DOCSLIB.ORG

Appendix: the Cassini Orbiter, Behind the Scenes

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Appendix: the Cassini Orbiter, Behind the Scenes Appendix: The Cassini Orbiter, Behind the Scenes In the pages that follow are pictures of Cassini orbiter operations personnel, beginning with those working at Caltech’s Jet Propulsion Laboratory (JPL) (Cassini’s Mission Operations Center), and then moving to pictures of operations personnel at each of the sites based outside of JPL where individual science instrument operations take place. The people depicted herein represent a subset of all of the people who have been part of the Cassini-Huygens Mission, from developing it as a candidate planetary-exploration mission in the early 1980s, to eventually being responsible for its design, construction, launch and flight. It is hoped that the knowledge exposited within this book will represent a small token of appreciation for the prodigious efforts of all of the people that have been involved with the Cassini-Huygens Mission. It is they who have made Cassini-Huygens a shining success, and their tireless efforts will continue to bear important scientific and cultural fruit far into the future. 1 The Cassini Mission Operations Center at Caltech’s Jet Propulsion Laboratory 1.1 The Cassini Program-Office Management, Resource Management, Mission Planning, and Outreach Teams Fig. 1 Row 1, left to right: M. Pao, J. Jones, C. Martinez, R. Pappalardo, S. Chatterjee, R. Zimmerman-Brachman, K. Chan; Row 2, left to right: G. Yee, D. Matson, C. Vetter, J. Nelson, E. Manor-Chapman, S. Payan; Row 3, left to right: K. Munsell, L. Spilker, A. Wessen, R. Woodall, V. Barlow, S. McConnell; Row 4: J. Smith, D. Bradford, R. Mitchell, D. Seal 783 784 Appendix: The Cassini Orbiter, Behind the Scenes 1.2 The Cassini Navigation Team Fig. 2 Row 1, left to right: E. Gist, I. Roundhill, J. Pojman, P. Antreasian, J. Frautnick, D. Vaughan; Row 2, left to right: M. Wang, R. Ionacescu, P. Thompson, J. Costello, S. Wagner, P. Williams; Row 3, left to right: K. Criddle, J. Jones, C. Ballard, F. Pelletier, B. Buffington, S. Gillam, S. Nolet; Row 4: V. Legerton, D. Roth, R. Jacobson, T. Goodson, P. Stumpf; Row 5, left to right: N. Strange, M. Wong, B. Stavert 1.3 The Cassini Mission Support Services Office Fig. 3 Row 1, left to right: O. Castillo, N. Patel, V. Trinh, T. Fujii, B. Wilson, M. Carranza, M. Rubio; Row 2, left to right: V. Villa, J. Ibanez, C. Wong, P. Smith, R. Aguilar, D. Coppedge, J. Kesterson; Row 3, left to right: R. Jobsky, C Lush, G. Eller, M. Weisenfelder, B. Elgin, D. Doan; Row 4, left to right: B. Mogensen, D. Doody, L. Mellinger, G. Chin Appendix: The Cassini Orbiter, Behind the Scenes 785 1.4 The Cassini Science Planning Team Fig. 4 Row 1, left to right: J. Pitesky, K. Steadman, A. Aguinaldo, R. Lopes, N. Vandermey, A. Hendrix, S. Edgington; Row 2, left to right: B. Larsen, L. Cheng, R. Lange, T. Ray, K. Grazier, B. Paczkowski, M. Burton, N. Kelly 1.5 The Cassini Instrument Operations Team (1) Fig. 5 Row 1, left to right: E. Martinez, J. Yoshimizu, C. To, P. Lee; Row 2, left to right: P. Andres, S. Linick, P. Callahan, H. Mortensen, D. Fleishman; Row 3: A. Culver, O. Harrison, C. Acton 786 Appendix: The Cassini Orbiter, Behind the Scenes 1.6 The Cassini Instrument Operations Team (2) Fig. 6 Row 1, left to right: L. Ly-Hollins, K. Kelleher, Y. Anderson; Row 2, left to right: A. Stevenson, B. Brooks, A. Tinio, R. Boehmer, P. Meegyeong; Row 3, left to right: C. Cordell, J. Gerhard, A. Anabtawi, E. Barbinis, M. Roy; Row 4, left to right: F. Loaiza, C. Avis, F. Leader, D. Kahan, S. Asmar, R. West 1.7 The Cassini Science and Uplink Office Fig. 7 Row 1, left to right: K. Weld, N. Rouse, C. Chouinard, B. Landry, K. Yetter, D. Tong; Row 2, left to right: R. Espinueva, J. Boyer, S. Goo, J. Berkeley, S. Chatterjee, L. Nakamura; Row 3, left to right: K. Magee, D. Conner, S. Javidnia, W. Heventhal, J. Carter, J. Krueger Appendix: The Cassini Orbiter, Behind the Scenes 787 1.8 The Cassini Spacecraft Operations Office Fig. 8 Row 1, left to right: R. Lin, L. Burke, K. Garcia, E. Wang, S. Adamiak; Row 2, left to right: J. Webster, K. Herman, P. Meakin, R. Lim, P. Morgan, M. Luna, J. Brown, A. Lee; Row 3, left to right: A. Ging, J. Wertz-Chen, C. Lee, T. Burke, M. Pellegrin, C. Mittelsteadt, S. Sarani, J. Millard, D. Beach; Row 4, left to right: C. Kirby, D. Bates, F. Chrisney, D. Morgan, R. Jurenko 1.9 The Cassini Spacecraft Operations Team Fig. 9 Row 1, left to right: G. Yang, R. Somawardhana, N. Grenander, C. Huynh, R. Mukai; Row 2, left to right: P. Yoder, C. Sagoian, K. Baddarudin, A. Thomas, R. Weaver; Row 3, left to right: L. Christodoulou, T. Barber, T. Zorn, S. Clark 788 Appendix: The Cassini Orbiter, Behind the Scenes 2 The Cassini Plasma Spectrometer (CAPS) Operations Group Fig. 10 The CAPS Operations Group. Left to right: Frank Crary, Prachet Mokashi, Greg Ferris and Judith Furman 3 The Cosmic Dust Analyzer (CDA) Operations Group Fig. 11 The CDA Operations Group: From left to right: S. Hsu (bottom), G. Matt, S. Helfert (top), G. Linkert, S. Kempf (top), D. Linkert, R. Srama (bottom), F. Postberg, E. Grün, G. Moragas-Klostermeyer (bottom), U. Beckmann Appendix: The Cassini Orbiter, Behind the Scenes 789 4 The Composite Infrared Spectrometer (CIRS) Operations Group Fig. 12 The CIRS Operations Group. Left to right, at Goddard Spaceflight Center: N. Gorius, G. Bjoraker, M. Segura, C. Nixon, D. Jennings, S. Albright, R. Achterberg, J. Pearl, A. Simon-Miller, A. Mamoutkine, E. Guandique, C. Anderson, J. Brasunas, R. Carlson, M. Kaelberer, J. Tingley; not pictured: V. Kunde and P. Romani; at the Jet Propulsion Laboratory: S. Edgington, S. Brooks, C. Roumeliotis; at the Observatoire de Paris-Meudon: E. Lellouch; at Oxford University, United Kingdom: S. Calcutt and N. Bowles 5 The Ion and Neutral Mass Spectrometer (INMS) Operations Group Fig. 13 The INMS Operations Group: Back row, left to right: David Gell (Analysis), Rob Thorpe (Ground System). Front row, left to right: Greg Fletcher (Operations team Lead), Aimee Cardenes (Operations Engineer), June Dunkelburger (Operations Engineer) 790 Appendix: The Cassini Orbiter, Behind the Scenes 6 The Imaging Science Subsystem (ISS) Group Fig. 14 The ISS Group. Left to right: Joe Spitale, Andre Brahic, Josh Riley, Robert Jacobson, Joseph Veverka, Andrew Ingersoll, Joe Ferrier, Tilmann Denk, Doug Dawson, Michael Evans, Gerhard Neukum (front), Ben Knowles (back), Thomas Roatsch (middle), Torrence Johnson (back), Henry “Luke” Dones, Carolyn Porco, Peter Thomas, Carl Murray, Sebastien Charnoz, Joseph Burns, Elizabeth “Zibi” Turtle, John Weiss, Emma Birath, Jason Perry, Preston Dyches, Daren Wilson, Paul Helfenstein, Ashwin Vasavada, Anthony DelGenio, Matthew Tiscareno, Michael Belanger Fig. 15 Individuals not included in the photo above. Top row, left to right: Emily Baker, Kevin Beurle (deceased), Bobby DiDia, Daiana DiNino; Bottom row, left to right: Pauline Helfenstein, Nicole Martin, Joe Mason Appendix: The Cassini Orbiter, Behind the Scenes 791 7 The Magnetospheric Imaging Instrument (MIMI) Operations Group Fig. 16 The MIMI Operations Group. Left to right: Jon Vandegriff, Analysis and Display Software Engineer; John Aiello, Science Planning Engineer; David LaVallee, Operations Team Lead (uplink); Martha Kusterer, Downlink Lead Engineer, INCA Display Software Engineer; Linda Burke, Operations Team Engineer (uplink and downlink); Scott Turner, INCA, SPICE, Science Planning Tool, and Command Automation Software Engineer; Stuart Nylund, Operations Team Engineer (uplink) 8 The Cassini Magnetometer (MAG) Operations Group Fig. 17 The MAG Operations Group: Top row, left to right: Steve Kellock (Instrument Manager), Nick Achilleos (Operations Engineer), Leah Al- concel (Operations Engineer). Bottom row, left to right: Charlotte Dunford (Archive Engineer), Tim Seears (Operations Engineer), Peter Slootweg (Operations Engineer). Right column: Adrian Hitchman (Archive Engineer), Joyce Wolf (Software Developer), Louise Lee (Software Developer). All personnel except JW and LL are current and former associates of Imperial College London. JW is associated with the Jet Propulsion Laboratory and LL with University of California, Los Angeles 792 Appendix: The Cassini Orbiter, Behind the Scenes 9 The Cassini RADAR Operations Group Fig. 18 The RADAR Operations Group: Front row, left to right: Young Gym, Alice Le Gall, Yanhua Anderson, Kathleen Kelleher. Back row, left to right: Richard West, Mike Janssen, Bill Johnson, Phil Callahan, Bryan Stiles, Gary Hamilton 10 The Radio and Plasma Wave Science (RPWS) Operations Group Fig. 19 The RPWS Operations Group. Front row: Robert Johnson, Terry Averkamp, Don Kirchner, George Hospodarsky; Back row: Bill Kurth, Bill Robison, Larry Granroth, Jessica Swanner, Ann Persoon, Chris Piker Appendix: The Cassini Orbiter, Behind the Scenes 793 11 The Radio Science Subsystem (RSS) Operations Group Fig. 20 The RSS Operations Group. From left to right: Sami Asmar (supervisor), John Klose, Elias Barbinis, Aseel Anabtawi (technical lead), Daniel Kahan, Don Fleischman 12 The Ultraviolet Imaging Spectrometer (UVIS) Operations Group Fig. 21 The UVIS Operations Group. From left to right: Michelle Kelly, Darren Osborne, David Judd, Alain Jouchoux, Heather Buck, Crystal Salcido, and John Donnelly 794 Appendix: The Cassini Orbiter, Behind the Scenes 13 The Visual and Infrared Mapping Spectrometer (VIMS) Operations Group Fig. 22 The VIMS Operations Group. From left to right: Dyer Lytle, Virginia Pasek, John Ivens, Bob Watson and Dan Moynihan Index A Amorphous ice, 476, 497 Absortive occultation(s), 182 Angular momentum, 414, 425, 430, 435, 436, 438, 439, 443–445, 449 Abundance, 83–86, 88–98, 100–104, 106, 107 Annular rings, 136 Acceleration, 344, 350, 353, 354, 356, 357, 359–361, 364, 365, 369, Anthe, 523, 532, 533 370 40Ar, 690, 695, 713, 717 Accretion, 425, 433, 442, 445–449, 537, 538, 541, 542, 544, 545, 547, A rings, 375–381, 383–387, 391–399, 401–403, 473, 474, 478–486, 548, 552–557, 559–562, 564, 566, 568 489, 492, 496, 501, 502 Accretional heating, 589–590 Arsine (AsH3/, 10, 13–14, 89, 90, 92, 106 Acetylene (C2H2/, 92, 94, 97, 100, 101, 103, 107, 122, 130, 131, 153, Asteroid belt, 57, 59, 64 182, 183, 186, 337 Atlas, 381, 386, 399, 438, 448 ACS.
Load more

Recommended publications
  • Analysis of Plasma Instabilities and Verification of the BOUT Code for The
    Analysis of plasma instabilities and verification of the BOUT code for the Large Plasma Device P. Popovich,1 M.V. Umansky,2 T.A. Carter,1, a) and B. Friedman1 1)Department of Physics and Astronomy and Center for Multiscale Plasma Dynamics, University of California, Los Angeles, CA 90095-1547 2)Lawrence Livermore National Laboratory, Livermore, CA 94550, USA (Dated: 8 August 2018) The properties of linear instabilities in the Large Plasma Device [W. Gekelman et al., Rev. Sci. Inst., 62, 2875 (1991)] are studied both through analytic calculations and solving numerically a system of linearized collisional plasma fluid equations using the 3D fluid code BOUT [M. Umansky et al., Contrib. Plasma Phys. 180, 887 (2009)], which has been successfully modified to treat cylindrical geometry. Instability drive from plasma pressure gradients and flows is considered, focusing on resistive drift waves, the Kelvin-Helmholtz and rotational interchange instabilities. A general linear dispersion relation for partially ionized collisional plasmas including these modes is derived and analyzed. For LAPD relevant profiles including strongly driven flows it is found that all three modes can have comparable growth rates and frequencies. Detailed comparison with solutions of the analytic dispersion relation demonstrates that BOUT accurately reproduces all characteristics of linear modes in this system. PACS numbers: 52.30.Ex, 52.35.Fp, 52.35.Kt, 52.35.Lv, 52.65.Kj arXiv:1004.4674v4 [physics.plasm-ph] 26 Jan 2011 a)Electronic mail: [email protected] 1 I. INTRODUCTION Understanding complex nonlinear phenomena in magnetized plasmas increasingly relies on the use of numerical simulation as an enabling tool.
    [Show full text]
  • Copyrighted Material
    Index Abulfeda crater chain (Moon), 97 Aphrodite Terra (Venus), 142, 143, 144, 145, 146 Acheron Fossae (Mars), 165 Apohele asteroids, 353–354 Achilles asteroids, 351 Apollinaris Patera (Mars), 168 achondrite meteorites, 360 Apollo asteroids, 346, 353, 354, 361, 371 Acidalia Planitia (Mars), 164 Apollo program, 86, 96, 97, 101, 102, 108–109, 110, 361 Adams, John Couch, 298 Apollo 8, 96 Adonis, 371 Apollo 11, 94, 110 Adrastea, 238, 241 Apollo 12, 96, 110 Aegaeon, 263 Apollo 14, 93, 110 Africa, 63, 73, 143 Apollo 15, 100, 103, 104, 110 Akatsuki spacecraft (see Venus Climate Orbiter) Apollo 16, 59, 96, 102, 103, 110 Akna Montes (Venus), 142 Apollo 17, 95, 99, 100, 102, 103, 110 Alabama, 62 Apollodorus crater (Mercury), 127 Alba Patera (Mars), 167 Apollo Lunar Surface Experiments Package (ALSEP), 110 Aldrin, Edwin (Buzz), 94 Apophis, 354, 355 Alexandria, 69 Appalachian mountains (Earth), 74, 270 Alfvén, Hannes, 35 Aqua, 56 Alfvén waves, 35–36, 43, 49 Arabia Terra (Mars), 177, 191, 200 Algeria, 358 arachnoids (see Venus) ALH 84001, 201, 204–205 Archimedes crater (Moon), 93, 106 Allan Hills, 109, 201 Arctic, 62, 67, 84, 186, 229 Allende meteorite, 359, 360 Arden Corona (Miranda), 291 Allen Telescope Array, 409 Arecibo Observatory, 114, 144, 341, 379, 380, 408, 409 Alpha Regio (Venus), 144, 148, 149 Ares Vallis (Mars), 179, 180, 199 Alphonsus crater (Moon), 99, 102 Argentina, 408 Alps (Moon), 93 Argyre Basin (Mars), 161, 162, 163, 166, 186 Amalthea, 236–237, 238, 239, 241 Ariadaeus Rille (Moon), 100, 102 Amazonis Planitia (Mars), 161 COPYRIGHTED
    [Show full text]
  • Mars Express Orbiter Radio Science
    MaRS: Mars Express Orbiter Radio Science M. Pätzold1, F.M. Neubauer1, L. Carone1, A. Hagermann1, C. Stanzel1, B. Häusler2, S. Remus2, J. Selle2, D. Hagl2, D.P. Hinson3, R.A. Simpson3, G.L. Tyler3, S.W. Asmar4, W.I. Axford5, T. Hagfors5, J.-P. Barriot6, J.-C. Cerisier7, T. Imamura8, K.-I. Oyama8, P. Janle9, G. Kirchengast10 & V. Dehant11 1Institut für Geophysik und Meteorologie, Universität zu Köln, D-50923 Köln, Germany Email: [email protected] 2Institut für Raumfahrttechnik, Universität der Bundeswehr München, D-85577 Neubiberg, Germany 3Space, Telecommunication and Radio Science Laboratory, Dept. of Electrical Engineering, Stanford University, Stanford, CA 95305, USA 4Jet Propulsion Laboratory, 4800 Oak Grove Drive, Pasadena, CA 91009, USA 5Max-Planck-Instuitut für Aeronomie, D-37189 Katlenburg-Lindau, Germany 6Observatoire Midi Pyrenees, F-31401 Toulouse, France 7Centre d’etude des Environnements Terrestre et Planetaires (CETP), F-94107 Saint-Maur, France 8Institute of Space & Astronautical Science (ISAS), Sagamihara, Japan 9Institut für Geowissenschaften, Abteilung Geophysik, Universität zu Kiel, D-24118 Kiel, Germany 10Institut für Meteorologie und Geophysik, Karl-Franzens-Universität Graz, A-8010 Graz, Austria 11Observatoire Royal de Belgique, B-1180 Bruxelles, Belgium The Mars Express Orbiter Radio Science (MaRS) experiment will employ radio occultation to (i) sound the neutral martian atmosphere to derive vertical density, pressure and temperature profiles as functions of height to resolutions better than 100 m, (ii) sound
    [Show full text]
  • Annualreport2005 Web.Pdf
    Vision Statement The Space Science Institute is a thriving center of talented, entrepreneurial scientists, educators, and other professionals who make outstanding contributions to humankind’s understanding and appreciation of planet Earth, the Solar System, the galaxy, and beyond. 2 | Space Science Institute | Annual Report 2005 From Our Director Excite. Explore. Discover. These words aptly describe what we do in the research realm as well as in education. In fact, they defi ne the essence of our mission. Our mission is facilitated by a unique blend of on- and off-site researchers coupled with an extensive portfolio of education and public outreach (EPO) projects. This past year has seen SSI grow from $4.1M to over $4.3M in grants, an increase of nearly 6%. We now have over fi fty full and part-time staff. SSI’s support comes mostly from NASA and the National Sci- ence Foundation. Our Board of Directors now numbers eight. Their guidance and vision—along with that of senior management—have created an environment that continues to draw world-class scientists to the Institute and allows us to develop educa- tion and outreach programs that benefi t millions of people worldwide. SSI has a robust scientifi c research program that includes robotic missions such as the Mars Exploration Rovers, fl ight missions such as Cassini and the Spitzer Space Telescope, Hubble Space Telescope (HST), and ground-based programs. Dr. Tom McCord joined the Institute in 2005 as a Senior Research Scientist. He directs the Bear Fight Center, a 3,000 square-foot research and meeting facility in Washington state.
    [Show full text]
  • 3.1 Discipline Science Results
    CASSINI FINAL MISSION REPORT 2019 1 SATURN Before Cassini, scientists viewed Saturn’s unique features only from Earth and from a few spacecraft flybys. During more than a decade orbiting the gas giant, Cassini studied the composition and temperature of Saturn’s upper atmosphere as the seasons changed there. Cassini also provided up-close observations of Saturn’s exotic storms and jet streams, and heard Saturn’s lightning, which cannot be detected from Earth. The Grand Finale orbits provided valuable data for understanding Saturn’s interior structure and magnetic dynamo, in addition to providing insight into material falling into the atmosphere from parts of the rings. Cassini’s Saturn science objectives were overseen by the Saturn Working Group (SWG). This group consisted of the scientists on the mission interested in studying the planet itself and phenomena which influenced it. The Saturn Atmospheric Modeling Working Group (SAMWG) was formed to specifically characterize Saturn’s uppermost atmosphere (thermosphere) and its variation with time, define the shape of Saturn’s 100 mbar and 1 bar pressure levels, and determine when the Saturn safely eclipsed Cassini from the Sun. Its membership consisted of experts in studying Saturn’s upper atmosphere and members of the engineering team. 2 VOLUME 1: MISSION OVERVIEW & SCIENCE OBJECTIVES AND RESULTS CONTENTS SATURN ........................................................................................................................................................................... 1 Executive
    [Show full text]
  • 20120016986.Pdf
    CIRS AND CIRS-LITE AS DESIGNED FOR THE OUTER PLANETS: TSSM, EJSM, JUICE J. Brasunas\ M. Abbas2, V. Bly!, M. Edgerton!, J. Hagopian\ W. Mamakos\ A. Morell\ B. Pasquale\ W. Smith!; !NASA God­ dard, Greenbelt, MD; 2NASA Marshall, Huntsville, AL; 3Design Interface, Finksburg, MD. Introduction: Passive spectroscopic remote sensing of mid infrared, a rich source of molecular lines in the outer planetary atmospheres and surfaces in the thermal infrared is solar system. The FTS approach is a workhorse compared a powerful tool for obtaining information about surface and with more specialized instruments such as heterodyne mi­ atmospheric temperatures, composition, and dynamics (via crowave spectrometers which are more limited in wavelength the thermal wind equation). Due to its broad spectral cover­ range and thus the molecular constituents detectable. As age, the Fourier transform spectrometer (FTS) is particularly such it is well adapted to map temperatures, composition, suited to the exploration and discovery of molecular species. aerosols, and condensates in Titan's atmosphere and surface NASA Goddard's Cassini CIRS FTS [I] (Fig. I) has given temperatures on Enceladus. Additionally, a lighter, more us important new insights into stratospheric composition and sensitive version ofCIRS can be used to advantage in other jets on Jupiter and Saturn, the cryo-vo1cano and thermal planetary missions, and for orbital and surface lunar mis­ stripes on Enceladus, and the polar vortex on Titan. We sions. have designed a lightweight successor to CIRS - called CIRS-lite - with improved spectral resolution (Table I) to Details of the four key components for CIRS-lite are: separate blended spectral lines (such as occur with isotopes).
    [Show full text]
  • Shear Flow-Interchange Instability in Nightside Magnetotail Causes Auroral Beads As a Signature of Substorm Onset
    manuscript submitted to JGR: Space Physics Shear flow-interchange instability in nightside magnetotail causes auroral beads as a signature of substorm onset Jason Derr1, Wendell Horton1, Richard Wolf2 1Institute for Fusion Studies and Applied Research Laboratories, University of Texas at Austin 2Physics and Astronomy Department, Rice University Key Points: • A wedge model is extended to obtain a MHD magnetospheric wave equation for the near-Earth magnetotail, including velocity shear effects. • Shear flow-interchange instability to replace shear flow-ballooning and interchange in- stabilities as substorm onset cause. • WKB applicability conditions suggest nonlinear analysis is necessary and yields spatial scale of most unstable mode’s variations. arXiv:1904.11056v1 [physics.space-ph] 24 Apr 2019 Corresponding author: Jason Derr, [email protected] –1– manuscript submitted to JGR: Space Physics Abstract A geometric wedge model of the near-earth nightside plasma sheet is used to derive a wave equation for low frequency shear flow-interchange waves which transmit E~ × B~ sheared zonal flows along magnetic flux tubes towards the ionosphere. Discrepancies with the wave equation result used in Kalmoni et al. (2015) for shear flow-ballooning instability are dis- cussed. The shear flow-interchange instability appears to be responsible for substorm onset. The wedge wave equation is used to compute rough expressions for dispersion relations and local growth rates in the midnight region of the nightside magnetotail where the instability develops, forming the auroral beads characteristic of geomagnetic substorm onset. Stability analysis for the shear flow-interchange modes demonstrates that nonlinear analysis is neces- sary for quantitatively accurate results and determines the spatial scale on which the instability varies.
    [Show full text]
  • + New Horizons
    Media Contacts NASA Headquarters Policy/Program Management Dwayne Brown New Horizons Nuclear Safety (202) 358-1726 [email protected] The Johns Hopkins University Mission Management Applied Physics Laboratory Spacecraft Operations Michael Buckley (240) 228-7536 or (443) 778-7536 [email protected] Southwest Research Institute Principal Investigator Institution Maria Martinez (210) 522-3305 [email protected] NASA Kennedy Space Center Launch Operations George Diller (321) 867-2468 [email protected] Lockheed Martin Space Systems Launch Vehicle Julie Andrews (321) 853-1567 [email protected] International Launch Services Launch Vehicle Fran Slimmer (571) 633-7462 [email protected] NEW HORIZONS Table of Contents Media Services Information ................................................................................................ 2 Quick Facts .............................................................................................................................. 3 Pluto at a Glance ...................................................................................................................... 5 Why Pluto and the Kuiper Belt? The Science of New Horizons ............................... 7 NASA’s New Frontiers Program ........................................................................................14 The Spacecraft ........................................................................................................................15 Science Payload ...............................................................................................................16
    [Show full text]
  • 2018: Aiaa-Space-Report
    AIAA TEAM SPACE TRANSPORTATION DESIGN COMPETITION TEAM PERSEPHONE Submitted By: Chelsea Dalton Ashley Miller Ryan Decker Sahil Pathan Layne Droppers Joshua Prentice Zach Harmon Andrew Townsend Nicholas Malone Nicholas Wijaya Iowa State University Department of Aerospace Engineering May 10, 2018 TEAM PERSEPHONE Page I Iowa State University: Persephone Design Team Chelsea Dalton Ryan Decker Layne Droppers Zachary Harmon Trajectory & Propulsion Communications & Power Team Lead Thermal Systems AIAA ID #908154 AIAA ID #906791 AIAA ID #532184 AIAA ID #921129 Nicholas Malone Ashley Miller Sahil Pathan Joshua Prentice Orbit Design Science Science Science AIAA ID #921128 AIAA ID #922108 AIAA ID #761247 AIAA ID #922104 Andrew Townsend Nicholas Wijaya Structures & CAD Trajectory & Propulsion AIAA ID #820259 AIAA ID #644893 TEAM PERSEPHONE Page II Contents 1 Introduction & Problem Background2 1.1 Motivation & Background......................................2 1.2 Mission Definition..........................................3 2 Mission Overview 5 2.1 Trade Study Tools..........................................5 2.2 Mission Architecture.........................................6 2.3 Planetary Protection.........................................6 3 Science 8 3.1 Observations of Interest.......................................8 3.2 Goals.................................................9 3.3 Instrumentation............................................ 10 3.3.1 Visible and Infrared Imaging|Ralph............................ 11 3.3.2 Radio Science Subsystem.................................
    [Show full text]
  • Accessing Pds Data in Pipeline Processing and Web Sites Through Pds Geosciences Orbital Data Explorer’S Web-Based Api (Rest) Interface
    45th Lunar and Planetary Science Conference (2014) 1026.pdf ACCESSING PDS DATA IN PIPELINE PROCESSING AND WEB SITES THROUGH PDS GEOSCIENCES ORBITAL DATA EXPLORER’S WEB-BASED API (REST) INTERFACE. K. J. Bennett, J. Wang, D. Scholes, Washington University in St. Louis, 1 Brookings Drive, Campus Box 1169, St. Louis, Missouri, 63130, {bennett, wang, sholes}@wunder.wustl.edu. Introduction: The Orbital Data Explorer (ODE) is tem (RSS). a web-based search tool (http://ode.rsl.wustl.edu) de- High Resolution Stereo Camera (HRSC), Mars Advanced Radar for Subsurface and Iono- veloped at NASA’s Planetary Data System’s (PDS) sphere Sounding (MARSIS), OMEGA Geosciences Node (http://pds-geosciences.wustl.edu/). Mars Express (Observatoire Mineralogie, Eau, Glaces, Through ODE, users can search, browse, and download Activite) Visible and Infrared Mineralogical a wide range of PDS Mars, Moon, Mercury, and Venus Mapping Spectrometer, and Planetary Fourier Spectrometer (PFS). data ([1,2,3,4]). Mars Orbiter Laser Altimeter (MOLA), and Mars Global In the fall of 2012, the Geosciences node intro- MOC Narrow Angle (NA) and Wide Angle Surveyor (MGS) duced a simple web-based API that allows non-PDS (WA) cameras. Gamma Ray Spectrometer (GRS) and Thermal web and processing tools to search for PDS products, Odyssey Emission Imaging System (THEMIS) obtain meta-data about those products, and download Viking Orbiter Visual Imaging Subsystem Camera A/B the products stored in ODE’s meta-data database. The Gamma Ray Spectrometer (GRS), Radio Sci- first version is now used by several teams in periodic MESSENGER ence Subsystem (RSS), Neutron Spectrometer processing and web sites.
    [Show full text]
  • Instrumental Methods for Professional and Amateur
    Instrumental Methods for Professional and Amateur Collaborations in Planetary Astronomy Olivier Mousis, Ricardo Hueso, Jean-Philippe Beaulieu, Sylvain Bouley, Benoît Carry, Francois Colas, Alain Klotz, Christophe Pellier, Jean-Marc Petit, Philippe Rousselot, et al. To cite this version: Olivier Mousis, Ricardo Hueso, Jean-Philippe Beaulieu, Sylvain Bouley, Benoît Carry, et al.. Instru- mental Methods for Professional and Amateur Collaborations in Planetary Astronomy. Experimental Astronomy, Springer Link, 2014, 38 (1-2), pp.91-191. 10.1007/s10686-014-9379-0. hal-00833466 HAL Id: hal-00833466 https://hal.archives-ouvertes.fr/hal-00833466 Submitted on 3 Jun 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. Instrumental Methods for Professional and Amateur Collaborations in Planetary Astronomy O. Mousis, R. Hueso, J.-P. Beaulieu, S. Bouley, B. Carry, F. Colas, A. Klotz, C. Pellier, J.-M. Petit, P. Rousselot, M. Ali-Dib, W. Beisker, M. Birlan, C. Buil, A. Delsanti, E. Frappa, H. B. Hammel, A.-C. Levasseur-Regourd, G. S. Orton, A. Sanchez-Lavega,´ A. Santerne, P. Tanga, J. Vaubaillon, B. Zanda, D. Baratoux, T. Bohm,¨ V. Boudon, A. Bouquet, L. Buzzi, J.-L. Dauvergne, A.
    [Show full text]
  • The Topography of Iapetus' Leading Side
    Icarus 193 (2008) 359–371 www.elsevier.com/locate/icarus The topography of Iapetus’ leading side Bernd Giese a,∗, Tilmann Denk b, Gerhard Neukum b, Thomas Roatsch a, Paul Helfenstein c, Peter C. Thomas c, Elizabeth P. Turtle d, Alfred McEwen e, Carolyn C. Porco f a DLR, Institute of Planetary Research, Rutherfordstr. 2, 12489 Berlin, Germany b Department of Earth Sciences, Freie Universität Berlin, 12249 Berlin, Germany c Center for Radiophysics and Space Research, Cornell University, Ithaca, NY 14853, USA d Johns Hopkins University Applied Physics Laboratory, 11100 Johns Hopkins Rd., Laurel, MD 20723, USA e Lunar and Planetary Laboratory, University of Arizona, 1541 E. University Blvd., Tucson, AZ 85721, USA f Cassini Imaging Central Laboratory for Operations, Space Science Institute, 4750 Walnut Street, Suite 205, Boulder, CO 80301, USA Received 12 December 2006; revised 15 May 2007 Available online 18 July 2007 Abstract We have used Cassini stereo images to study the topography of Iapetus’ leading side. A terrain model derived at resolutions of 4–8 km reveals that Iapetus has substantial topography with heights in the range of −10 km to +13 km, much more than observed on the other middle-sized satellites of Saturn so far. Most of the topography is older than 4 Ga [Neukum, G., Wagner, R., Denk, T., Porco, C.C., 2005. Lunar Planet. Sci. XXXVI. Abstract 2034] which implies that Iapetus must have had a thick lithosphere early in its history to support this topography. Models of lithospheric deflection by topographic loads provide an estimate of the required elastic thickness in the range of 50–100 km.
    [Show full text]