The Europa Jupiter System Mission
Total Page：16
File Type：pdf, Size：1020Kb
Load more
Recommended publications
-
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]. -
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. -
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. -
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. -
Current Status of the EJSM Jupiter Europa Orbiter Flagship Mission Design
Current Status of the EJSM Jupiter Europa Orbiter Flagship Mission Design Presentation to the International workshop: “Europa lander: science goals and experiments” 2/09 Presented by: Karla B. Clark EJSM–JEO Study Manager Jet Propulsion Laboratory California Institute of Technology Jupiter Europa Orbiter The NASA Element of the Europa Jupiter System Mission EJSM Baseline Mission Overview • NASA & ESA share mission leadership • Two independently launched and operated flight systems with complementary payloads – Jupiter Europa Orbiter (JEO): NASA-led mission element – Jupiter Ganymede Orbiter (JGO): ESA-led mission element • Mission Timeline – Nominal Launch: 2020 – Jovian system tour phase: 2–3 years – Moon orbital phase: 6–12 months – End of Prime Missions: 2029 • ~10–11 Instruments on each flight system, including Radio Science 2/8/08 Predecisional, For Planning Purposes Only 2 JGO Baseline Mission Overview • ESA-led portion of EJSM • Objectives: Jupiter System, Callisto, Ganymede • Launch vehicle: Arianne 5 • Power source: Solar Arrays • Mission timeline: – Launch: 2020 • Uses 6-year Venus-Earth-Earth gravity assist trajectory – Jovian system tour phase: ~28 months Wide Angle and Medium Resolution Camera • Multiple satellite flybys V/NIR Imaging Spectrometer – 9 Ganymede – 21 Callisto (19 close flybys) EUV/FUV Imaging Spectrometer – Ganymede orbital phase: 260 days Ka-band transponder – End of prime mission: 2029 Ultra Stable Oscillator – Spacecraft final disposition: Ganymede surface impact Magnetometer • Radiation: ~85 krad behind -
LISA, the Gravitational Wave Observatory
The ESA Science Programme Cosmic Vision 2015 – 25 Christian Erd Planetary Exploration Studies, Advanced Studies & Technology Preparations Division 04-10-2010 1 ESAESA spacespace sciencescience timelinetimeline JWSTJWST BepiColomboBepiColombo GaiaGaia LISALISA PathfinderPathfinder Proba-2Proba-2 PlanckPlanck HerschelHerschel CoRoTCoRoT HinodeHinode AkariAkari VenusVenus ExpressExpress SuzakuSuzaku RosettaRosetta DoubleDouble StarStar MarsMars ExpressExpress INTEGRALINTEGRAL ClusterCluster XMM-NewtonXMM-Newton CassiniCassini-H-Huygensuygens SOHOSOHO ImplementationImplementation HubbleHubble OperationalOperational 19901990 19941994 19981998 20022002 20062006 20102010 20142014 20182018 20222022 XMM-Newton • X-ray observatory, launched in Dec 1999 • Fully operational (lost 3 out of 44 X-ray CCD early in mission) • No significant loss of performances expected before 2018 • Ranked #1 at last extension review in 2008 (with HST & SOHO) • 320 refereed articles per year, with 38% in the top 10% most cited • Observing time over- subscribed by factor ~8 • 2,400 registered users • Largest X-ray catalogue (263,000 sources) • Best sensitivity in 0.2-12 keV range • Long uninterrupted obs. • Follow-up of SZ clusters 04-10-2010 3 INTEGRAL • γ-ray observatory, launched in Oct 2002 • Imager + Spectrograph (E/ΔE = 500) + X- ray monitor + Optical camera • Coded mask telescope → 12' resolution • 72 hours elliptical orbit → low background • P/L ~ nominal (lost 4 out 19 SPI detectors) • No serious degradation before 2016 • ~ 90 refereed articles per year • Obs -
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. -
Ganymede Science Questions and Future Exploration
Planetary Science Decadal Survey Community White Paper Ganymede science questions and future exploration Geoffrey C. Collins, Wheaton College, Norton, Massachusetts [email protected] Claudia J. Alexander, Jet Propulsion Laboratory Edward B. Bierhaus, Lockheed Martin Michael T. Bland, Washington University in St. Louis Veronica J. Bray, University of Arizona John F. Cooper, NASA Goddard Space Flight Center Frank Crary, Southwest Research Institute Andrew J. Dombard, University of Illinois at Chicago Olivier Grasset, University of Nantes Gary B. Hansen, University of Washington Charles A. Hibbitts, Johns Hopkins University Applied Physics Laboratory Terry A. Hurford, NASA Goddard Space Flight Center Hauke Hussmann, DLR, Berlin Krishan K. Khurana, University of California, Los Angeles Michelle R. Kirchoff, Southwest Research Institute Jean-Pierre Lebreton, European Space Agency Melissa A. McGrath, NASA Marshall Space Flight Center William B. McKinnon, Washington University in St. Louis Jeffrey M. Moore, NASA Ames Research Center Robert T. Pappalardo, Jet Propulsion Laboratory G. Wesley Patterson, Johns Hopkins University Applied Physics Laboratory Louise M. Prockter, Johns Hopkins University Applied Physics Laboratory Kurt Retherford, Southwest Research Institute James H. Roberts, Johns Hopkins University Applied Physics Laboratory Paul M. Schenk, Lunar and Planetary Institute David A. Senske, Jet Propulsion Laboratory Adam P. Showman, University of Arizona Katrin Stephan, DLR, Berlin Federico Tosi, Istituto Nazionale di Astrofisica, Rome Roland J. Wagner, DLR, Berlin Introduction Ganymede is a planet-sized (larger than Mercury) moon of Jupiter with unique characteristics, such as being the largest satellite in the solar system, the most centrally condensed solid body in the solar system, and the only solid body in the outer solar system known to posses an internally generated magnetic field. -
Outer Planets Flagship Mission Results
Outer Planets Flagship Mission Results Curt Niebur OPF Program Scientist NASA Headquarters OPAG Meeting March 9, 2008 Study Background and Purpose • NASA and ESA are using a multistep downselection process to carefully select their next “flagship” missions – Multiple studies in this process intended to inform decisionmakers on science value, implementation risk/issues, cost and cost risk, and technology needs • Step 1 (2007): NASA and ESA operated independently of one another – PSD conducted detailed studies for several flagship missions (Europa, Titan, Enceladus, and Jovian System Observer) • AA Stern selected two of these concepts (Europa and Titan) for further study/evaluation in 2008 – ESA solicited Cosmic Vision Class L proposals • ESA selected Laplace and Tandem proposals (as well as IXO and LISA) • Step 2 (2008): NASA and ESA began a closer collaboration – Europa and Laplace concepts combined into Europa Jupiter System Mission – Titan and Tandem concepts combined into Titan Saturn System Mission • Step 3 (2009): Single concept moves forward for further work – NASA will focus on risk mitigation – ESA will conduct industry studies of 3 Class L concepts (OP, IXO, an LISA) for downselect beyond 2010 2 Organization and Implementation • Two concepts downselected for further joint NASA-ESA study in 2008 – Europa Jupiter System Mission (EJSM) consisting of a Jupiter Europa Orbiter (JEO, contributed by NASA) and a Jupiter Ganymede Orbiter (JGO, contributed by ESA) – Titan Saturn System Mission (TSSM) consisting of a Saturn Titan Orbiter -
Exploration of the Jovian System by EJSM (Europa Jupiter System Mission): Origin of Jupiter and Evolution of Satellites
Trans. JSASS Aerospace Tech. Japan Vol. 8, No. ists27, pp. Tk_35-Tk_38, 2010 Topics Exploration of the Jovian System by EJSM (Europa Jupiter System Mission): Origin of Jupiter and Evolution of Satellites 1) 2) 2) 2) 3) By Sho SASAKI , Masaki FUJIMOTO , Takeshi TAKASHIMA , Hajime YANO , Yasumasa KASABA , 4) 4) 2) 2) Yukihiro TAKAHASHI , Jun KIMURA , Tatsuaki OKADA , Yasuhiro KAWAKATSU , 2) 2) 2) 2) 2) Yuichi TSUDA , Jun-ichiro KAWAGUCHI , Ryu FUNASE , Osamu MORI , Mutsuko MORIMOTO , 5) 6) 7) Masahiro IKOMA , Takeshi NAGANUMA , Atsushi YAMAJI , 8) 9) Hauke HUSSMANN , Kei KURITA and JUPITER WORKING GROUP 1)National Astronomical Observatory of Japan, Oshu, Japan 2)The Institute of Space and Astronautical Science, JAXA, Sagamihara, Japan 3)Tohoku University, Sendai, Japan 4)Hokkaido University, Sapporo, Japan 5)Tokyo Institute of Technology, Tokyo, Japan 6)Hiroshima University, Higashi-Hiroshima, Japan 7)Kyoto University, Kyoto, Japan 8)German Aerospace Center, Berlin, Germany 9)Earthquake Research Institute, The University of Tokyo, Tokyo, Japan (Received July 16th, 2009) EJSM (Europa Jupiter System Mission) is a planned Jovian system mission with three spacecraft aiming at coordinated observations of the Jovian satellites especially Europa and the magnetosphere, atmosphere and interior of Jupiter. It was formerly called "Laplace" mission. In October 2007, it was selected as one of future ESA scientific missions Cosmic Vision (2015-2025). From the beginning, Japanese group is participating in the discussion process of the mission. JAXA will take a role on the magnetosphere spinner JMO (Jupiter Magnetosphere Orbiter). On the other hand, ESA will take charge of JGO (Jupiter Ganymede Orbiter) and NASA will be responsible for JEO (Jupiter Europa Orbiter). -
From the Moon to the Moons: Encedalus, Ganymede and Europa
Journal of Cosmology, 2010, Vol 5, pages xxx In PRESS Cosmology, January 13, 2010 From the Moon to the Moons: Encedalus, Ganymede and Europa. The Search for Life and Reliable Biomarkers J. Chela-Flores, Ph.D., The Abdus Salam ICTP, Strada Costiera 11, 34014 Trieste, Italia, and Instituto de Estudios Avanzados, IDEA, Caracas 1015A, República Bolivariana de Venezuela Abstract The recent renewal of interest in exploring the Moon has led to further novel possibilities for the exploration of the Solar System. It is in the outer Solar System where the biggest challenges await our efforts, both in the development of instrumentation and in the clarification of the biosignatures that should be clear indications of life, as opposed to non-life signals. We argue that in the present-day larger scope of cosmology we can undertake one of the most important missions of the space sciences within our own solar system, namely the search for and discovery of a second genesis. This may be accomplished by landing on Europa's surface. We conclude that the implementation of penetrators in future exploration of the outer solar system is worthy of all the financial and technical support that will be needed, both at the national, as well as at the international level. Keywords: Astrobiology, instrumentation, exploration of the solar system, Europa, Enceladus, Biosignatures 1. Introduction It seems appropriate for a journal devoted to cosmology to encompass the field of astrobiology and to move beyond the "anthropic principle" of quantum physics, the standard astroparticle physics and astrophysics that dominate the field of classical cosmology. -
Title: Exploration of Europa Cynthia B
Title: Exploration of Europa Cynthia B. Phillips1, D. L. Blaney2, R. T. Pappalardo2, H. Hussman3, G. Collins4, R. M. Mastrapa1, J. F. Cooper5, R. Greeley6, J. B. Dalton2, T. A. Hurford5, E. B. Bierhaus7, F. Nimmo8, D. A. Williams6, D. A. Senske2, W. B. McKinnon9 1SETI Institute, 2NASA JPL/Caltech, 3DLR Institute of Planetary Research, Berlin, 4Wheaton College, 5NASA Goddard, 6Arizona State University, 7Lockheed Martin Corporation, 8 Univ. Calif. Santa Cruz, 9Washington University in St. Louis Corresponding Author: Cynthia B. Phillips Carl Sagan Center for the Study of Life in the Universe SETI Institute 515 N. Whisman Rd. Mountain View, CA 94043 [email protected] 650-810-0230 1. Introduction Data from the Galileo spacecraft revealed that Europa's icy surface likely hides a global subsurface ocean with a volume nearly three times that of Earth's oceans. The existence of liquid water in the outer solar system was once thought a remote possibility, but the combination of geological, gravitational, and magnetic field observations and theory make it appear likely that liquid water exists beneath Europa's icy surface. It is now recognized that oceans may exist within many large icy moons and potentially even within icy dwarf planets, but Europa's inferred thin ice shell, potentially active surface- ocean and ocean-silicate mantle exchange, and chemical resources from surface irradiation elevate its priority for astrobiological exploration. A Europa mission is the first step in understanding the potential for icy satellites as abodes for life. Many unanswered questions remain following the Galileo mission. How thick is the ice shell? Is Europa currently geologically active? How does the ocean interact with the ice shell and with the underlying rocky layer? What is the composition of Europa’s surface and ocean? Are there organic or inorganic biosignatures? These questions can only be answered by a new mission to Europa and the Jupiter system.