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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. -
SATELLITES at WORK Space in the Seventies
SaLf ILMITRATBONS REPROMhdONkp N BLACK ANd WHiT? SATELLITES AT WORK Space in the Seventies 4 (SPACE IN N72-13 8 6 6 (NASA-EP-8 ) SATELLITES AT WORK THE SEVENTIES) W.R. Corliss (NASA) Jun. 1971 29 p CSCL 22B Unclas Reproduced by G3/31 11470 NATIONAL TECHNICAL u. INFORMATION SERVICE U S Department of Commerce Springfield VA 22151 J National Aeronautics and Space Administration SPACE IN THE SEVENTIES Man has walked on the Moon, made scientific observations there, and brought back to Earth samples of the lunar surface. Unmanned scientific spacecraft have probed for facts about matter, radiation and magnetism in space, and have collected data relating to the Moon, Venus, Mars, the Sun and some of the stars, and reported their findings to ground stations on Earth. Spacecraft have been put into orbit around the Earth as weather observation stations, as communications relay stations for a world-wide telephone and television network, and as aids to navigation. In addition, the space program has accelerated the advance of technology for science and industry, contributing many new ideas, processes and materials. All this took place in the decade of the Sixties. What next? What may be expected of space exploration in the Seventies? NASA has prepared a series of publications and motion pictures to provide a look forward to SPACE IN THE SEVENTIES. The topics covered in this series include: Earth orbital science; planetary exploration; practical applications of satellites; technology utilization; man in space; and aeronautics. SPACE IN THE SEVENTIES presents the planned programs of NASA for the coming decade. -
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. -
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 -
Aurorae and Airglow Results of the Research on the International
VARIATIONS IN THE Ha EMISSION AND HYDROGEN DISTRIBUTION IN THE UPPER ATMOSPHERE AND THE GEOCORONA L. M. Fishkova and N. M. Martsvaladze ABSTRACT: The variations in intensity of the hydrogen emission showed a maximum during the minimum of solar activity in 1962-1963. The distribution of hydrogen content at altitudes from 400 to 1300 km was calculated. It in creased during the period of the minimum in the solar cycle. No concentration of H, emis sion around the ecliptic was detected. During the International Quiet Solar Year, spectral observa tions of the intensity of H, emission 6563 a in the airglow spec trum were conducted in Abastumani [l, 21. Continuous observations from f ,hyleighs "w 1953 to 1964 provided for finding the annual variations in H, intensity related to the cycle of solar activ ity (Fig. 1). With a decrease in solar activity, the H, intensity increased and reached a maximum in 1962-1963 while, from 1964, it again began to decrease. Such a variation in the H, intensity can be explained by the variations in Fig. 1. Variations in the the amount of hydrogen during the Average Annual Intensities solar cycle. With a decrease in of H, Emission During the the solar activity, the temperature Cycle of Solar Activity. of the thermopause decreases , which then leads to an increase in the concentration of atomic hydrogen in the exosphere and the geocorona. For example, theoretical calculations [SI show that a change in temperature of the themopause from - 2000 to - 1000° K during the transition from maximum to minimum solar activity can bring about an increase in the hydrogen concentration at altitudes of 500-3000 km, almost by one order of magnitude. -
A Tenuous, Collisional Atmosphere on Callisto
A tenuous, collisional atmosphere on Callisto Shane R. Carberry Mogana;b;c;∗, Orenthal J. Tuckerd, Robert E. Johnsone;f , Audrey Vorburgerg, Andre Gallig, Benoit Marchandh, Angelo Tafunii, Sunil Kumarc, Iskender Sahina, Katepalli R. Sreenivasana;b;f aTandon School of Engineering, New York University, New York, USA; bCenter for Space Sci- ence, New York University Abu Dhabi, Abu Dhabi, UAE; cDivision of Engineering, New York University Abu Dhabi, Abu Dhabi, UAE; dNASA Goddard Space Flight Center, Maryland, USA; eUniversity of Virginia, Virginia, USA; f Physics Department, New York University, New York, USA; gPhysikalisches Institut, University of Bern, Bern, Switzerland; hHigh Per- formance and Research Computing Center, New York University Abu Dhabi, UAE; iSchool of Applied Engineering and Technology, New Jersey Institute of Technology, New Jersey, USA Abstract A simulation tool which utilizes parallel processing is developed to describe molecu- lar kinetics in 2D, single- and multi-component atmospheres on Callisto. This expands on our previous study on the role of collisions in 1D atmospheres on Callisto composed of radiolytic products (Carberry Mogan et al., 2020) by implementing a temperature gradient from noon to midnight across Callisto's surface and introducing sublimated water vapor. We compare single-species, ballistic and collisional O2,H2 and H2O at- mospheres, as well as an O2+H2O atmosphere to 3-species atmospheres which contain H2 in varying amounts. Because the H2O vapor pressure is extremely sensitive to the surface temperatures, the density drops several orders of magnitude with increasing distance from the subsolar point, and the flow transitions from collisional to ballistic accordingly. In an O2+H2O atmosphere the local temperatures are determined by H2O near the subsolar point and transition with increasing distance from the subsolar point to being determined by O2. -
The Space-Based Global Observing System in 2010 (GOS-2010)
WMO Space Programme SP-7 The Space-based Global Observing For more information, please contact: System in 2010 (GOS-2010) World Meteorological Organization 7 bis, avenue de la Paix – P.O. Box 2300 – CH 1211 Geneva 2 – Switzerland www.wmo.int WMO Space Programme Office Tel.: +41 (0) 22 730 85 19 – Fax: +41 (0) 22 730 84 74 E-mail: [email protected] Website: www.wmo.int/pages/prog/sat/ WMO-TD No. 1513 WMO Space Programme SP-7 The Space-based Global Observing System in 2010 (GOS-2010) WMO/TD-No. 1513 2010 © World Meteorological Organization, 2010 The right of publication in print, electronic and any other form and in any language is reserved by WMO. Short extracts from WMO publications may be reproduced without authorization, provided that the complete source is clearly indicated. Editorial correspondence and requests to publish, reproduce or translate these publication in part or in whole should be addressed to: Chairperson, Publications Board World Meteorological Organization (WMO) 7 bis, avenue de la Paix Tel.: +41 (0)22 730 84 03 P.O. Box No. 2300 Fax: +41 (0)22 730 80 40 CH-1211 Geneva 2, Switzerland E-mail: [email protected] FOREWORD The launching of the world's first artificial satellite on 4 October 1957 ushered a new era of unprecedented scientific and technological achievements. And it was indeed a fortunate coincidence that the ninth session of the WMO Executive Committee – known today as the WMO Executive Council (EC) – was in progress precisely at this moment, for the EC members were very quick to realize that satellite technology held the promise to expand the volume of meteorological data and to fill the notable gaps where land-based observations were not readily available. -
Temporal Variability of Atomic Hydrogen from the Mesopause To
PUBLICATIONS Journal of Geophysical Research: Space Physics RESEARCH ARTICLE Temporal Variability of Atomic Hydrogen From 10.1002/2017JA024998 the Mesopause to the Upper Thermosphere Key Points: Liying Qian1 , Alan G. Burns1 , Stan S. Solomon1 , Anne K. Smith2 , Joseph M. McInerney1 , • In the mesopause, hydrogen density is 3 1,2 1 3 1,2 higher in summer than in winter, and Linda A. Hunt , Daniel R. Marsh , Hanli Liu ,MartinG.Mlynczak , and Francis M. Vitt higher at solar minimum than at 1 2 solar maximum High Altitude Observatory, National Center for Atmospheric Research, Boulder, CO, USA, Atmospheric Chemistry 3 • MSIS exhibits reverse seasonal Observations and Modeling Laboratory, National Center for Atmospheric Research, Boulder, CO, USA, NASA Langley variation than WACCM and SABER Research Center, Hampton, VA, USA do in the mesopause region • In the upper thermosphere, H is higher at solar minimum than solar Abstract We investigate atomic hydrogen (H) variability from the mesopause to the upper thermosphere, maximum, higher in winter than summer, and also higher at night on time scales of solar cycle, seasonal, and diurnal, using measurements made by the Sounding of the than day Atmosphere using Broadband Emission Radiometry (SABER) instrument on the Thermosphere Ionosphere Mesosphere Energetics Dynamics satellite, and simulations by the National Center for Atmospheric Research Whole Atmosphere Community Climate Model-eXtended (WACCM-X). In the mesopause region (85 to Correspondence to: 95 km), the seasonal and solar cycle variations of H simulated by WACCM-X are consistent with those from L. Qian, SABER observations: H density is higher in summer than in winter, and slightly higher at solar minimum than [email protected] at solar maximum. -
Short-Term Variability and Mass Loss in Be Stars I
A&A 588, A56 (2016) Astronomy DOI: 10.1051/0004-6361/201528026 & c ESO 2016 Astrophysics Short-term variability and mass loss in Be stars I. BRITE satellite photometry of η and μ Centauri D. Baade1, Th. Rivinius2, A. Pigulski3,A.C.Carciofi4, Ch. Martayan2,A.F.J.Moffat5,G.A.Wade6,W.W.Weiss7, J. Grunhut1, G. Handler8,R.Kuschnig9,7,A.Mehner2,H.Pablo5,A.Popowicz10,S.Rucinski11, and G. Whittaker11 1 European Organisation for Astronomical Research in the Southern Hemisphere (ESO), Karl-Schwarzschild-Str. 2, 85748 Garching, Germany e-mail: [email protected] 2 European Organisation for Astronomical Research in the Southern Hemisphere (ESO), Casilla 19001, Santiago 19, Chile 3 Astronomical Institute, Wrocław University, Kopernika 11, 51-622 Wrocław, Poland 4 Instituto de Astronomia, Geofísica e Ciências Atmosféricas, Universidade de São Paulo, Rua do Matão 1226, Cidade Universitária, 05508-900 São Paulo, SP, Brazil 5 Département de physique and Centre de Recherche en Astrophysique du Québec (CRAQ), Université de Montréal, CP 6128, Succ. Centre-Ville, Montréal, Québec, H3C 3J7, Canada 6 Department of Physics, Royal Military College of Canada, PO Box 17000, Stn Forces, Kingston, Ontario K7K 7B4, Canada 7 Institute of Astronomy, University of Vienna, Universitätsring 1, 1010 Vienna, Austria 8 Nicolaus Copernicus Astronomical Center, ul. Bartycka 18, 00-716 Warsaw, Poland 9 Department of Physics and Astronomy, University of British Columbia, Vancouver, BC V6T1Z1, Canada 10 Institute of Automatic Control, Silesian University of Technology, Gliwice, Poland 11 Department of Astronomy & Astrophysics, University of Toronto, 50 St. George St, Toronto, Ontario, M5S 3H4, Canada Received 21 December 2015 / Accepted 1 February 2016 ABSTRACT Context. -
The History Problem: the Politics of War
History / Sociology SAITO … CONTINUED FROM FRONT FLAP … HIRO SAITO “Hiro Saito offers a timely and well-researched analysis of East Asia’s never-ending cycle of blame and denial, distortion and obfuscation concerning the region’s shared history of violence and destruction during the first half of the twentieth SEVENTY YEARS is practiced as a collective endeavor by both century. In The History Problem Saito smartly introduces the have passed since the end perpetrators and victims, Saito argues, a res- central ‘us-versus-them’ issues and confronts readers with the of the Asia-Pacific War, yet Japan remains olution of the history problem—and eventual multiple layers that bind the East Asian countries involved embroiled in controversy with its neighbors reconciliation—will finally become possible. to show how these problems are mutually constituted across over the war’s commemoration. Among the THE HISTORY PROBLEM THE HISTORY The History Problem examines a vast borders and generations. He argues that the inextricable many points of contention between Japan, knots that constrain these problems could be less like a hang- corpus of historical material in both English China, and South Korea are interpretations man’s noose and more of a supportive web if there were the and Japanese, offering provocative findings political will to determine the virtues of peaceful coexistence. of the Tokyo War Crimes Trial, apologies and that challenge orthodox explanations. Written Anything less, he explains, follows an increasingly perilous compensation for foreign victims of Japanese in clear and accessible prose, this uniquely path forward on which nationalist impulses are encouraged aggression, prime ministerial visits to the interdisciplinary book will appeal to sociol- to derail cosmopolitan efforts at engagement. -
ARIEL – 13Th Appleton Space Conference PLANETS ARE UBIQUITOUS
Background image credit NASA ARIEL – 13th Appleton Space Conference PLANETS ARE UBIQUITOUS OUR GALAXY IS MADE OF GAS, STARS & PLANETS There are at least as many planets as stars Cassan et al, 2012; Batalha et al., 2015; ARIEL – 13th Appleton Space Conference 2 EXOPLANETS TODAY: HUGE DIVERSITY 3700+ PLANETS, 2700 PLANETARY SYSTEMS KNOWN IN OUR GALAXY ARIEL – 13th Appleton Space Conference 3 HUGE DIVERSITY: WHY? FORMATION & EVOLUTION PROCESSES? MIGRATION? INTERACTION WITH STAR? Accretion Gaseous planets form here Interaction with star Planet migration Ices, dust, gas ARIEL – 13th Appleton Space Conference 4 STAR & PLANET FORMATION/EVOLUTION WHAT WE KNOW: CONSTRAINTS FROM OBSERVATIONS – HERSCHEL, ALMA, SOLAR SYSTEM Measured elements in Solar system ? Image credit ESA-Herschel, ALMA (ESO/NAOJ/NRAO), Marty et al, 2016; André, 2012; ARIEL – 13th Appleton Space Conference 5 THE SUN’S PLANETS ARE COLD SOME KEY O, C, N, S MOLECULES ARE NOT IN GAS FORM T ~ 150 K Image credit NASA Juno mission, NASA Galileo ARIEL – 13th Appleton Space Conference 6 WARM/HOT EXOPLANETS O, C, N, S (TI, VO, SI) MOLECULES ARE IN GAS FORM Atmospheric pressure 0.01Bar H2O gas CO2 gas CO gas CH4 gas HCN gas TiO gas T ~ 500-2500 K Condensates VO gas H2S gas 1 Bar Gases from interior ARIEL – 13th Appleton Space Conference 7 CHEMICAL MEASUREMENTS TODAY SPECTROSCOPIC OBSERVATIONS WITH CURRENT INSTRUMENTS (HUBBLE, SPITZER,SPHERE,GPI) • Precision of 20 ppm can be reached today by Hubble-WFC3 • Current data are sparse, instruments not absolutely calibrated • ~ 40 planets analysed -
Photographs Written Historical and Descriptive
CAPE CANAVERAL AIR FORCE STATION, MISSILE ASSEMBLY HAER FL-8-B BUILDING AE HAER FL-8-B (John F. Kennedy Space Center, Hanger AE) Cape Canaveral Brevard County Florida PHOTOGRAPHS WRITTEN HISTORICAL AND DESCRIPTIVE DATA HISTORIC AMERICAN ENGINEERING RECORD SOUTHEAST REGIONAL OFFICE National Park Service U.S. Department of the Interior 100 Alabama St. NW Atlanta, GA 30303 HISTORIC AMERICAN ENGINEERING RECORD CAPE CANAVERAL AIR FORCE STATION, MISSILE ASSEMBLY BUILDING AE (Hangar AE) HAER NO. FL-8-B Location: Hangar Road, Cape Canaveral Air Force Station (CCAFS), Industrial Area, Brevard County, Florida. USGS Cape Canaveral, Florida, Quadrangle. Universal Transverse Mercator Coordinates: E 540610 N 3151547, Zone 17, NAD 1983. Date of Construction: 1959 Present Owner: National Aeronautics and Space Administration (NASA) Present Use: Home to NASA’s Launch Services Program (LSP) and the Launch Vehicle Data Center (LVDC). The LVDC allows engineers to monitor telemetry data during unmanned rocket launches. Significance: Missile Assembly Building AE, commonly called Hangar AE, is nationally significant as the telemetry station for NASA KSC’s unmanned Expendable Launch Vehicle (ELV) program. Since 1961, the building has been the principal facility for monitoring telemetry communications data during ELV launches and until 1995 it processed scientifically significant ELV satellite payloads. Still in operation, Hangar AE is essential to the continuing mission and success of NASA’s unmanned rocket launch program at KSC. It is eligible for listing on the National Register of Historic Places (NRHP) under Criterion A in the area of Space Exploration as Kennedy Space Center’s (KSC) original Mission Control Center for its program of unmanned launch missions and under Criterion C as a contributing resource in the CCAFS Industrial Area Historic District.