New Horizons Mission 557
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Observation of the Airglow from the ISS by the IMAP Mission *Y
2013/3/13(ANGWIN workshop, Tachikawa) Observation of the airglow from the ISS by the IMAP mission *Y. Akiya [1], A. Saito [1], T. Sakanoi [2], Y. Hozumi [1], A. Yamazaki [3], Y. Otsuka [4] [1] Graduation School of Science, Kyoto University , [2] PPARC, Tohoku University, [3] ISAS/JAXA, [4] STE Laboratory, Nagoya University ----- Outline ----- Introduction of the IMAP mission Visible and near-infrared spectrographic imager Samples of airglow observation by VISI Summary “ISS-IMAP” mission Ionosphere, Mesosphere, Upper atmosphere and Plasmasphere Imagers of the ISS-IMAP mapping mission from the mission International Space Station (ISS) Observational imagers were installed on the Exposure Facility of Japanese Experimental Module: August 9th, 2012. Initial checkout: August and September, 2012 Nominal observations: October, 2012 - [Pictures: Courtesy of JAXA/NASA] [this issue]. According to characteristics of airglow emissions, wavelength range from 630 to 762 nm. Typical total intensity of such as intensity, emission height, background continuum, etc., we airglow is 100 1000 R as listed in Table 1, and 10 % variation of selected the airglow emissions which will be measured with VISI, the total intensity must be detected in order to investigate the and determined the requirements for instrumental design. The airglow variation pattern. In addition, short exposure cycle less targets and requirements are summarized in Table 1. than several seconds is necessary to measure small-scale airglow Table 1. Scientific Targets of VISI signatures (see Table 1) considering the orbital speed of ISS (~8 km/s). Airglow Required Region Scientific Typical A sectional view of VISI and its specifications are given in (waele- spatial (height) target intensity Figure 4 and Table 2, respectively. -
Juno Telecommunications
The cover The cover is an artist’s conception of Juno in orbit around Jupiter.1 The photovoltaic panels are extended and pointed within a few degrees of the Sun while the high-gain antenna is pointed at the Earth. 1 The picture is titled Juno Mission to Jupiter. See http://www.jpl.nasa.gov/spaceimages/details.php?id=PIA13087 for the cover art and an accompanying mission overview. DESCANSO Design and Performance Summary Series Article 16 Juno Telecommunications Ryan Mukai David Hansen Anthony Mittskus Jim Taylor Monika Danos Jet Propulsion Laboratory California Institute of Technology Pasadena, California National Aeronautics and Space Administration Jet Propulsion Laboratory California Institute of Technology Pasadena, California October 2012 This research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. Reference herein to any specific commercial product, process, or service by trade name, trademark, manufacturer, or otherwise, does not constitute or imply endorsement by the United States Government or the Jet Propulsion Laboratory, California Institute of Technology. Copyright 2012 California Institute of Technology. Government sponsorship acknowledged. DESCANSO DESIGN AND PERFORMANCE SUMMARY SERIES Issued by the Deep Space Communications and Navigation Systems Center of Excellence Jet Propulsion Laboratory California Institute of Technology Joseph H. Yuen, Editor-in-Chief Published Articles in This Series Article 1—“Mars Global -
Planetary Science Division Status Report
Planetary Science Division Status Report Jim Green NASA, Planetary Science Division January 26, 2017 Astronomy and Astrophysics Advisory CommiBee Outline • Planetary Science ObjecFves • Missions and Events Overview • Flight Programs: – Discovery – New FronFers – Mars Programs – Outer Planets • Planetary Defense AcFviFes • R&A Overview • Educaon and Outreach AcFviFes • PSD Budget Overview New Horizons exploresPlanetary Science Pluto and the Kuiper Belt Ascertain the content, origin, and evoluFon of the Solar System and the potenFal for life elsewhere! 01/08/2016 As the highest resolution images continue to beam back from New Horizons, the mission is onto exploring Kuiper Belt Objects with the Long Range Reconnaissance Imager (LORRI) camera from unique viewing angles not visible from Earth. New Horizons is also beginning maneuvers to be able to swing close by a Kuiper Belt Object in the next year. Giant IcebergsObjecve 1.5.1 (water blocks) floatingObjecve 1.5.2 in glaciers of Objecve 1.5.3 Objecve 1.5.4 Objecve 1.5.5 hydrogen, mDemonstrate ethane, and other frozenDemonstrate progress gasses on the Demonstrate Sublimation pitsDemonstrate from the surface ofDemonstrate progress Pluto, potentially surface of Pluto.progress in in exploring and progress in showing a geologicallyprogress in improving active surface.in idenFfying and advancing the observing the objects exploring and understanding of the characterizing objects The Newunderstanding of Horizons missionin the Solar System to and the finding locaons origin and evoluFon in the Solar System explorationhow the chemical of Pluto wereunderstand how they voted the where life could of life on Earth to that pose threats to and physical formed and evolve have existed or guide the search for Earth or offer People’sprocesses in the Choice for Breakthrough of thecould exist today life elsewhere resources for human Year forSolar System 2015 by Science Magazine as exploraon operate, interact well as theand evolve top story of 2015 by Discover Magazine. -
Selection of the Insight Landing Site M. Golombek1, D. Kipp1, N
Manuscript Click here to download Manuscript InSight Landing Site Paper v9 Rev.docx Click here to view linked References Selection of the InSight Landing Site M. Golombek1, D. Kipp1, N. Warner1,2, I. J. Daubar1, R. Fergason3, R. Kirk3, R. Beyer4, A. Huertas1, S. Piqueux1, N. E. Putzig5, B. A. Campbell6, G. A. Morgan6, C. Charalambous7, W. T. Pike7, K. Gwinner8, F. Calef1, D. Kass1, M. Mischna1, J. Ashley1, C. Bloom1,9, N. Wigton1,10, T. Hare3, C. Schwartz1, H. Gengl1, L. Redmond1,11, M. Trautman1,12, J. Sweeney2, C. Grima11, I. B. Smith5, E. Sklyanskiy1, M. Lisano1, J. Benardino1, S. Smrekar1, P. Lognonné13, W. B. Banerdt1 1Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109 2State University of New York at Geneseo, Department of Geological Sciences, 1 College Circle, Geneseo, NY 14454 3Astrogeology Science Center, U.S. Geological Survey, 2255 N. Gemini Dr., Flagstaff, AZ 86001 4Sagan Center at the SETI Institute and NASA Ames Research Center, Moffett Field, CA 94035 5Southwest Research Institute, Boulder, CO 80302; Now at Planetary Science Institute, Lakewood, CO 80401 6Smithsonian Institution, NASM CEPS, 6th at Independence SW, Washington, DC, 20560 7Department of Electrical and Electronic Engineering, Imperial College, South Kensington Campus, London 8German Aerospace Center (DLR), Institute of Planetary Research, 12489 Berlin, Germany 9Occidental College, Los Angeles, CA; Now at Central Washington University, Ellensburg, WA 98926 10Department of Earth and Planetary Sciences, University of Tennessee, Knoxville, TN 37996 11Institute for Geophysics, University of Texas, Austin, TX 78712 12MS GIS Program, University of Redlands, 1200 E. Colton Ave., Redlands, CA 92373-0999 13Institut Physique du Globe de Paris, Paris Cité, Université Paris Sorbonne, France Diderot Submitted to Space Science Reviews, Special InSight Issue v. -
THE ATTITUDE CONTROL and DETERMINATION SYSTEMS of the SAS-A Satellite
THE ATTITUDE CONTROL and DETERMINATION SYSTEMS of the SAS-A SATElliTE F. F. Mobley, A high-speed wheel inside the satellite provides the basic attitude sta B. E. Tossman, bilization for SAS-A. Wobbling of the spin axis is removed by an G. H. Fountain ultra-sensitive nutation damper which uses a copper vane pendulum on a taut-band suspension to dissipate energy by eddy-currents. The spin axis can be oriented anywhere in space as required for the X-ray ex periment by a magnetic control system operated by commands from the ground station at Quito, Ecuador. Magnetic torquing is also used to maintain the satellite spin rate at 1/ 12 revolution per minute. These systems are outgrowths of APL developments for previous satellites, chosen for simplicity and maximum expectation of satisfactory performance in orbit. The in-orbit performance has been essentially flawless. Introduction HE ATTITUDE CONTROL SYSTEM is used to a simple and reliable open-loop system, using orient SAS-A so that the X-ray detectors can commands from the ground. This is very appealing Tscan the regions of the celestial sphere in an or since the weight and power limitations on the derly and efficient manner to detect and measure SAS-A satellite do not permit an elaborate closed new X-ray sources. The two X-ray collimators loop control system. are mounted perpendicular to the satellite spin In addition to detecting and analyzing new (Z) axis. As the satellite rotates slowly about its X-ray sources, the experimenter is interested in Z axis, the detectors scan a 5-degree-wide great correlating X-ray sources with known visible stars, circle path in the celestial sphere. -
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 -
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. -
Hubble Space Telescope Primer for Cycle 25
January 2017 Hubble Space Telescope Primer for Cycle 25 An Introduction to the HST for Phase I Proposers 3700 San Martin Drive Baltimore, Maryland 21218 [email protected] Operated by the Association of Universities for Research in Astronomy, Inc., for the National Aeronautics and Space Administration How to Get Started For information about submitting a HST observing proposal, please begin at the Cycle 25 Announcement webpage at: http://www.stsci.edu/hst/proposing/docs/cycle25announce Procedures for submitting a Phase I proposal are available at: http://apst.stsci.edu/apt/external/help/roadmap1.html Technical documentation about the instruments are available in their respective handbooks, available at: http://www.stsci.edu/hst/HST_overview/documents Where to Get Help Contact the STScI Help Desk by sending a message to [email protected]. Voice mail may be left by calling 1-800-544-8125 (within the US only) or 410-338-1082. The HST Primer for Cycle 25 was edited by Susan Rose, Senior Technical Editor and contributions from many others at STScI, in particular John Debes, Ronald Downes, Linda Dressel, Andrew Fox, Norman Grogin, Katie Kaleida, Matt Lallo, Cristina Oliveira, Charles Proffitt, Tony Roman, Paule Sonnentrucker, Denise Taylor and Leonardo Ubeda. Send comments or corrections to: Hubble Space Telescope Division Space Telescope Science Institute 3700 San Martin Drive Baltimore, Maryland 21218 E-mail:[email protected] CHAPTER 1: Introduction In this chapter... 1.1 About this Document / 7 1.2 What’s New This Cycle / 7 1.3 Resources, Documentation and Tools / 8 1.4 STScI Help Desk / 12 1.1 About this Document The Hubble Space Telescope Primer for Cycle 25 is a companion document to the HST Call for Proposals1. -
Stardust Comet Flyby
NATIONAL AERONAUTICS AND SPACE ADMINISTRATION Stardust Comet Flyby Press Kit January 2004 Contacts Don Savage Policy/Program Management 202/358-1727 NASA Headquarters, Washington DC Agle Stardust Mission 818/393-9011 Jet Propulsion Laboratory, Pasadena, Calif. Vince Stricherz Science Investigation 206/543-2580 University of Washington, Seattle, WA Contents General Release ……………………………………......………….......................…...…… 3 Media Services Information ……………………….................…………….................……. 5 Quick Facts …………………………………………..................………....…........…....….. 6 Why Stardust?..................…………………………..................………….....………......... 7 Other Comet Missions ....................................................................................... 10 NASA's Discovery Program ............................................................................... 12 Mission Overview …………………………………….................……….....……........…… 15 Spacecraft ………………………………………………..................…..……........……… 25 Science Objectives …………………………………..................……………...…........….. 34 Program/Project Management …………………………...................…..…..………...... 37 1 2 GENERAL RELEASE: NASA COMET HUNTER CLOSING ON QUARRY Having trekked 3.2 billion kilometers (2 billion miles) across cold, radiation-charged and interstellar-dust-swept space in just under five years, NASA's Stardust spacecraft is closing in on the main target of its mission -- a comet flyby. "As the saying goes, 'We are good to go,'" said project manager Tom Duxbury at NASA's Jet -
Chemical Composition of Pluto's Aerosols Analogues
EPSC Abstracts Vol. 13, EPSC-DPS2019-941-1, 2019 EPSC-DPS Joint Meeting 2019 c Author(s) 2019. CC Attribution 4.0 license. Chemical composition of Pluto’s aerosols analogues Lora Jovanovic (1), Thomas Gautier (1), Nathalie Carrasco (1), Véronique Vuitton (2), Cédric Wolters (2), François-Régis Orthous-Daunay (2), Ludovic Vettier (1), Laurène Flandinet (2) ([email protected]) (1) Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Guyancourt, France (2) Institut de Planétologie et d’Astrophysique de Grenoble (IPAG), Grenoble, France Abstract Table 1: Types of Pluto’s aerosols analogues produced with the PAMPRE experiment. The discovery of haze in Pluto’s atmosphere on July 14th, 2015, has raised lots of questions. To help Corresponding understand the data provided by the New Horizons Composition of the gas mixture altitude on spacecraft, Pluto’s aerosols analogues were Pluto [2] synthetized and their chemical composition was 99% N2 : 1% CH4 : 500 ppm CO 400 km determined by high-resolution mass spectrometry 95% N2 : 5% CH4 : 500 ppm CO 600 km (Orbitrap technique). 2.2. High-resolution mass spectrometry 1. Introduction (HRMS) study On July 14th, 2015, when Pluto was flown by the New Horizons spacecraft, aerosols were detected in its We analyzed the soluble fraction of Pluto’s aerosols atmosphere, mainly composed of molecular nitrogen analogues, dissolved in a 50:50 (v/v)% methanol:acetonitrile mixture. The analytical N2, methane CH4, with around 500 ppm of carbon monoxide CO [1,2,3]. These aerosols aggregate into instrument used was the LTQ Orbitrap XL several thin haze layers that extend at more than (ThermoFisher Scientific). -
A Deep Search for Additional Satellites Around the Dwarf Planet
Search for Additional Satellites around Haumea A Preprint typeset using LTEX style emulateapj v. 01/23/15 A DEEP SEARCH FOR ADDITIONAL SATELLITES AROUND THE DWARF PLANET HAUMEA Luke D. Burkhart1,2, Darin Ragozzine1,3,4, Michael E. Brown5 Search for Additional Satellites around Haumea ABSTRACT Haumea is a dwarf planet with two known satellites, an unusually high spin rate, and a large collisional family, making it one of the most interesting objects in the outer solar system. A fully self-consistent formation scenario responsible for the satellite and family formation is still elusive, but some processes predict the initial formation of many small moons, similar to the small moons recently discovered around Pluto. Deep searches for regular satellites around KBOs are difficult due to observational limitations, but Haumea is one of the few for which sufficient data exist. We analyze Hubble Space Telescope (HST) observations, focusing on a ten-consecutive-orbit sequence obtained in July 2010, to search for new very small satellites. To maximize the search depth, we implement and validate a non-linear shift-and-stack method. No additional satellites of Haumea are found, but by implanting and recovering artificial sources, we characterize our sensitivity. At distances between 10,000 km and 350,000 km from Haumea, satellites with radii as small as 10 km are ruled out, assuming∼ an albedo∼ (p 0.7) similar to Haumea. We also rule out satellites larger∼ than &40 km in most of the Hill sphere using≃ other HST data. This search method rules out objects similar in size to the small moons of Pluto. -
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.