Cassini-Huygens Probe Telecommunications
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The Contribution of Global Ocean Observation of Continuity of HY-2
CGMS-XXXVI-CNSA-WP-04 Prepared by CNSA Agenda Item: III/3&4 The contribution of global ocean observation of continuity of HY-2 satellite HY-2 satellite, an ocean dynamic environment observation satellite, mainly ` objective is monitoring and detecting the parameters of ocean dynamic environment. These parameters include sea surface wind fields, sea surface height, wave height, gravity field, ocean circulation and sea surface temperature etc. The contribution of global ocean observation of continuity of HY-2 satellite 1. Introduction HY-2 satellite scatterometer provides sea surface wind fields, which can offset the observation gap of the plan of global scatterometer. At the same time, HY-2 satellite altimeter provides sea surface height, significant wave height, sea surface wind speed and polar ice sheet elevation, which can offset the observation gap of the plan of global altimeter around 2012, and can offset the observation gap of JASON-1&2 at polar area. More details as follows. 2. Observation of sea surface wind fields The analysis accuracy of wind field for ocean-atmosphere can improve 10-20% by using the satellite scatterometer data, by which can improve greatly the quality of initial wind field of numerical atmospheric forecast model in coastal ocean. Satellite scatterometer data has play important role on study of large-scale ocean phenomenon, such as sea-air interactions, ocean circulation, EI Nino etc. The figure 1 shows that QuikSCAT scatterometer has operational application in 1999, but it has not the following plan. ERS-2 scatterometer mission has transferred to METOP ASCAT in 2006. GCOM-B1 will launch in 2008, one of its payloads is an ocean vector wind measurement (OVWM) instruments, and it also called AlphaScat. -
In Brief Modified to Increase Engine Reliability
r bulletin 102 — may 2000 3rd Space Station ESA, together with a European industrial Element to be Launched consortium headed by DaimlerChrysler (D) and including Belgian, Dutch and French NASA and the Russian Aviation and partners, was responsible for the design, Space Agency (Rosaviakosmos) plan that development and delivery of the core data the next component of the International management system, which provides Space Station (ISS) – the Zvezda service Zvezda’s main computer. module – will be launched on 12 July from the Baikonur Cosmodrome in Kazakhstan. ESA also has a contract with Rosaviakosmos and RSC-Energia for Following a Joint Programme Review and performing system and interface a General Designers’ Review in Moscow, it integration tasks required for docking with was agreed that Zvezda (Russian for Zvezda by ESA’s Automated Transfer ‘star’) will be launched by a Proton rocket Vehicle (ATV), which will be used for ISS with the second and third stage engines re-boost and logistics support missions In Brief modified to increase engine reliability. from 2003 onwards. Through its ATV industrial consortium led by Aerospatiale Zvezda will provide the early living quarters Matra Lanceurs (F), ESA is also procuring for ISS crew, together with the life sup- some Russian hardware and software for port, electrical power distribution, data use with the ATV. management, flight control, and propul- sion systems for the ISS. On the scientific side, ESA has concluded contracts with Rosaviakosmos and RSC- Energia for the conduct of scientific experiments on Zvezda, including the Global Timing System (GTS) and a radiobiology experiment (called Matroshka) to monitor and analyse radiation doses in ISS crew. -
Mars Reconnaissance Orbiter
Chapter 6 Mars Reconnaissance Orbiter Jim Taylor, Dennis K. Lee, and Shervin Shambayati 6.1 Mission Overview The Mars Reconnaissance Orbiter (MRO) [1, 2] has a suite of instruments making observations at Mars, and it provides data-relay services for Mars landers and rovers. MRO was launched on August 12, 2005. The orbiter successfully went into orbit around Mars on March 10, 2006 and began reducing its orbit altitude and circularizing the orbit in preparation for the science mission. The orbit changing was accomplished through a process called aerobraking, in preparation for the “science mission” starting in November 2006, followed by the “relay mission” starting in November 2008. MRO participated in the Mars Science Laboratory touchdown and surface mission that began in August 2012 (Chapter 7). MRO communications has operated in three different frequency bands: 1) Most telecom in both directions has been with the Deep Space Network (DSN) at X-band (~8 GHz), and this band will continue to provide operational commanding, telemetry transmission, and radiometric tracking. 2) During cruise, the functional characteristics of a separate Ka-band (~32 GHz) downlink system were verified in preparation for an operational demonstration during orbit operations. After a Ka-band hardware anomaly in cruise, the project has elected not to initiate the originally planned operational demonstration (with yet-to-be used redundant Ka-band hardware). 201 202 Chapter 6 3) A new-generation ultra-high frequency (UHF) (~400 MHz) system was verified with the Mars Exploration Rovers in preparation for the successful relay communications with the Phoenix lander in 2008 and the later Mars Science Laboratory relay operations. -
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 -
NASA's STEREO Mission
NASA’s STEREO Mission J.B. Gurman STEREO Project Scientist W.T. Thompson STEREO Chief Observer Solar Physics Laboratory, Helophysics Division NASA Goddard Space Flight Center 1 The STEREO Mission • Science and technology definition team report, 1997 December: • Understand the origin and consequences of coronal mass ejections (CMEs) • Two spacecraft in earth-leading and -lagging orbits near 1 AU (Solar Terrestrial Probe line) • “Beacon” mode for near-realtime warning of potentially geoeffective events 2 Level 1 Requirements • Understand the causes and mechanisms of CME initiation • Characterize the propagation of CMEs through the heliosphere • Discover the mechanisms and sites of energetic particle acceleration in the low corona and the interplanetary medium • Develop a 3D, time-dependent model of the magnetic topology, temperature, density, and velocity structure of the ambient solar wind 3 Implementation • Two nearly identical spacecraft launched by a single ELV • Bottom spacecraft in stack has adapter ring, some strengthening • Spacecraft built at Johns Hopkins University APL • Four science investigations 4 Scientific Instruments • S/WAVES - broad frequency response RF detection of Type II, III bursts • PLASTIC - solar wind plasma and suprathermal ion composition measurements • IMPACT - energetic electrons and ions, magnetic field • SECCHI - EUV, coronagraphs and heliospheric imagers (surface to 1.5 AU) 5 Instrument Hardware • PLASTIC IMPACT boom IMPACT boom SECCHI SCIP SECCHI HI S/WAVES 6 Orbit Design • Science team selected a separation -
Nustar Observatory Guide
NuSTAR Guest Observer Program NuSTAR Observatory Guide Version 3.2 (June 2016) NuSTAR Science Operations Center, California Institute of Technology, Pasadena, CA NASA Goddard Spaceflight Center, Greenbelt, MD nustar.caltech.edu heasarc.gsfc.nasa.gov/docs/nustar/index.html i Revision History Revision Date Editor Comments D1,2,3 2014-08-01 NuSTAR SOC Initial draft 1.0 2014-08-15 NuSTAR GOF Release for AO-1 Addition of more information about CZT 2.0 2014-10-30 NuSTAR SOC detectors in section 3. 3.0 2015-09-24 NuSTAR SOC Update to section 4 for release of AO-2 Update for NuSTARDAS v1.6.0 release 3.1 2016-05-10 NuSTAR SOC (nusplitsc, Section 5) 3.2 2016-06-15 NuSTAR SOC Adjustment to section 9 ii Table of Contents Revision History ......................................................................................................................................................... ii 1. INTRODUCTION ................................................................................................................................................... 1 1.1 NuSTAR Program Organization ..................................................................................................................................................................................... 1 2. The NuSTAR observatory .................................................................................................................................... 2 2.1 NuSTAR Performance ........................................................................................................................................................................................................ -
On the Use of Scatterometer Winds in Nwp
ON THE USE OF SCATTEROMETER WINDS IN NWP Ad Stoffelen KNMI, de Bilt, the Netherlands, Email: [email protected] Lars Isaksen, Didier le Meur ECMWF, Reading, UK ABSTRACT Over the last years the processing of ERS scatterometer winds has been refined. Subsequently, High Resolution Limited Area Model, HIRLAM, and ECMWF model data assimilation experiments have been carried out to assess the impact of one scatterometer, ERS-1 and of two scatterometers, ERS-1 and ERS-2, on the analyses and forecasts. We found that scatterometer winds have a clear and beneficial impact in the data assimilation cycle and on the forecasts. Furthermore, ECMWF has shown that ERS scatterometer data improve the prediction of tropical cyclones in 4Dvar, where unprecedented skillful medium-range forecasts result of potential large social-economic value. Nevertheless, scatterometer winds contain much sub-synoptic scale information where the smallest scales resolved are difficult to assimilate into a Numerical Weather Prediction, NWP, model. This is mainly due to the otherwise general sparsity of the observing system over the ocean. In line with this it is found that scatterometer data coverage is very important for obtaining a large impact. In that respect future scatterometer systems such as SeaWinds on QuikSCAT and ADEOS- II, and ASCAT on EPS are promising. 1. INTRODUCTION After the launch of ERS-1 much improvement has been made in the interpretation of scatterometer backscatter measurements and a good quality wind product has emerged (Stoffelen and Anderson, 1997a, 1997b and 1997c). The consistency of the scatterometer winds over the swath makes them particularly useful for nowcasting purposes and several examples of the usefulness of the direct visual presentation of scatterometer winds to a meteorologist can be given. -
ASCAT – Metop's Advanced Scatterometer
ascat ASCAT – Metop’s Advanced Scatterometer R.V. Gelsthorpe Earth Observation Programmes Development Department, ESA Directorate of Application Programmes, ESTEC, Noordwijk, The Netherlands E. Schied Dornier Satelllitensysteme*, Friedrichshafen, Germany J.J.W. Wilson Eumetsat, Darmstadt, Germany Introduction Figure 1 indicates the form of the variation of Wind scatterometers already flown on ESA’s backscattering coefficient with relative wind ERS-1 and ERS-2 satellites have demonstrated direction (at a fixed incidence angle) for a range the value of such instruments for the global of wind speeds. determination of sea-surface wind vectors. These highly successful instruments – part of If an instrument were to be constructed that the Active Microwave Instrument (AMI) – were determined the sea-surface backscattering conceived about twenty years ago. During coefficient from a single look direction, the the intervening period, there has been a overlapping nature of the curves would limit considerable evolution in the capabilities of its capabilities to providing a rather coarse spaceborne hardware. estimate of wind speed and no information on wind direction. The earliest successful space- ASCAT is an advanced scatterometer that will fly as part of the borne wind scatterometer, that of Seasat, used payload of the Metop satellites, which in turn form part of the two dual-polarised antennas pointed at 45 and Eumetsat Polar System. It is developed by Dornier Satellitensysteme 135 deg with respect to the satellite’s direction under the leadership of Matra Marconi Space**, the satellite Prime of flight to determine sea-surface scattering Contractor, for ESA. From its polar orbit, ASCAT will measure sea- coefficients from two directions separated by surface winds in two 500 km wide swaths and will achieve global 90 deg. -
+ 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 -
Collision Avoidance Operations in a Multi-Mission Environment
AIAA 2014-1745 SpaceOps Conferences 5-9 May 2014, Pasadena, CA Proceedings of the 2014 SpaceOps Conference, SpaceOps 2014 Conference Pasadena, CA, USA, May 5-9, 2014, Paper DRAFT ONLY AIAA 2014-1745. Collision Avoidance Operations in a Multi-Mission Environment Manfred Bester,1 Bryce Roberts,2 Mark Lewis,3 Jeremy Thorsness,4 Gregory Picard,5 Sabine Frey,6 Daniel Cosgrove,7 Jeffrey Marchese,8 Aaron Burgart,9 and William Craig10 Space Sciences Laboratory, University of California, Berkeley, CA 94720-7450 With the increasing number of manmade object orbiting Earth, the probability for close encounters or on-orbit collisions is of great concern to spacecraft operators. The presence of debris clouds from various disintegration events amplifies these concerns, especially in low- Earth orbits. The University of California, Berkeley currently operates seven NASA spacecraft in various orbit regimes around the Earth and the Moon, and actively participates in collision avoidance operations. NASA Goddard Space Flight Center and the Jet Propulsion Laboratory provide conjunction analyses. In two cases, collision avoidance operations were executed to reduce the risks of on-orbit collisions. With one of the Earth orbiting THEMIS spacecraft, a small thrust maneuver was executed to increase the miss distance for a predicted close conjunction. For the NuSTAR observatory, an attitude maneuver was executed to minimize the cross section with respect to a particular conjunction geometry. Operations for these two events are presented as case studies. A number of experiences and lessons learned are included. Nomenclature dLong = geographic longitude increment ΔV = change in velocity dZgeo = geostationary orbit crossing distance increment i = inclination Pc = probability of collision R = geostationary radius RE = Earth radius σ = standard deviation Zgeo = geostationary orbit crossing distance I. -
Mariner to Mercury, Venus and Mars
NASA Facts National Aeronautics and Space Administration Jet Propulsion Laboratory California Institute of Technology Pasadena, CA 91109 Mariner to Mercury, Venus and Mars Between 1962 and late 1973, NASA’s Jet carry a host of scientific instruments. Some of the Propulsion Laboratory designed and built 10 space- instruments, such as cameras, would need to be point- craft named Mariner to explore the inner solar system ed at the target body it was studying. Other instru- -- visiting the planets Venus, Mars and Mercury for ments were non-directional and studied phenomena the first time, and returning to Venus and Mars for such as magnetic fields and charged particles. JPL additional close observations. The final mission in the engineers proposed to make the Mariners “three-axis- series, Mariner 10, flew past Venus before going on to stabilized,” meaning that unlike other space probes encounter Mercury, after which it returned to Mercury they would not spin. for a total of three flybys. The next-to-last, Mariner Each of the Mariner projects was designed to have 9, became the first ever to orbit another planet when two spacecraft launched on separate rockets, in case it rached Mars for about a year of mapping and mea- of difficulties with the nearly untried launch vehicles. surement. Mariner 1, Mariner 3, and Mariner 8 were in fact lost The Mariners were all relatively small robotic during launch, but their backups were successful. No explorers, each launched on an Atlas rocket with Mariners were lost in later flight to their destination either an Agena or Centaur upper-stage booster, and planets or before completing their scientific missions. -
Cassini RADAR Sequence Planning and Instrument Performance Richard D
IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING, VOL. 47, NO. 6, JUNE 2009 1777 Cassini RADAR Sequence Planning and Instrument Performance Richard D. West, Yanhua Anderson, Rudy Boehmer, Leonardo Borgarelli, Philip Callahan, Charles Elachi, Yonggyu Gim, Gary Hamilton, Scott Hensley, Michael A. Janssen, William T. K. Johnson, Kathleen Kelleher, Ralph Lorenz, Steve Ostro, Member, IEEE, Ladislav Roth, Scott Shaffer, Bryan Stiles, Steve Wall, Lauren C. Wye, and Howard A. Zebker, Fellow, IEEE Abstract—The Cassini RADAR is a multimode instrument used the European Space Agency, and the Italian Space Agency to map the surface of Titan, the atmosphere of Saturn, the Saturn (ASI). Scientists and engineers from 17 different countries ring system, and to explore the properties of the icy satellites. have worked on the Cassini spacecraft and the Huygens probe. Four different active mode bandwidths and a passive radiometer The spacecraft was launched on October 15, 1997, and then mode provide a wide range of flexibility in taking measurements. The scatterometer mode is used for real aperture imaging of embarked on a seven-year cruise out to Saturn with flybys of Titan, high-altitude (around 20 000 km) synthetic aperture imag- Venus, the Earth, and Jupiter. The spacecraft entered Saturn ing of Titan and Iapetus, and long range (up to 700 000 km) orbit on July 1, 2004 with a successful orbit insertion burn. detection of disk integrated albedos for satellites in the Saturn This marked the start of an intensive four-year primary mis- system. Two SAR modes are used for high- and medium-resolution sion full of remote sensing observations by a dozen instru- (300–1000 m) imaging of Titan’s surface during close flybys.