DOCSLIB.ORG

AN OVERVIEW of the JUNO MISSION to JUPITER Abstract Contents 1 Overview

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
AN OVERVIEW of the JUNO MISSION to JUPITER Abstract Contents 1 Overview ISTS 2006-o-2-06V AN OVERVIEW OF THE JUNO MISSION TO JUPITER Richard Grammier Jet Propulsion Laboratory 4800 Oak Grove Drive, MS 301-360, Pasadena, CA 91101-8099 USA (Email: [email protected]) Abstract radiometer for mapping atmospheric composition and dynamics, a dual- Arriving in orbit around the planet Jupiter frequency radio-gravity science system, in 2016 after a five-year journey, the Juno plasma detectors, energetic particle spacecraft will begin a one-year detectors, an ultraviolet investigation of the gas giant in order to imager/spectrometer, a plasma wave understand its origin and evolution by experiment, and a visible camera for determining its water abundance and imaging Jupiter’s poles for the first time. constraining its core mass (Figure 1). In Operations at Jupiter are simple and addition, Juno will map the planet’s repetitive. When the investigation is magnetic and gravitational fields, map its complete, the spacecraft will de-orbit into atmosphere, and explore the three- the planet itself. dimensional structure of Jupiter’s polar magnetosphere and auroras. Contents Abstract 1 1 Overview 1 2 Project Implementation 2 2.1 Science Investigations 3 2.1.1 Origin 3 2.1.2 Interior 4 2.1.3 Atmosphere 5 2.1.4 Magnetosphere 5 3 Mission Design 6 Figure 1: Juno will discriminate among different models for giant planet formation. 4 The Spacecraft 7 5 Conclusion 8 These investigations will be conducted over the course of thirty-two 11-day 6 Acknowledgements 8 elliptical polar orbits of the planet. The orbits are designed to avoid Jupiter’s 1 Overview highest radiation regions. Juno’s goal is to understand the origin and The spacecraft is a spinning, solar- evolution of Jupiter. As a gas giant, Jupiter powered system carrying a complement of can provide a wealth of knowledge that can eight science instruments for conducting help us understand the origin of our own the investigations. The spacecraft systems solar system as well understand other and instruments take advantage of planetary systems being discovered around significant design and operational heritage other stars. from previous space missions. Using a spinning, solar powered Juno’s scientific payload consists of a spacecraft, Juno will produce global maps dual-technique magnetometer, a microwave of the gravity, magnetic fields, and 1 An Overview of the Juno Mission to Jupiter ISTS 2006-o-2-06V atmospheric composition from a unique Atmospheric Composition and polar orbit with a close perijove (closest Dynamics is measured by atmospheric point to Jupiter) (Figure 2). The nominal sounding to pressures greater than 100 32-orbit mission will produce an extensive bars, producing a three-dimensional map of sample of Jupiter’s full range of latitudes the water and ammonia abundances; and and longitudes. Juno will accomplish its determining how deep the belts, zones, and mission through a combination of in situ other features penetrate. and remote observations. The largest structure in the solar system, Jupiter’s polar magnetosphere and its coupling to the atmosphere are explored by measuring auroral emissions, plasmas, fields, waves and radio emissions. 2 Project Implementation The Juno project is implemented as part of NASA’s New Frontier Program, under the leadership of Dr. Scott Bolton, the Principle Investigator (PI) from Southwest Research Institute (SwRI). The day-to-day project management and implementation is delegated to the Jet Propulsion Laboratory (JPL), under the leadership of Rick Grammier, the Project Manager (PM). SwRI and JPL teamed with several companies, universities and other NASA centers to provide the scientific instruments and spacecraft systems. JPL is providing Figure 2: Using a spinning, solar powered the overall management, project spacecraft, Juno will produce global maps of engineering, mission design and navigation, the gravity, magnetic fields, and atmospheric mission operations, payload management, composition from a unique polar orbit with a telecommunications/gravity science system, close perijove. microwave radiometer (MWR) experiment, and part of the dual-technique Juno’s investigations divide into four magnetometer. major themes: Origin, Interior Structure, Lockheed Martin (LM) is the primary Atmospheric Composition and Dynamics, spacecraft contractor and is responsible for and the Polar Magnetosphere. Origin the design, build, and test of the spacecraft discriminates among different models for as well, as the integration of the payload giant planet formation, constraining the instruments. LM also performs mission mass of the solid core by measuring the operations with JPL. gravitational field and determining the The home institution of the PI, SwRI abundance of certain heavy elements provides two of the instruments for the (oxygen and nitrogen) in Jupiter’s polar magnetosphere investigation— atmosphere via microwave observations of Ultraviolet Spectrometer (UVIS) and Jovian water and ammonia. Auroral Distributions Experiment Interior Structure maps the gravitational (JADE)—and manages the science team and magnetic fields with sufficient and the education and public outreach resolution to determine the origin of the program. magnetic field, the core mass and the Goddard Space Flight Center (GSFC) is nature of deep convection. providing the combined magnetometer experiment. Applied Physics Lab (APL) is 2 Project Implementation providing the Energetic Particle Detector sound atmospheric ammonia and water (EPD). The University of Iowa is providing from below the ammonia cloud tops to as the Waves experiment. The visible camera deep as practical. provider has not yet been selected. (The visible camera is not a science instrument and has no scientific requirements associated with it.) 2.1 SCIENCE INVESTIGATIONS 2.1.1 Origin The primary science goal of understanding planetary formation and evolution is directly related to the study of Jupiter’s interior and atmosphere. The mass of Jupiter’s core helps distinguish among Figure 3: Juno’s measurement of O competing scenarios regarding the planet’s discriminates among Jupiter’s formation formation. Jupiter’s water abundance is key scenarios. Abundances of Ar, Kr, Se, C, and S in understanding giant planet formation are well determined on Jupiter at 3x Solar. O and the delivery of volatiles throughout the is not yet determined. Juno determines both solar system (Figure 3). the N and O abundances. The microwave radiometer (MWR) instrument determines the water abundance The number of channels is sufficient to in Jupiter. It maps the water over all fully sample the desired pressure range and latitudes, thus eliminating sampling bias reach below 100 bars. inherent in limited probe measurements. The instrument is based upon a number The instrument consists of six different of previous, Earth-orbiting experiments, antennas, radiometers, and with the most recent heritage to the control/calibration electronics. The MWR Advanced Microwave Radiometer (AMR) uses six frequencies for atmospheric for the Ocean Surface Topography Mission sounding, from 0.6 GHz to 23 GHz (OSTM). (Figure 4). The wavelengths are chosen to Figure 4: Each of the six MWR antennas uses a different frequency from a range chosen to sound atmospheric ammonia and water from below the ammonia cloud tops to as deep as practical. 3 An Overview of the Juno Mission to Jupiter ISTS 2006-o-2-06V band downlink and X- and Ka-band 2.1.2 Interior uplink/downlink. Juno measures the gravity field, magnetic field, and water abundance, to determine the structure of the planet, the nature of deep convection, and the process of magnetic field generation. Juno’s low perijove allows the measurement of the gravity field to a high harmonic degree and unprecedented accuracy. The Juno measurement of the low-order gravitational harmonics, together with microwave data on envelope composition, provide key constraints on planetary structure and the mass of Jupiter’s core (Figure 5). Figure 6: Juno’s precise gravity measurements provide new constraints on Jupiter’s core mass and internal convection. Diamonds represent current knowledge. Triangles show expected tidal responses. The lines show signatures of solid-body (dashed lines) and differential (red line) rotation. By mapping Jupiter’s magnetic field with a resolution exceeding that available for any other planet, including Earth, Juno seeks to understand the origin of planetary magnetic fields. Juno also seeks to detect magnetic- field secular variation in order to image Figure 5: Juno investigates the structure fluid motions at the surface of the dynamo- and convection of Jupiter’s interior by generating region. The experiment reaching through the meteorological layer. A measures the high harmonics of the possible inner “rock” core is shown, surrounded by a “blue” metallic hydrogen magnetic field at small distance, which is envelope and a “yellow” outer envelope of crucial to understanding the dynamo molecular hydrogen, all hidden beneath the mechanism (Figure 7). visible cloud deck. The Magnetometer experiment consists of a pair of fluxgate sensors (FGM) that Juno’s gravity-science experiment measure the three components of the provides data on Jupiter’s internal vector magnetic field, and an orthogonal convection and deep winds (Figure 6). This array of scalar helium magnetometer (SHM) experiment is capable of both X- and Ka- cells that measure the magnitude of the band uplink and downlink. During the field. Both the FGM and SHM are flight mission, the X-band portion is the primary proven
Load more

Recommended publications
  • The 4 Major Asteroids and Chiron Report For
    The 4 Major Asteroids and Chiron Report for Brad Roberts 10 January 1964 6:33 AM Winnipeg, Manitoba,Canada Calculated for: Standard time, Time Zone 6 hours West Latitude: 49 N 53 Longitude: 97 W 09 Positions of Planets at Birth: Sun 19 Cap 18 Asc. 20 Sag 35 Moon 1 Sag 21 MC 21 Lib 49 Mercury 6 Cap 24 2nd cusp 0 Aqu 56 Venus 21 Aqu 54 3rd cusp 17 Pis 07 Mars 27 Cap 52 5th cusp 15 Tau 45 Jupiter 11 Ari 42 6th cusp 4 Gem 07 Saturn 21 Aqu 25 Ceres 9 Sag 44 Uranus 9 Vir 47 Pallas 20 Sco 12 Neptune 17 Sco 47 Juno 23 Sco 36 Pluto 14 Vir 47 Vesta 4 Cap 54 True Node11 Can 47 Chiron 11 Pis 23 Aspects and orbs: Conjunction : 7 Deg 00 Min Trine : 5 Deg 00 Min Opposition : 6 Deg 00 Min Sextile : 3 Deg 00 Min Square : 4 Deg 00 Min Interpretations by astrologer Dave Campbell Report and Text Copyright By Cosmic Patterns Software, Inc. The contents of this report are protected by Copyright law. By purchasing this report you agree to comply with this Copyright. Libra Moon, Inc www.libramoonastrology.com www.zodiac-reports.com Chapter 1: Ceres Ceres in Sagittarius: You nurture people with your generosity cheerfulness and encouragement. Giving them the optimism and openness they need. You aim to inspire them and make them feel like they are it. Your honest disposition and behavior is also a gift for them to know your devotion to them. All of these things are exactly what you need in order to feel cared for.
    [Show full text]
  • Juno Spacecraft Description
    Juno Spacecraft Description By Bill Kurth 2012-06-01 Juno Spacecraft (ID=JNO) Description The majority of the text in this file was extracted from the Juno Mission Plan Document, S. Stephens, 29 March 2012. [JPL D-35556] Overview For most Juno experiments, data were collected by instruments on the spacecraft then relayed via the orbiter telemetry system to stations of the NASA Deep Space Network (DSN). Radio Science required the DSN for its data acquisition on the ground. The following sections provide an overview, first of the orbiter, then the science instruments, and finally the DSN ground system. Juno launched on 5 August 2011. The spacecraft uses a deltaV-EGA trajectory consisting of a two-part deep space maneuver on 30 August and 14 September 2012 followed by an Earth gravity assist on 9 October 2013 at an altitude of 559 km. Jupiter arrival is on 5 July 2016 using two 53.5-day capture orbits prior to commencing operations for a 1.3-(Earth) year-long prime mission comprising 32 high inclination, high eccentricity orbits of Jupiter. The orbit is polar (90 degree inclination) with a periapsis altitude of 4200-8000 km and a semi-major axis of 23.4 RJ (Jovian radius) giving an orbital period of 13.965 days. The primary science is acquired for approximately 6 hours centered on each periapsis although fields and particles data are acquired at low rates for the remaining apoapsis portion of each orbit. Juno is a spin-stabilized spacecraft equipped for 8 diverse science investigations plus a camera included for education and public outreach.
    [Show full text]
  • Occultation Newsletter Volume 8, Number 4
    Volume 12, Number 1 January 2005 $5.00 North Am./$6.25 Other International Occultation Timing Association, Inc. (IOTA) In this Issue Article Page The Largest Members Of Our Solar System – 2005 . 4 Resources Page What to Send to Whom . 3 Membership and Subscription Information . 3 IOTA Publications. 3 The Offices and Officers of IOTA . .11 IOTA European Section (IOTA/ES) . .11 IOTA on the World Wide Web. Back Cover ON THE COVER: Steve Preston posted a prediction for the occultation of a 10.8-magnitude star in Orion, about 3° from Betelgeuse, by the asteroid (238) Hypatia, which had an expected diameter of 148 km. The predicted path passed over the San Francisco Bay area, and that turned out to be quite accurate, with only a small shift towards the north, enough to leave Richard Nolthenius, observing visually from the coast northwest of Santa Cruz, to have a miss. But farther north, three other observers video recorded the occultation from their homes, and they were fortuitously located to define three well- spaced chords across the asteroid to accurately measure its shape and location relative to the star, as shown in the figure. The dashed lines show the axes of the fitted ellipse, produced by Dave Herald’s WinOccult program. This demonstrates the good results that can be obtained by a few dedicated observers with a relatively faint star; a bright star and/or many observers are not always necessary to obtain solid useful observations. – David Dunham Publication Date for this issue: July 2005 Please note: The date shown on the cover is for subscription purposes only and does not reflect the actual publication date.
    [Show full text]
  • Juno Magnetometer (MAG) Standard Product Data Record and Archive Volume Software Interface Specification
    Juno Magnetometer Juno Magnetometer (MAG) Standard Product Data Record and Archive Volume Software Interface Specification Preliminary March 6, 2018 Prepared by: Jack Connerney and Patricia Lawton Juno Magnetometer MAG Standard Product Data Record and Archive Volume Software Interface Specification Preliminary March 6, 2018 Approved: John E. P. Connerney Date MAG Principal Investigator Raymond J. Walker Date PDS PPI Node Manager Concurrence: Patricia J. Lawton Date MAG Ground Data System Staff 2 Table of Contents 1 Introduction ............................................................................................................................. 1 1.1 Distribution list ................................................................................................................... 1 1.2 Document change log ......................................................................................................... 2 1.3 TBD items ........................................................................................................................... 3 1.4 Abbreviations ...................................................................................................................... 4 1.5 Glossary .............................................................................................................................. 6 1.6 Juno Mission Overview ...................................................................................................... 7 1.7 Software Interface Specification Content Overview .........................................................
    [Show full text]
  • Planetary Science
    Mission Directorate: Science Theme: Planetary Science Theme Overview Planetary Science is a grand human enterprise that seeks to discover the nature and origin of the celestial bodies among which we live, and to explore whether life exists beyond Earth. The scientific imperative for Planetary Science, the quest to understand our origins, is universal. How did we get here? Are we alone? What does the future hold? These overarching questions lead to more focused, fundamental science questions about our solar system: How did the Sun's family of planets, satellites, and minor bodies originate and evolve? What are the characteristics of the solar system that lead to habitable environments? How and where could life begin and evolve in the solar system? What are the characteristics of small bodies and planetary environments and what potential hazards or resources do they hold? To address these science questions, NASA relies on various flight missions, research and analysis (R&A) and technology development. There are seven programs within the Planetary Science Theme: R&A, Lunar Quest, Discovery, New Frontiers, Mars Exploration, Outer Planets, and Technology. R&A supports two operating missions with international partners (Rosetta and Hayabusa), as well as sample curation, data archiving, dissemination and analysis, and Near Earth Object Observations. The Lunar Quest Program consists of small robotic spacecraft missions, Missions of Opportunity, Lunar Science Institute, and R&A. Discovery has two spacecraft in prime mission operations (MESSENGER and Dawn), an instrument operating on an ESA Mars Express mission (ASPERA-3), a mission in its development phase (GRAIL), three Missions of Opportunities (M3, Strofio, and LaRa), and three investigations using re-purposed spacecraft: EPOCh and DIXI hosted on the Deep Impact spacecraft and NExT hosted on the Stardust spacecraft.
    [Show full text]
  • Phase Integral of Asteroids Vasilij G
    A&A 626, A87 (2019) Astronomy https://doi.org/10.1051/0004-6361/201935588 & © ESO 2019 Astrophysics Phase integral of asteroids Vasilij G. Shevchenko1,2, Irina N. Belskaya2, Olga I. Mikhalchenko1,2, Karri Muinonen3,4, Antti Penttilä3, Maria Gritsevich3,5, Yuriy G. Shkuratov2, Ivan G. Slyusarev1,2, and Gorden Videen6 1 Department of Astronomy and Space Informatics, V.N. Karazin Kharkiv National University, 4 Svobody Sq., Kharkiv 61022, Ukraine e-mail: [email protected] 2 Institute of Astronomy, V.N. Karazin Kharkiv National University, 4 Svobody Sq., Kharkiv 61022, Ukraine 3 Department of Physics, University of Helsinki, Gustaf Hällströmin katu 2, 00560 Helsinki, Finland 4 Finnish Geospatial Research Institute FGI, Geodeetinrinne 2, 02430 Masala, Finland 5 Institute of Physics and Technology, Ural Federal University, Mira str. 19, 620002 Ekaterinburg, Russia 6 Space Science Institute, 4750 Walnut St. Suite 205, Boulder CO 80301, USA Received 31 March 2019 / Accepted 20 May 2019 ABSTRACT The values of the phase integral q were determined for asteroids using a numerical integration of the brightness phase functions over a wide phase-angle range and the relations between q and the G parameter of the HG function and q and the G1, G2 parameters of the HG1G2 function. The phase-integral values for asteroids of different geometric albedo range from 0.34 to 0.54 with an average value of 0.44. These values can be used for the determination of the Bond albedo of asteroids. Estimates for the phase-integral values using the G1 and G2 parameters are in very good agreement with the available observational data.
    [Show full text]
  • Radiation: Lessons Learned
    Radiation:Radiation: LessonsLessons LearnedLearned Scott Bolton Southwest Research Institute Insoo Jun Jet Propulsion Laboratory This document has been reviewed for export control and it does NOT contain controlled technical data. Juno Science Objectives • Origin – Determine O/H ratio (water abundance) and constrain core mass to decide among alternative theories of origin. • Interior – Understand Jupiter's interior structure and dynamical properties by mapping its gravitational and magnetic fields. • Atmosphere – Map variations in atmospheric composition, temperature, cloud opacity and dynamics to depths greater than 100 bars. • Polar Magnetosphere – Explore the three-dimensional structure of Jupiter's polar magnetosphere and aurorae. Juno Juno Payload Gravity Science (JPL/Italy) Magnetometer— MAG (GSFC) Microwave Radiometer— MWR (JPL) Energetic Particles —JEDI (APL) Plasma ions and electrons — JADE (SwRI) Plasma waves/radio — Waves (U of Iowa) Ultra Violet Imager — UVS (SwRI) Visible Camera – Juno Cam (Malin) InfraRed Imager – JIRAM (Italy) Radiation Lessons Learned 3 Juno Juno Mission Design Launch: August 2011 5 year cruise Baseline mission: 32 polar orbits Perijove ~5000 km 11 day period Spinner Solar-powered Orbit is designed to avoid radiation from the inner belts of Jupiter. Dips inside inner belt at perijove and goes above belts (Juno is in polar orbit). Radiation Lessons Learned 4 Juno Orbit 4: Juno Gravity Science 5 days 4 days 6-hour Jupiter science pass 3 days 2 days 1 day Opportunities for 0 communication 11 with Earth 10
    [Show full text]
  • Iso and Asteroids
    r bulletin 108 Figure 1. Asteroid Ida and its moon Dactyl in enhanced colour. This colour picture is made from images taken by the Galileo spacecraft just before its closest approach to asteroid 243 Ida on 28 August 1993. The moon Dactyl is visible to the right of the asteroid. The colour is ‘enhanced’ in the sense that the CCD camera is sensitive to near-infrared wavelengths of light beyond human vision; a ‘natural’ colour picture of this asteroid would appear mostly grey. Shadings in the image indicate changes in illumination angle on the many steep slopes of this irregular body, as well as subtle colour variations due to differences in the physical state and composition of the soil (regolith). There are brighter areas, appearing bluish in the picture, around craters on the upper left end of Ida, around the small bright crater near the centre of the asteroid, and near the upper right-hand edge (the limb). This is a combination of more reflected blue light and greater absorption of near-infrared light, suggesting a difference Figure 2. This image mosaic of asteroid 253 Mathilde is in the abundance or constructed from four images acquired by the NEAR spacecraft composition of iron-bearing on 27 June 1997. The part of the asteroid shown is about 59 km minerals in these areas. Ida’s by 47 km. Details as small as 380 m can be discerned. The moon also has a deeper near- surface exhibits many large craters, including the deeply infrared absorption and a shadowed one at the centre, which is estimated to be more than different colour in the violet than any 10 km deep.
    [Show full text]
  • Appendix 1 1311 Discoverers in Alphabetical Order
    Appendix 1 1311 Discoverers in Alphabetical Order Abe, H. 28 (8) 1993-1999 Bernstein, G. 1 1998 Abe, M. 1 (1) 1994 Bettelheim, E. 1 (1) 2000 Abraham, M. 3 (3) 1999 Bickel, W. 443 1995-2010 Aikman, G. C. L. 4 1994-1998 Biggs, J. 1 2001 Akiyama, M. 16 (10) 1989-1999 Bigourdan, G. 1 1894 Albitskij, V. A. 10 1923-1925 Billings, G. W. 6 1999 Aldering, G. 4 1982 Binzel, R. P. 3 1987-1990 Alikoski, H. 13 1938-1953 Birkle, K. 8 (8) 1989-1993 Allen, E. J. 1 2004 Birtwhistle, P. 56 2003-2009 Allen, L. 2 2004 Blasco, M. 5 (1) 1996-2000 Alu, J. 24 (13) 1987-1993 Block, A. 1 2000 Amburgey, L. L. 2 1997-2000 Boattini, A. 237 (224) 1977-2006 Andrews, A. D. 1 1965 Boehnhardt, H. 1 (1) 1993 Antal, M. 17 1971-1988 Boeker, A. 1 (1) 2002 Antolini, P. 4 (3) 1994-1996 Boeuf, M. 12 1998-2000 Antonini, P. 35 1997-1999 Boffin, H. M. J. 10 (2) 1999-2001 Aoki, M. 2 1996-1997 Bohrmann, A. 9 1936-1938 Apitzsch, R. 43 2004-2009 Boles, T. 1 2002 Arai, M. 45 (45) 1988-1991 Bonomi, R. 1 (1) 1995 Araki, H. 2 (2) 1994 Borgman, D. 1 (1) 2004 Arend, S. 51 1929-1961 B¨orngen, F. 535 (231) 1961-1995 Armstrong, C. 1 (1) 1997 Borrelly, A. 19 1866-1894 Armstrong, M. 2 (1) 1997-1998 Bourban, G. 1 (1) 2005 Asami, A. 7 1997-1999 Bourgeois, P. 1 1929 Asher, D.
    [Show full text]
  • Juno Mission to Jupiter
    National Aeronautics and Space Administration Juno Mission to Jupiter unknown how deeply rooted Jupiter’s colorful, banded clouds and planet-sized spots are. And scientists yearn to understand what powers the auroras — Jupiter’s northern and southern lights. These mysteries make it clear that although Jupiter’s colorful clouds get most of the attention, some of the most enticing mysteries are hiding deep inside the planet. A Five-Year Journey Juno’s trip to Jupiter will take about five years. Though the journey may seem long, this flight plan allows the mission to use Earth’s gravity to speed the craft on its way. The spacecraft first loops around the inner solar system and then swings past Earth two years after launch to get a boost that will propel it onward to its With the exception of the sun, Jupiter is the most destination. dominant object in the solar system. Because of its enormous size and the fact that it was likely the first In July 2016, Juno will fire its main engine and slip of the planets to form, it has profoundly influenced the into orbit around the giant planet to begin its scientific formation and evolution of the other bodies that orbit mission. our star. NASA’s Juno mission will allow us to examine this gas giant planet from its innermost core to the outer A Solar-Powered, Spinning Spacecraft reaches of its enormous magnetic force field. Jupiter’s orbit is five times farther from the sun than Earth’s location, so the giant planet receives about During its mission, Juno will map Jupiter’s gravity 25 times less sunlight than Earth.
    [Show full text]
  • Nasa Technical Memorandum .1
    NASA TECHNICAL MEMORANDUM NASA TM X-64677 COMETS AND ASTEROIDS: A Strategy for Exploration REPORT OF THE COMET AND ASTEROID MISSION STUDY PANEL May 1972 .1!vP -V (NASA-TE-X- 6 q767 ) COMETS AND ASTEROIDS: A RR EXPLORATION (NASA) May 1972 CSCL 03A NATIONAL AERONAUTICS AND SPACE ADMINISTRATION Reproduced by ' NATIONAL "TECHINICAL INFORMATION: SERVICE US Depdrtmett ofCommerce :. Springfield VA 22151 TECHNICAL REPORT STANDARD TITLE PAGE · REPORT NO. 2. GOVERNMENT ACCESSION NO. 3, RECIPIENT'S CATALOG NO. NASA TM X-64677 . TITLE AND SUBTITLE 5. REPORT aE COMETS AND ASTEROIDS ___1_ A Strategy for Exploration 6. PERFORMING ORGANIZATION CODE AUTHOR(S) 8. PERFORMING ORGANIZATION REPORT # Comet and Asteroid Mission Study Panel PERFORMING ORGANIZATION NAME AND ADDRESS 10. WORK UNIT NO. 11. CONTRACT OR GRANT NO. 13. TYPE OF REPORT & PERIOD COVERED 2. SPONSORING AGENCY NAME AND ADDRESS National Aeronautics and Space Administration Technical Memorandum Washington, D. C. 20546 14. SPONSORING AGENCY CODE 5. SUPPLEMENTARY NOTES ABSTRACT Many of the asteroids probably formed near the orbits where they are found today. They accreted from gases and particles that represented the primordial solar system cloud at that location. Comets, in contrast to asteroids, probably formed far out in the solar system, and at very low temperatures; since they have retained their volatile components they are probably the most primordial matter that presently can be found anywhere in the solar system. Exploration and detailed study of comets and asteroids, therefore, should be a significant part of NASA's efforts to understand the solar system. A comet and asteroid program should consist of six major types of projects: ground-based observations;Earth-orbital observations; flybys; rendezvous; landings; and sample returns.
    [Show full text]
  • A Look Inside the Juno Mission to Jupiter12 Richard S
    A Look Inside the Juno Mission to Jupiter12 Richard S. Grammier Jet Propulsion Laboratory, California Institute of Technology 4800 Oak Grove Drive, M/S 301-320 Pasadena, CA 91109 818-354-0596 [email protected] Abstract—Juno, the second mission within the New deep-space maneuvers approximately one year after launch, Frontiers Program, is a Jupiter polar orbiter mission perform an Earth-gravity assist approximately 26 months designed to return high-priority science data that spans after launch, and achieve Jupiter orbit insertion in 2016 after across multiple divisions within NASA’s Science Mission a five-year journey. Juno will investigate the gas giant for Directorate. Juno’s science objectives, coupled with the one year, operating a suite of eight instruments to meet its natural constraints of a cost-capped, PI-led mission and the scientific objectives. After completing one year of orbital harsh environment of Jupiter, have led to a very unique science, the spacecraft will de-orbit into Jupiter for the mission and spacecraft design. purpose of planetary protection. The mission and spacecraft design accommodates the required payload suite of instruments in a way that maximizes science data collection and return, maintains a simplified orbital operations approach, and meets the many challenges associated with operating a spin-stabilized, solar- powered spacecraft in Jupiter’s high radiation and magnetic environment. The project’s efforts during the preliminary design phase have resulted in an integrated design and operations approach that meets all science objectives, retains significant technical, schedule and cost margins, and has retired key risks and challenges.
    [Show full text]