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Observation of Pc 3/5 Magnetic Pulsations Around the Cusp at Mid Altitude
1 OBSERVATION OF PC 3/5 MAGNETIC PULSATIONS AROUND THE CUSP AT MID ALTITUDE Liu Yonghua(1), Liu Ruiyuan(1), B. J. Fraser(2), S. T. Ables(2), Xu Zhonghua(1), Zhang Beichen(1), Shi Jiankui(3), Liu Zhenxing(3), Huang Dehong(1), Hu Zejun(1), Chen Zhuotian(1), Wang Xiao(3), Malcolm Dunlop(4), A. Balogh(5) (1) Polar Research Institute of China, 451 Jinqiao Rd., Shanghai 200136, P. R. CHINA, [email protected] (2) The University of Newcastle, University Drive, Callaghan NSW 2308, AUSTRALIA, [email protected] (3)The Center of Space Science & Applied Research, Chinese Academy of Science, Post Box8701, Beijing 100080, jkshi@@center.cssar.ac.cn (4) The Rutherford Appleton Laboratory, Chilton, DIDCOT, Oxfordshire, OX11 0QX, UK, [email protected] (5)Space and Atmospheric Physics Group, Imperial College, London, [email protected] ABSTRACT transmitted straightforwardly from solar wind to the ionosphere (Bolshakova & Troitskaia, 1984). So far most Since launched in year 2000 the Cluster mission has research work on such topic are on basis of observation passed the region around the cusp at mid-altitude (~6Re) at ground or/and data from satellite located in the for many times, where ULF wave activities are rich in. upstream of solar wind or in the magnetosheath. To my From 0800 to 1300UT on October 30 2002 the Cluster knowledge, few authors take a study based on the spacecrafts ran along an orbit of southern cusp- measurement at the mid-altitude of the cusp. It seems plasmasphere-northern cusp that provides an excellent reasonable to assume that such a measurement be a direct observation of ULF waves in dayside magnetosphere. -
OUFTI-1 Environmental Impact Assessment
Date: 11/02/2016 Issue: 1 Rev: 1 Page: 1 of 11 OUFTI-1 Environmental Impact Assessment Reference 3_OUF_ENV_IMPACT_1.0 Issue/Rev Issue 1 Rev 0 Date 11/02/2016 Distribution OUFTI-1 team OUFTI-1 Environmental Impact Assessment Date: 11/02/2016 Issue: 1 Rev: 1 Page: 2 of 11 AUTHORS Name Email Telephone X. Werner [email protected] +32 4 366 37 38 S. De Dijcker [email protected] +32 4 366 37 38 RECORD OF REVISIONS Iss/Rev Date Author Section/page Change description 1/0 11/02/2016 X.Werner, All Initial issue S. De Dijcker Copyright University of Liège [2016]. OUFTI-1 Environmental Impact Assessment Date: 11/02/2016 Issue: 1 Rev: 1 Page: 3 of 11 TABLE OF CONTENTS Authors ....................................................................................................................................... 2 Record of revisions ..................................................................................................................... 2 1. Activities and Objectives ................................................................................................... 4 1.1. Project description ....................................................................................................... 4 1.2. Soyuz launch vehicle ................................................................................................... 5 1.3. Arianespace ................................................................................................................. 7 1.4. Conclusion .................................................................................................................. -
Laser Retroreflectors for Insight and an International Mars Geophysical Network (MGN)
50th Lunar and Planetary Science Conference 2019 (LPI Contrib. No. 2132) 1492.pdf Laser Retroreflectors for InSight and an International Mars Geophysical Network (MGN). S. Dell’Agnello1, G.O. Delle Monache1, L. Porcelli1,2, M. Tibuzzi1, L. Salvatori1, C. Mondaini1, M. Muccino1, L. Ioppi1, O. Luongo1, M. Petrassi1, G. Bianco1,3, R. Vittori1,4, W.B. Banerdt5, J.F. Grinblat5, C. Benedetto3, F. Pasquali3, R. Mugnuolo3, D.C. Gruel5, J.L.Vago6 and P. Baglioni6. 1Istituto Nazionale di Fisica Nucleare–Laboratori Nazionali di Frascati (INFN–LNF), Via E. Fermi 40, 00044, Frascati, Italy ([email protected]); 2Dipartimento di Fisica, Università della Calabria (UniCal), Via P. Bucci, 87036, Arcavacata di Rende, Italy; 3Agenzia Spaziale Italiana– Centro di Geodesia Spaziale “Giuseppe Colombo” (ASI–CGS), Località, Terlecchia 75100, Matera, Italy; 4Italian Air Force, Rome, Italy, ASI and Embassy of Italy in Washington DC; 5NASA–Jet Propulsion Laboratory (JPL), California Institute of Technology, Pasadena, CA 91109, USA; 6ESA–ESTEC, Noordwijk, The Netherlands. Abstract. There are laser retroreflectors on the Moon, of the INFN-ASI Affiliation-Association to NASA- but there were no laser retroreflectors on Mars until the SSERVI sservi.nasa.gov) is shown in the figure below. NASA InSight mission [1][2] landed and started oper- ating successfully on the surface of the red planet on Nov. 26, 2018. The ESA ExoMars Schiaparelli mis- sion, which unfortunately failed Mars landing in 2016, was carrying a laser retroreflector like InSight [3]. These instruments are positioned by measuring the time-of-flight of short laser pulses, the so-called “laser ranging” technique (for details on satellite/lunar laser ranging and altimetry see https://ilrs.gsfc.nasa.gov). -
Planned Yet Uncontrolled Re-Entries of the Cluster-Ii Spacecraft
PLANNED YET UNCONTROLLED RE-ENTRIES OF THE CLUSTER-II SPACECRAFT Stijn Lemmens(1), Klaus Merz(1), Quirin Funke(1) , Benoit Bonvoisin(2), Stefan Löhle(3), Henrik Simon(1) (1) European Space Agency, Space Debris Office, Robert-Bosch-Straße 5, 64293 Darmstadt, Germany, Email:[email protected] (2) European Space Agency, Materials & Processes Section, Keplerlaan 1, 2201 AZ Noordwijk, Netherlands (3) Universität Stuttgart, Institut für Raumfahrtsysteme, Pfaffenwaldring 29, 70569 Stuttgart, Germany ABSTRACT investigate the physical connection between the Sun and Earth. Flying in a tetrahedral formation, the four After an in-depth mission analysis review the European spacecraft collect detailed data on small-scale changes Space Agency’s (ESA) four Cluster II spacecraft in near-Earth space and the interaction between the performed manoeuvres during 2015 aimed at ensuring a charged particles of the solar wind and Earth's re-entry for all of them between 2024 and 2027. This atmosphere. In order to explore the magnetosphere was done to contain any debris from the re-entry event Cluster II spacecraft occupy HEOs with initial near- to southern latitudes and hence minimise the risk for polar with orbital period of 57 hours at a perigee altitude people on ground, which was enabled by the relative of 19 000 km and apogee altitude of 119 000 km. The stability of the orbit under third body perturbations. four spacecraft have a cylindrical shape completed by Small differences in the highly eccentric orbits of the four long flagpole antennas. The diameter of the four spacecraft will lead to various different spacecraft is 2.9 m with a height of 1.3 m. -
Church of the Brethren May Meet Hrre In
' ' , s i * Take inventory of your printed” sup One word can tell the Btory of con plies; If you need anything, the - tinued business activity in the com - j ■ ' Times stands ready to give munity—Advertising. vi:;/ you Bervice, • . AND THE SJIOUE TIMES FOUR CENTS /,-;t VOL. LX . No. 33 OCEAN GROVE, NEW JERSEY, FRIDAY, AUGUST 16, 1935 - / ' : $ THOMSON GETS ‘MARTHA" IS BIBLE LESSON HOTEL MEN WANT CHURCH 7,500 HEAR BISHOP MOUZON Mrs. Gertrude Brown To Teach At OF THE BRETHREN RARE SOUVENIRS St; Paul’s MORE PUBLICITY in Au ditoriu m sermons “Martha” is the Bible class les MAY MEET HRRE IN 1936 THREE ANNIVERSARY: MEMOS son for .the coming Sundny. Text, WILL REQUEST LARGER BUD “Jesus loved! Martha and her sister ARE PRESENTED and! Lazarus,” John,: 11:5: Read GET APPROPRIATION. Preacher Sees Chance For Uniting of Three Luke, 10\38-42 and John, VI '.17-28. National Convention Would Bring Eight Thou Sixth Founders’ Day, Stokes Gold Dr, Francis Harvey Green will be Appoint Nominating Committee Branches of Methodist Church—Prays For en Wedding and Dr. Ballard’s the teacher 'at the|. Auditorium For Report at September Meet sand Delegates for Eight Days—Dr. Hen Bible Class,, at" 2.30. .Written Ques Birthday Arc Noted In Special ing of Ocean Grove Hotel As Kingdom of God and Revival of Hope, tions will be answered at the begin son Offers Buildings for Sessions—Ar Announcements. ning of theperiod. sociation. Endorse Play-Ground Faith and Love— Gives His Definition of Three precious documents have The Assembly BiblejClhss, which D rive/ rangements Committee Decides Today. -
Rapid Development of Navigation Payloads for Galileo Full Operational Capability
Changing the economics of space RAPID DEVELOPMENT OF NAVIGATION PAYLOADS FOR GALILEO FULL OPERATIONAL CAPABILITY Alex da Silva Curiel Dubai, January 2011 SSTL - the company UK-based satellite manufacturing company owned by EADS Astrium NV (99%) and the University of Surrey (1%) • Formed in 1985, the Company now employs >320 staff and occupies dedicated facilities in Surrey, Kent & Colorado 2 A history of success 34 Satellites completed – c.200 satellite years on-orbit experience 10 Further satellites (35-43) - currently being prepared for launch 18 payloads in progress (4 optical, 14 navigation) HERITAGE: Flight proven - low risk RESULTS: All projects fixed price, delivered on-time and on-budget SUCCESS: Very high mission success – 100% mission success in last 10 years – proven equipment and full redundancy CUSTOMERS: Variety of customers including many “blue chip” operators as well as 15 successful training programmes 3 What is Galileo? Galileo is a joint initiative of the European Commission (EC) and the European Space Agency (ESA). Galileo will be Europe’s own global navigation satellite system, providing a highly accurate, guaranteed global positioning service under civilian control. It will be inter-operable with GPS and GLONASS, the two other global satellite navigation systems 4 Galileo Services • Galileo offers 5 services: – Open signal, dual frequency, mass market use – Commercial signal, better accuracy, service guarantee – authenticated data – Safety-of-Life signal, high integrity service certified for use in safety related -
Design for Demise Analysis for Launch Vehicles
A first design for demise analysis for launch vehicles Henrik Simon, Stijn Lemmens Space debris: Inactive, manmade objects in space Source: ESA Overview Introduction Fundamentals Modelling approach Results and discussion Summary and outlook What is the motivation and task? INTRODUCTION Motivation . Mitigation: Prevention of creation and limitation of long-term presence . Guidelines: LEO removal within 25 years . LEO removal within 25 years after mission end . Casualty risk limit for re-entry: 1 in 10,000 Rising altitude Decay & re-entry above 2000 km Source: NASA Source: NASA Solution: Design for demise Source: ESA Scope of the thesis . Typical design of upper stages . General Risk assessment . Design for demise solutions to reduce the risk ? ? ? Risk A Risk B Risk C Source: CNES How do we assess the risk and simulate the re-entry? FUNDAMENTALS Fundamentals: Ground risk assessment Ah = + 2 Ai � ℎ = =1 � Source: NASA Source: NASA 3.5 m 5.0 m 2 2 ≈ ≈ Fundamentals: Re-entry simulation tools SCARAB: Spacecraft-oriented approach . CAD-like modelling . 6 DoF flight dynamics . Break-up / fragmentation computed How does a rocket upper stage look like? MODELLING Modelling approach . Research on typical design: . Elongated . Platform . Solid Rocket Motor . Lack of information: . Create common intersection . Deliberately stay top-level and only compare effects Modelling approach Modelling approach 12 Length [m] 9 7 5 3 2 150 300 500 700 800 1500 2200 Mass [kg] How much is the risk and how can we reduce it? SIMULATIONS Example of SCARAB re-entry simulation 6x Casualty risk of all reference cases Typical survivors Smaller Smaller fragments fragments Pressure tanks Pressure tanks Main tank Engine Main structure + tanks Design for Demise . -
Enabling Interstellar Probe
This article appeared in a journal published by Elsevier. The attached copy is furnished to the author for internal non-commercial research and education use, including for instruction at the authors institution and sharing with colleagues. Other uses, including reproduction and distribution, or selling or licensing copies, or posting to personal, institutional or third party websites are prohibited. In most cases authors are permitted to post their version of the article (e.g. in Word or Tex form) to their personal website or institutional repository. Authors requiring further information regarding Elsevier’s archiving and manuscript policies are encouraged to visit: http://www.elsevier.com/copyright Author's personal copy Acta Astronautica 68 (2011) 790–801 Contents lists available at ScienceDirect Acta Astronautica journal homepage: www.elsevier.com/locate/actaastro Enabling interstellar probe Ralph L. McNutt Jr.a,n, Robert F. Wimmer-Schweingruber b,1, the International Interstellar Probe Team a The Johns Hopkins University Applied Physics Laboratory, 11100 Johns Hopkins Road, M/S MP3-E128, Laurel, MD 20723, USA b Institut fuer Experimentelle und Angewandte Physik, University of Kiel, Leibnizstrasse 11, D-24118 Kiel, Germany article info abstract Article history: The scientific community has advocated a scientific probe to the interstellar medium for Received 15 February 2010 over 30 years. While the Voyager spacecraft have passed through the termination shock Received in revised form of the solar wind, they have limited lifetimes as their radioisotope power supplies 16 June 2010 decay. It remains unclear whether they can reach the heliopause, the boundary between Accepted 2 July 2010 shocked solar wind and interstellar plasmas, and, in any case, they will not reach the Available online 17 August 2010 undisturbed interstellar medium. -
Chapter 1 Introduction
Chapter 1 Introduction The magnetosheath lies between the bow shock and the magnetopause and is formed by the deflected, heated, and decelerated solar wind with a minor magnetospheric plasma component. The terrestrial magnetosheath field and flow structure have been extensively studied because they affect the transfer of mass, momentum, and energy between the solar wind and the Earth’s magnetosphere. When magnetic shear across the magnetopause is high and dayside reconnection is occurring, the coupling between the solar wind and the magnetosphere is substantially enhanced relative to periods when there is no reconnection [ Paschmann et al ., 1979; Sonnerup et al ., 1981]. The magnetosphere becomes energized leading to phenomena such as the aurora. When the terrestrial magnetosphere is closed, or when the solar wind dynamic pressure is sufficiently high, magnetic field lines pile up near the magnetopause forcing out the normally resident plasma leading to the formation of a plasma depletion layer. Because of the limited amount of available data, the Jovian magnetosheath has been less extensively studied than the Earth’s magnetosheath. Factors that control the size, shape, and rigidity of the magnetosheath are much different at Jupiter and the Earth. At Jupiter the solar wind dynamic pressure is down by more than an order of magnitude and the Alfvén Mach number is nearly double the mean values observed near Earth. Furthermore, at Jupiter the force balance at the magnetopause is not well approximated by balancing the contributions of the external solar wind dynamic pressure against the internal magnetic pressure. Magnetospheric energetic particles, thermal plasma, and dynamic pressure associated with the rapid rotation of Jupiter provide non-negligible contributions to the internal pressure [ Smith et al ., 1974]. -
ASTRONOMY and ASTROPHYSICS Seismology of Δ Scuti Stars in the Praesepe Cluster II
Astron. Astrophys. 338, 511–520 (1998) ASTRONOMY AND ASTROPHYSICS Seismology of δ Scuti stars in the Praesepe cluster II. Identification of radial modes and their associated stellar parameters M.M. Hernandez´ 1?,F.Perez´ Hernandez´ 1, E. Michel2, J.A. Belmonte1, M.J. Goupil2, and Y. Lebreton2 1 Instituto de Astrof´ısica de Canarias, E-38200 La Laguna, Tenerife, Spain 2 DASGAL, URA CNRS 335, Observatoire de Paris, F-92195 Meudon, France Received 5 January 1998 / Accepted 20 July 1998 Abstract. An analysis based on a comparison between obser- Several attempts have been made to obtain stellar informa- vations and stellar models has been carried out to identify radial tion from δ Scuti stars (e.g. Mangeney et al. 1991; Goupil et modes of oscillations in several multi-periodic δ Scuti stars of al. 1993; Perez´ Hernandez´ et al. 1995; Guzik & Bradley 1995). the Praesepe cluster (BU, BN, BW and BS Cnc). The assump- All have had to face the absence of the greater part of the the- tion that all the stars considered have common parameters, such oretical modes in the observed spectrum. Noise level, selection as metallicity, distance or age, is imposed as a constraint. Even mechanisms, geometrical effects and also mutual interference so, there is a large number of possible solutions, partially caused between very close modes (as recently illustrated by Belmonte by the rotational effects on the pulsation frequencies and on the et al. 1997) contribute towards explaining this phenomenon. stars’ positions in the HR diagram, which need to be parame- Even in the case of a large number of detected modes, such as terized. -
NASA Satellite Laser Ranging Program
NASA Satellite Laser Ranging Program NASA Goddard Space Flight Center Ron Sebeny MOBLAS 4 Station Manager December 9, 2011 What is Satellite Laser Ranging? Map of International Laser Ranging Service (ILRS) Network Metsahovi PotsdamRiga Mendeleevo Borowiec Komsomolsk Herstmonceux Wettzell Zimmerwald Graz Simiez Changchun Grasse (2) Maidanak Cagliari KtiKatzive lly Beijing Greenbelt San Fernando Matera Keystone (4) Monument Peak Riyadh Wuhan Simosato McDonald Helwan Shanghai Kunming Santiago de Cuba Haleakala Arequipa South Africa Tahiti Yarragadee CiConcepcion Mt. Stromlo Legend: NASA NASA Partner International Cooperating Project: Satellite Laser Ranging (SLR) NASA SLR Network: • Eight Ground Stations • Part of International Laser Ranging Service (ILRS) • Data operations – Data reception, processing, and analysis – Orbit determination – Acquisition generation – Data Archive Laser Ranging Satellite Missions (past/present) : • Geodetic: – Larets, Starlette, Stella, Ajisai, LAGEOS-1, LAGEOS-2, Etalon-1, Etalon-2, BLITS • Earth Sensing/Technology Demonstration: – CHAMP, GRACE-A, GRACE-B, ICESat, Jason-1, Jason-2, Envisat, ERS-2, ETS-8, Beacon-C, TerraSAR-X, SOHLA-1, GOCE, CryoSat-2 • NitiNavigation: – GLONASS-102, GLONASS-115, GLONASS-120, GPS-35, GPS-36, GIOVE-A, GIOVE-B, Compass-M1 4 MOBLAS 4 Monument Peak MOBLAS 4 Monument Peak What is LRO? • Lunar Reconnaissance Orbiter – NASA’s Mission to map the moons surface with highest accuracy to date (highly successful thus far) • Laser ranggging to LRO will imp rove the scientific value of the -
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GIOVE-A’S FREGAT DISPOSAL ASSESSMENT D. Navarro-Reyes(1), R. Zandbergen(2), D. Escobar(3) (1)ESA/ESTEC, Keplerlaan 1, 2200 AG Noordwijk, The Netherlands, Email: [email protected] (2) ESA/ESOC, Robert-Bosch-Str. 5, D-64293 Darmstadt, Germany, Email: [email protected] (3)GMV at ESOC, ESA/ESOC Robert-Bosch-Str. 5, D-64293 Darmstadt, Germany, Email: [email protected] ABSTRACT dedicated stations deployed around the world. The Galileo constellation is defined as a Walker 27/3/1 and is composed of 3 equally-spaced orbital planes with a Galileo will be Europe’s own global navigation satellite nominal inclination of 56 degrees and a semi-major axis system, providing a highly accurate, guaranteed global of 29,600 km. Each plane will contain nine equally- positioning service under civilian control. Following the spaced satellites plus a spare satellite. The first launches approval of Galileo in 1999, a demonstration element are foreseen in 2010, with the full constellation was added – the Galileo System Test Bed (GSTB) with deployed by end 2013. the GIOVE-A and GIOVE-B satellites – to allow early experimentation with the navigation signals and services Following the approval of Galileo in 1999, a before committing to the final constellation design. demonstration element was added – the Galileo System Test Bed (GSTB) with the GIOVE-A and GIOVE-B GIOVE-A (launched on 28 Dec 2005) and GIOVE-B satellites, whose mission was: (launched on 26 April 2008) were injected in the Galileo operational orbit (semi-major axis 29600 km, x To secure use of the frequencies allocated by the circular orbit, inclination 56 degrees) by direct injection International Telecommunications Union (ITU) for with Soyuz/FREGAT launch vehicle.