EJSM Theme: The Emergence of Habitable Worlds Around Gas Giants • Goal 1: Determine if the Jupiter system harbors habitable worlds • Goal 2: Characterize Jupiter system processes – Ocean characteristics (for Europa and Ganymede and perhaps other satellites) – Satellite system – Ice shells and subsurface water – Jupiter atmosphere – Deep internal structure, and (for – Magnetodisk/magnetosphere Ganymede) intrinsic magnetic field – Jovian system Interactions – External environments – Jovian system origin – Global surface compositions – Surface features and future landing sites Emphasis on icy moon habitability and Jupiter system processes 5 JGO Science: Overview • Key JGO science phases – Ganymede: Detailed orbital study . Elliptical orbit first, then circular orbit – Jupiter system: In-depth exploration .
    [Show full text]
  • Jupiter Mass
    CESAR Science Case Jupiter Mass Calculating a planet’s mass from the motion of its moons Student’s Guide Mass of Jupiter 2 CESAR Science Case Table of Contents The Mass of Jupiter ........................................................................... ¡Error! Marcador no definido. Kepler’s Three Laws ...................................................................................................................................... 4 Activity 1: Properties of the Galilean Moons ................................................................................................. 6 Activity 2: Calculate the period of your favourite moon ................................................................................. 9 Activity 3: Calculate the orbital radius of your favourite moon .................................................................... 12 Activity 4: Calculate the Mass of Jupiter ..................................................................................................... 15 Additional Activity: Predict a Transit ............................................................................................................ 16 To know more… .......................................................................................................................... 19 Links ............................................................................................................................................ 19 Mass of Jupiter 3 CESAR Science Case Background Kepler’s Three Laws The three Kepler’s Laws, published between
    [Show full text]