ESA Space Weather STUDY Alcatel Consortium
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Climate Change and Human Health: Risks and Responses
Climate change and human health RISKS AND RESPONSES Editors A.J. McMichael The Australian National University, Canberra, Australia D.H. Campbell-Lendrum London School of Hygiene and Tropical Medicine, London, United Kingdom C.F. Corvalán World Health Organization, Geneva, Switzerland K.L. Ebi World Health Organization Regional Office for Europe, European Centre for Environment and Health, Rome, Italy A.K. Githeko Kenya Medical Research Institute, Kisumu, Kenya J.D. Scheraga US Environmental Protection Agency, Washington, DC, USA A. Woodward University of Otago, Wellington, New Zealand WORLD HEALTH ORGANIZATION GENEVA 2003 WHO Library Cataloguing-in-Publication Data Climate change and human health : risks and responses / editors : A. J. McMichael . [et al.] 1.Climate 2.Greenhouse effect 3.Natural disasters 4.Disease transmission 5.Ultraviolet rays—adverse effects 6.Risk assessment I.McMichael, Anthony J. ISBN 92 4 156248 X (NLM classification: WA 30) ©World Health Organization 2003 All rights reserved. Publications of the World Health Organization can be obtained from Marketing and Dis- semination, World Health Organization, 20 Avenue Appia, 1211 Geneva 27, Switzerland (tel: +41 22 791 2476; fax: +41 22 791 4857; email: [email protected]). Requests for permission to reproduce or translate WHO publications—whether for sale or for noncommercial distribution—should be addressed to Publications, at the above address (fax: +41 22 791 4806; email: [email protected]). The designations employed and the presentation of the material in this publication do not imply the expression of any opinion whatsoever on the part of the World Health Organization concerning the legal status of any country, territory, city or area or of its authorities, or concerning the delimitation of its frontiers or boundaries. -
Potential European Contributions to Europa Lander Mission
The Europa Initiative for ESA’s M5 mission Report to OPAG Michel Blanc, Geraint Jones, Olga Prieto-Ballesteros, Veerle Sterken, Javier Gomez-Elvira, David Mimoun, Adam Masters, Sascha Kempf, Luciano Iess, John Cooper, Zita Martins, Ralph Lorenz, Jérémie lasue, Nicolas André, Bruce Bills, Gael Choblet, Geoff Collins, Philippe Garnier, Kevin Hand, Paul Hartogh, Krishan Khurana, Andrea Longobardo, Katrin Stephan, Federico Tosi, Steve Vance, Tim van Hoolst, Roland Wagner, Frances Westall, Martin Wolverk, William Desprats, Ryan Russell, Georges Balmino, Julien Laurent-Varin and the Europa Initiative team August 11th, 2016 1 EI WORKING SCHEME Europa M5 for an ESA contribution to the Europa Lander mission Initiative Penetrator Contribution to Cubesat? Orbiter or… NASA lander A – GLOBAL GEOPHYSICSMagnetospheric interactions CHARACTERIZE EUROPA AS A COMPLEX DYNAMICAL SYSTEM B – ExosphereOF COUPLED LAYERS(neutrals, dust, plumes) FROM CORE TO PLASMA ENVELOPE THROUGH OCEAN AND CRYOSPHERE dimension RESPONDING TO E – Geophysics (internalJUPITER SYSTEM FORCING: TIDAL, MAGNETOSPHERICstructure, incl. Characterization of the ocean) themes ASTROBIOLOGY CONTRIBUTE TO NASA’s LANDER SCIENCE Science AND PROVIDE AN ADDITIONAL ELEMENT (AWL) As resources permit « Spacecraft » dimension EI contribution to EUROPA LanDer : SubmitteD LOI’s Joint Europa Mission (Blanc/Prieto-Ballesteros) • Baseline: Carrier-Orbiter + lander joint NASA/ESA mission: – P1a: Carrier-Orbiter provided by ESA, operated by NASA; – P1b: Alternative option: Carrier-Orbiter provided and operated by NASA; science platform (+ sub-systems?) provided by ESA – Science platform open to both ESA member states and NASA • Option 1: Augmented surface science: Astrobiology Wet Laboratory (AWL) provided by ESA + Member States to enhance landing site exploration. • Option 2: Augmented orbital science - cubesat released from carrier. -
Planetary Wave Signatures in the Equatorial Atmosphere–Ionosphere System, and Mesosphere- E- and F-Region Coupling
ARTICLE IN PRESS Journal of Atmospheric and Solar-Terrestrial Physics 68 (2006) 509–522 www.elsevier.com/locate/jastp Planetary wave signatures in the equatorial atmosphere–ionosphere system, and mesosphere- E- and F-region coupling M.A. Abdua,Ã, T.K. Ramkumarb, I.S. Batistaa, C.G.M. Bruma, H. Takahashia, B.W. Reinischc, J.H.A. Sobrala aNational Institute for Space Research—INPE, Sao Jose dos Campos, 12245-970 SP, Brazil bNational MST Radar Facility, Gadanki, India cUniversity of Massachusetts, Lowell, USA Available online 8 November 2005 Abstract Upward transport of wave energy and momentum due to gravity, tidal and planetary waves from below and extra- tropics controls the phenomenology of the equatorial atmosphere–ionosphere system. An important aspect of this phenomenology is the development of small- and large-scale structures including thin layers in the mesosphere and E- region, and the formation of wide spectrum plasma structures of the equatorial F-region, widely known as equatorial spread F/plasma bubble irregularities (that are known to have significant impact on space application systems based on trans-ionospheric radio waves propagation). It seems that the effects of tidal and gravity waves at mesospheric and thermospheric heights and their control of ionospheric densities, electric fields and currents are relatively better known than are the effects originating from vertical coupling due to planetary waves. Results from airglow, radar and ionospheric sounding observations demonstrate the existence of significant planetary wave influence on plasma parameters at E- and F- region heights over equatorial latitudes. We present and discuss here some results showing planetary wave oscillations in concurrent mesospheric winds and equatorial electrojet intensity variations in the Indian sector as well as in the mesospheric airglow and F-layer height variation in Brazil. -
Mission to Jupiter
This book attempts to convey the creativity, Project A History of the Galileo Jupiter: To Mission The Galileo mission to Jupiter explored leadership, and vision that were necessary for the an exciting new frontier, had a major impact mission’s success. It is a book about dedicated people on planetary science, and provided invaluable and their scientific and engineering achievements. lessons for the design of spacecraft. This The Galileo mission faced many significant problems. mission amassed so many scientific firsts and Some of the most brilliant accomplishments and key discoveries that it can truly be called one of “work-arounds” of the Galileo staff occurred the most impressive feats of exploration of the precisely when these challenges arose. Throughout 20th century. In the words of John Casani, the the mission, engineers and scientists found ways to original project manager of the mission, “Galileo keep the spacecraft operational from a distance of was a way of demonstrating . just what U.S. nearly half a billion miles, enabling one of the most technology was capable of doing.” An engineer impressive voyages of scientific discovery. on the Galileo team expressed more personal * * * * * sentiments when she said, “I had never been a Michael Meltzer is an environmental part of something with such great scope . To scientist who has been writing about science know that the whole world was watching and and technology for nearly 30 years. His books hoping with us that this would work. We were and articles have investigated topics that include doing something for all mankind.” designing solar houses, preventing pollution in When Galileo lifted off from Kennedy electroplating shops, catching salmon with sonar and Space Center on 18 October 1989, it began an radar, and developing a sensor for examining Space interplanetary voyage that took it to Venus, to Michael Meltzer Michael Shuttle engines. -
Global Ionosphere-Thermosphere-Mesosphere (ITM) Mapping Across Temporal and Spatial Scales a White Paper for the NRC Decadal
Global Ionosphere-Thermosphere-Mesosphere (ITM) Mapping Across Temporal and Spatial Scales A White Paper for the NRC Decadal Survey of Solar and Space Physics Andrew Stephan, Scott Budzien, Ken Dymond, and Damien Chua NRL Space Science Division Overview In order to fulfill the pressing need for accurate near-Earth space weather forecasts, it is essential that future measurements include both temporal and spatial aspects of the evolution of the ionosphere and thermosphere. A combination of high altitude global images and low Earth orbit altitude profiles from simple, in-the-medium sensors is an optimal scenario for creating continuous, routine space weather maps for both scientific and operational interests. The method presented here adapts the vast knowledge gained using ultraviolet airglow into a suggestion for a next-generation, near-Earth space weather mapping network. Why the Ionosphere, Thermosphere, and Mesosphere? The ionosphere-thermosphere-mesosphere (ITM) region of the terrestrial atmosphere is a complex and dynamic environment influenced by solar radiation, energy transfer, winds, waves, tides, electric and magnetic fields, and plasma processes. Recent measurements showing how coupling to other regions also influences dynamics in the ITM [e.g. Immel et al., 2006; Luhr, et al, 2007; Hagan et al., 2007] has exposed the need for a full, three- dimensional characterization of this region. Yet the true level of complexity in the ITM system remains undiscovered primarily because the fundamental components of this region are undersampled on the temporal and spatial scales that are necessary to expose these details. The solar and space physics research community has been driven over the past decade toward answering scientific questions that have a high level of practical application and relevance. -
University of Iowa Instruments in Space
University of Iowa Instruments in Space A-D13-089-5 Wind Van Allen Probes Cluster Mercury Earth Venus Mars Express HaloSat MMS Geotail Mars Voyager 2 Neptune Uranus Juno Pluto Jupiter Saturn Voyager 1 Spaceflight instruments designed and built at the University of Iowa in the Department of Physics & Astronomy (1958-2019) Explorer 1 1958 Feb. 1 OGO 4 1967 July 28 Juno * 2011 Aug. 5 Launch Date Launch Date Launch Date Spacecraft Spacecraft Spacecraft Explorer 3 (U1T9)58 Mar. 26 Injun 5 1(U9T68) Aug. 8 (UT) ExpEloxrpelro r1e r 4 1915985 8F eJbu.l y1 26 OEGxOpl o4rer 41 (IMP-5) 19697 Juunlye 2 281 Juno * 2011 Aug. 5 Explorer 2 (launch failure) 1958 Mar. 5 OGO 5 1968 Mar. 4 Van Allen Probe A * 2012 Aug. 30 ExpPloiorenre 3er 1 1915985 8M Oarc. t2. 611 InEjuxnp lo5rer 45 (SSS) 197618 NAouvg.. 186 Van Allen Probe B * 2012 Aug. 30 ExpPloiorenre 4er 2 1915985 8Ju Nlyo 2v.6 8 EUxpKlo 4r e(rA 4ri1el -(4IM) P-5) 197619 DJuenc.e 1 211 Magnetospheric Multiscale Mission / 1 * 2015 Mar. 12 ExpPloiorenre 5e r 3 (launch failure) 1915985 8A uDge.c 2. 46 EPxpiolonreeerr 4130 (IMP- 6) 19721 Maarr.. 313 HMEaRgCnIe CtousbpeShaetr i(cF oMxu-1ltDis scaatelell itMe)i ssion / 2 * 2021081 J5a nM. a1r2. 12 PionPeioenr e1er 4 1915985 9O cMt.a 1r.1 3 EExpxlpolorerer r4 457 ( S(IMSSP)-7) 19721 SNeopvt.. 1263 HMaalogSnaett oCsupbhee Sriact eMlluitlet i*scale Mission / 3 * 2021081 M5a My a2r1. 12 Pioneer 2 1958 Nov. 8 UK 4 (Ariel-4) 1971 Dec. 11 Magnetospheric Multiscale Mission / 4 * 2015 Mar. -
Marina Galand
Thermosphere - Ionosphere - Magnetosphere Coupling! Canada M. Galand (1), I.C.F. Müller-Wodarg (1), L. Moore (2), M. Mendillo (2), S. Miller (3) , L.C. Ray (1) (1) Department of Physics, Imperial College London, London, U.K. (2) Center for Space Physics, Boston University, Boston, MA, USA (3) Department of Physics and Astronomy, University College London, U.K. 1." Energy crisis at giant planets Credit: NASA/JPL/Space Science Institute 2." TIM coupling Cassini/ISS (false color) 3." Modeling of IT system 4." Comparison with observaons Cassini/UVIS 5." Outstanding quesAons (Pryor et al., 2011) SATURN JUPITER (Gladstone et al., 2007) Cassini/UVIS [UVIS team] Cassini/VIMS (IR) Credit: J. Clarke (BU), NASA [VIMS team/JPL, NASA, ESA] 1. SETTING THE SCENE: THE ENERGY CRISIS AT THE GIANT PLANETS THERMAL PROFILE Exosphere (EARTH) Texo 500 km Key transiLon region Thermosphere between the space environment and the lower atmosphere Ionosphere 85 km Mesosphere 50 km Stratosphere ~ 15 km Troposphere SOLAR ENERGY DEPOSITION IN THE UPPER ATMOSPHERE Solar photons ion, e- Neutral Suprathermal electrons B ion, e- Thermal e- Ionospheric Thermosphere Ne, Nion e- heang Te P, H * + Airglow Neutral atmospheric Exothermic reacAons heang IS THE SUN THE MAIN ENERGY SOURCE OF PLANERATY THERMOSPHERES? W Main energy source: UV solar radiaon Main energy source? EartH Outer planets CO2 atmospHeres Exospheric temperature (K) [aer Mendillo et al., 2002] ENERGY CRISIS AT THE GIANT PLANETS Observed values at low to mid-latudes solsce equinox Modeled values (Sun only) [Aer -
Estimating Random Transverse Velocities in the Fast Solar Wind from EISCAT Interplanetary Scintillation Measurements
c Annales Geophysicae (2002) 20: 1265–1277 European Geophysical Society 2002 Annales Geophysicae Estimating random transverse velocities in the fast solar wind from EISCAT Interplanetary Scintillation measurements A. Canals1, A. R. Breen1, L. Ofman2, P. J. Moran1, and R. A. Fallows1 1Physics Department, University of Wales, Aberystwyth, Wales, UK 2The Catholic University of America and NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA Received: 17 October 2001 – Revised: 21 February 2002 – Accepted: 13 March 2002 Abstract. Interplanetary scintillation measurements can process of constructive and destructive interference change yield estimates of a large number of solar wind parameters, these phase variations into amplitude variations. As the ir- including bulk flow speed, variation in bulk velocity along regularities move out in the solar wind, the effect is to cast a the observing path through the solar wind and random varia- drifting diffraction pattern across the Earth. If the pattern is tion in transverse velocity. This last parameter is of particular sampled using two radio telescopes when the ray paths from interest, as it can indicate the flux of low-frequency Alfven´ the radio source to the antenna lie in the same radial plane – waves, and the dissipation of these waves has been proposed a plane passing through the center of the Sun – then a high as an acceleration mechanism for the fast solar wind. Anal- degree of correlation is present between the scintillation at ysis of IPS data is, however, a significantly unresolved prob- the two sites. The time lag for maximum correlation pro- lem and a variety of a priori assumptions must be made in in- vides a direct estimation of the scintillation drift velocity. -
Information Summaries
TIROS 8 12/21/63 Delta-22 TIROS-H (A-53) 17B S National Aeronautics and TIROS 9 1/22/65 Delta-28 TIROS-I (A-54) 17A S Space Administration TIROS Operational 2TIROS 10 7/1/65 Delta-32 OT-1 17B S John F. Kennedy Space Center 2ESSA 1 2/3/66 Delta-36 OT-3 (TOS) 17A S Information Summaries 2 2 ESSA 2 2/28/66 Delta-37 OT-2 (TOS) 17B S 2ESSA 3 10/2/66 2Delta-41 TOS-A 1SLC-2E S PMS 031 (KSC) OSO (Orbiting Solar Observatories) Lunar and Planetary 2ESSA 4 1/26/67 2Delta-45 TOS-B 1SLC-2E S June 1999 OSO 1 3/7/62 Delta-8 OSO-A (S-16) 17A S 2ESSA 5 4/20/67 2Delta-48 TOS-C 1SLC-2E S OSO 2 2/3/65 Delta-29 OSO-B2 (S-17) 17B S Mission Launch Launch Payload Launch 2ESSA 6 11/10/67 2Delta-54 TOS-D 1SLC-2E S OSO 8/25/65 Delta-33 OSO-C 17B U Name Date Vehicle Code Pad Results 2ESSA 7 8/16/68 2Delta-58 TOS-E 1SLC-2E S OSO 3 3/8/67 Delta-46 OSO-E1 17A S 2ESSA 8 12/15/68 2Delta-62 TOS-F 1SLC-2E S OSO 4 10/18/67 Delta-53 OSO-D 17B S PIONEER (Lunar) 2ESSA 9 2/26/69 2Delta-67 TOS-G 17B S OSO 5 1/22/69 Delta-64 OSO-F 17B S Pioneer 1 10/11/58 Thor-Able-1 –– 17A U Major NASA 2 1 OSO 6/PAC 8/9/69 Delta-72 OSO-G/PAC 17A S Pioneer 2 11/8/58 Thor-Able-2 –– 17A U IMPROVED TIROS OPERATIONAL 2 1 OSO 7/TETR 3 9/29/71 Delta-85 OSO-H/TETR-D 17A S Pioneer 3 12/6/58 Juno II AM-11 –– 5 U 3ITOS 1/OSCAR 5 1/23/70 2Delta-76 1TIROS-M/OSCAR 1SLC-2W S 2 OSO 8 6/21/75 Delta-112 OSO-1 17B S Pioneer 4 3/3/59 Juno II AM-14 –– 5 S 3NOAA 1 12/11/70 2Delta-81 ITOS-A 1SLC-2W S Launches Pioneer 11/26/59 Atlas-Able-1 –– 14 U 3ITOS 10/21/71 2Delta-86 ITOS-B 1SLC-2E U OGO (Orbiting Geophysical -
Radio Scintillation Observations of the Solar Wind - Recent Results from Eiscat and Proposals for a New-Generation System
RADIO SCINTILLATION OBSERVATIONS OF THE SOLAR WIND - RECENT RESULTS FROM EISCAT AND PROPOSALS FOR A NEW-GENERATION SYSTEM A.R. Breen(1), G. Woan(2) (1)University of Wales Aberystwyth, Ceredigion SY23 3BZ, Wales, Email: [email protected] (2)University of Glasgow, Glasgow G12 8QQ, Scotland, Email: [email protected] ABSTRACT the spectral shape measured by a single antenna [2, 3] Measurements of radio scintillation which use the or – with greater accuracy, from the form of the cross- motion of ~100 km scale size density irregularities as spectra of the scintillation patterns measured at two flow tracers for solar wind speed (the technique of widely-separated sites at a time when the raypaths from Interplanetary Scintillation or IPS) have been used to source to antennas lie in a plane radial to the Sun [4, 5]. study the solar wind for many years. Recently Single antenna systems can make many more improvements to analysis methods have transformed observations but velocities derived from multi-site the capabilities of this technique and it has emerged as systems allow more accurate estimates of velocity [6]. a powerful tool for probing regions of the solar wind IPS measurements contain contributions from the which are hard to study by other means - particularly whole of the extended ray-path through the solar the region from ~25 solar radii (R) out to ~100 R. As atmosphere from the distant source to the receiving this is the region in which interaction between streams antenna(s). In earlier studies the inability to distinguish of solar wind and between mass ejections and the between contributions from different regions of the background wind determine the solar wind structure solar wind led to a "blurred" view of solar wind seen at Earth orbit good measurements of this region structure. -
Equatorial Ionospheric Response to Different Estimated Disturbed
PUBLICATIONS Journal of Geophysical Research: Space Physics RESEARCH ARTICLE Equatorial Ionospheric Response to Different Estimated 10.1002/2017JA024265 Disturbed Electric Fields as Investigated Using Sheffield Key Points: University Plasmasphere Ionosphere Model at INPE • The equatorial ionosphere response to different disturbed electric fields is M. A. Bravo1,2 , I. S. Batista1 , J. R. Souza1, and A. J. Foppiano3 analyzed using the SUPIM-INPE model • fi We want to nd the best alternative of 1Instituto Nacional de Pesquisas Espaciais, São José dos Campos, São Paulo, Brazil, 2Now at Universidad de Santiago de fi disturbed electric eld, both 3 temporally and spatially, when E × B Chile, Estación Central, Santiago, Chile, Universidad de Concepción, Concepción, Chile measurements are not available • The comparison between simulations and observations will serve to find a Abstract Good ionospheric modeling is important to understand anomalous effects, mainly during hierarchy among the different types of geomagnetic storm events. Ionospheric electric fields, thermospheric winds, and neutral composition are drifts affected at different degrees, depending on the intensity of the magnetic disturbance which, in turns, affects the electron density distribution at all latitudes. The most important disturbed parameter for the equatorial Supporting Information: ionosphere is the electric field, which is responsible for the equatorial ionization anomaly. Here various • Supporting Information S1 electric field measurements and models are analyzed: (1) measured by the Jicamarca incoherent scatter radar Correspondence to: (ISR), (2) from Jicamarca Unattended Long-Term studies of the Ionosphere and Atmosphere (JULIA) radar, 0 M. A. Bravo, (3) deduced from magnetometers, (4) calculated from the time variations of the F layer height (dh F/dt), [email protected] and (5) deduced from interplanetary electric field determinations. -
A Comparison Study on Thermal Control Techniques for a Nanosatellite Carrying Infrared Science Instrument
ICES-2020-15 A comparison study on thermal control techniques for a nanosatellite carrying infrared science instrument Shanmugasundaram Selvadurai1, Amal Chandran2, Sunil C Joshi3 and Teo Hang Tong Edwin 4 Nanyang Technological University, Singapore, 639798 David Valentini5 Thales Alenia Space, Cannes, 06150, France Friedhelm Olschewski6 University of Wuppertal, 42119 Wuppertal, Germany Based on current technological advancements and forecasts, nanosatellites will be used for both scientific and defense applications leveraging advantages on both development cost and development lifecycle. As nanosatellites become more capable, there is an increase in demand for high power applications which makes the missions complex from implementing a proper thermal control system (TCS) to dissipate the huge waste heat generated. One of the applications for nanosatellites is advanced infrared imaging for both scientific and military applications. ARCADE (Atmospheric coupling and Dynamics Explorer), a 27U satellite is being developed by Satellite Research Centre (SaRC) at Nanyang Technological University (NTU) for scientific objectives. The main payload AtmoLITE needs a detector cool down at -30°C and to meet this requirement, an appropriate classical TCS is chosen and described in this paper. Nanosatellites carrying infrared, cryogenic or other scientific instruments that need active cooling, should be equipped with a proper TCS within the highly constrained available volume. Another objective of this study is to compare the existing TCS for nanosatellites and adopt a suitable and efficient TCS for a scientific nanosatellite mission carrying a generic science instrument that needs an active cooling of up to 95K. TCS using Heat pipes (HP), single-phase mechanically pumped fluid loop (SMPFL), and two-phase mechanically pumped fluid loop systems (2ΦMPFL) have been extensively used only by larger satellites.