DOCSLIB.ORG

Italian SKA White Book

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text

Load more

Italian SKA White Book June 28, 2013 Editors1 & Contributors: L. Feretti1, I. Prandoni1, G. Brunetti1, C. Burigana2,35, A. Capetti3, M. Della Valle4, A. Ferrara5, G. Ghirlanda6, F. Govoni7, S. Molinari8, A. Possenti7, R. Scaramella9, L. Testi10,11, P. Tozzi11, G. Umana12, A. Wolter13 Other Contributors: L. Amati2, C. Baccigalupi14, M.T. Beltrán11, G. Bonnoli6, S. Borgani15,16,17, E. Branchini18, J.R. Brucato11, C. Buemi12, Z.-Y. Cai15, S. Campana6, S. Capozziello19,20, V. Casasola1, P. Caselli21,11, R. Cassano1, P. Castangia7, , C. Ceccarelli22,11, R. Cesaroni11, C. Codella11, L. Costamante23, S. Covino6, G. Cresci24, P. D’Avanzo6, M. De Laurentis19,20, G. De Lucia15, A. De Rosa2, G. de Zotti25, I. Donnarumma8,31, S. Ettori24, M. Feroci8,36, F. Finelli2, F. Fontani11,F. Fraternali26, F. Gastaldello27, G. Ghisellini6, G. Giovannini26,1, M. Giroletti1, M. Gitti26,24, A. Gruppuso2, D. Guidetti1, L. Guzzo6, L. Hunt11, P. Leto1, C. Maccone28, M. Magliocchetti8, F. Mannucci11, A. Marconi29, M. Massardi1, S. Matarrese30, P. Mazzotta31, A. Melandri6, A. Melchiorri32, N. Menci9, A. Mesinger5, M. Murgia7, M. Negrello25, M.E. Palumbo12, F. Panessa8, D. Paoletti2, P. Parma1, F. Perrotta16, C. M. Raiteri3, E. M. Rossi33, A. C. Ruggeri19,20, R. Salvaterra27, L. Stella9, G. Tagliaferri6, F. Tavecchio6, A. Tarchi7, A. Tramacere34, C. Trigilio12, G. Trinchieri13, T. Trombetti2, S. Turriziani31, V. Vacca1,T. Venturi1, D. Vergani2, M. Viel16,17, L. Zampieri25 1E-mail to: [email protected],[email protected] Affiliations: 1INAF – IRA,Via Piero Gobetti 101, I-40129, Bologna, Italy 2INAF – IASF, Via Piero Gobetti 101, I-40129, Bologna, Italy 3INAF – OA Torino, Strada Osservatorio 20, I-10025, Pino Torinese (To), Italy 4INAF – OA Capodimonte, Salita Moiariello 16, I-80131, Napoli, Italy 5Scuola Normale Superiore, Piazza dei Cavalieri 7, I-56126, Pisa, Italia 6INAF – OA Brera, via Bianchi 46, I-23807, Merate, Italy 7INAF – OA Cagliari, loc. Poggio dei Pini, Strada 54, I-09012 Capoterra 8INAF – IAPS Roma, Via Fosso del Cavalaiere 100, I-00133, Roma, Italy 9INAF – OA Roma, Via Frascati 33, I-00040, Monte Porzio Catone (RM), Italy 10ESO – Karl-Schwarzshild-Strasse 2, D-85748, Garching b. München, Germany 11INAF, OA Arcetri, Largo E. Fermi 5, I-50125, Firenze, Italy 12INAF, OA Catania, via S. Sofia 78, I-95123, Catania, Italy 13INAF – OA Brera, via Brera 28, I-20121, Milano, Italy 14SISSA, via S. Sofia 78, I-95123, Triestre, Italy 15Università di Trieste, Dipartimento di Fisica, via Valerio 2, I-34127, Trieste, Italy 16INAF – OA Trieste, via G.B. Tiepolo 11, I-34143, Trieste, Italy 17INFN - Sez. di Trieste, Università di Trieste, via Valerio 2, I-34127, Italy 18Università di Roma Tre, Dip. di Matematica e Fisica, via della Vasca Navale 84, I-00146, Roma, Italy 19Università di Napoli "Federico II", Dip. di Scienze Fisiche, Complesso Universitario di Monte S. Angelo Ed.G, Via Cinthia, I-80126, Napoli, Italy 20INFN, Sez. di Napoli, Complesso Universitario di Monte S. Angelo Ed.G, Via Cinthia, I-80126, Napoli, Italy 21School of Physics and Astronomy, University of Leeds, Leeds LS2 9JT, UK 22Institut de Planétologie et d’Astrophysique de Grenoble (IPAG) UMR 5274, UJF-Grenoble 1/CNRS- INSU, Grenoble F-38041, France 23University of Perugia, I-06123 Perugia, Italy 24INAF – OA Bologna, Via Ranzani 2, I–40126, Bologna, Italy 25INAF – OA Padova, Vicolo dell’Osservatorio 5, I-35122, Padova, Italy 26Universitá di Bologna, Dip. di Astronomia, Via Ranzani 2, I-40126, Bologna, Italy 27INAF – IASF, via Bassini 15, I-20133, Milano, Italy 28International Academy of Astronautics (IAA), P.O. Box 1268-16, F-75766, Paris Cedex 16, France 29Universitá di Firenze, Dipartimento di Fisica e Astronomia, Via Sansone 1, I-50019, Sesto Fiorentino (Firenze), Italy 30Universitá di Padova, Dipartimento di Fisica, Via Marzolo 8, I-35131, Padova, Italy 31Universitá di Roma "Tor Vergata", Dipartimento di Fisica, Via della Ricerca Scientifica, 1, I-00133, Roma, Italy 32Universitá di Roma "La Sapienza", Dipartimento di Fisica, P.le Aldo Moro 2, I-00185, Roma, Italy 33Leiden Observatory, Leiden University, P.O. Box 9513, 2300 RA, Leiden, The Netherlands 34ISDC, Geneve University, Chemin d’Ecogia 16, F-1290 Versoix, Switzerland 35Universitá di Ferrara, Dipartimento di Fisica e Scienze della Terra, Via Giuseppe Saragat 1, I-44100, Ferrara, Italy 36INFN, Sez. di Roma "Tor Vergata", Via della Ricerca Scientifica, 1, I-00133, Roma, Italy –1– This Book has been produced in the framework of SKA–related INAF initiatives and has been endorsed by the INAF Scientific Council Contents Preface 6 I Introduction 7 1 The SKA and its Scientific Perspectives 8 1.1 SKA Science Drivers 8 2 Italian Involvement in Preparatory Work for the SKA 13 2.1 SKA-driven Scientific Activity 13 2.2 Synergies with Other Future Facilities 18 II Italian Astrophysical Science Interests 19 3 Cosmology 20 3.1 Studying the Dark Ages and Cosmic Dawn with the Square Kilometer Array A. Mesinger & A. Ferrara 20 3.2 Dark energy observational tests and the SKA perspective S. Capozziello, M. De Laurentis, A. C. Ruggeri 24 3.3 Probing the matter power spectrum at small scales M. Viel 30 3.4 Cosmological Constraints from the Large Scale Structure E. Branchini, L. Guzzo, M. Magliocchetti, G. de Zotti 32 3.5 Cosmology with Gamma–Ray Bursts: status, perspectives and SKA contribution L. Amati, M. De Laurentis, M. Della Valle 36 3.6 Synergy with CMB projects C. Burigana, T. Trombetti, G. de Zotti, C. Baccigalupi, F. Finelli, A. Gruppuso, F. Perrotta, A. De Rosa 41 4 Galaxy Formation and Evolution 56 4.1 Theoretical Background G. De Lucia, S. Borgani 56 4.2 Radio-Continuum Studies I. Prandoni, G. de Zotti, L. Hunt, M. Magliocchetti, P. Tozzi, Z.-Y. Cai, M. Negrello 58 4.3 Line Studies G. Cresci, F. Fraternali, L. Hunt, A. Marconi, A. Wolter, A. Capetti, F. Gastaldello, F. Mannucci, N. Menci, P. Tozzi, G. Trinchieri, V. Casasola, D. Vergani 70 3 5 AGN physics 81 5.1 Relativistic jets with SKA A. Wolter, F. Tavecchio, G. Bonnoli, M.Giroletti, S. Turriziani, A. Tramacere, I. Don- narumma, L. Costamante 81 5.2 Radio emission from Low Luminosity radio-AGNs M. Giroletti, F. Panessa 83 5.3 Nuclear radio emission from quiescent galaxies A. Capetti 84 5.4 The life cycle of radio AGN M. Murgia, P. Parma 85 5.5 Probing AGNs with Water (Mega)Masers A. Tarchi, P. Castangia 88 6 Galaxy Clusters and Magnetic Fields 92 6.1 Galaxy Clusters, Cosmic Web, and Particle Acceleration Mechanisms G. Brunetti, L. Feretti, F. Govoni, P. Tozzi, R. Cassano, M. Gitti, P. Mazzotta, T. Venturi, S. Ettori 92 6.2 Magnetic Fields F. Govoni, V. Vacca, M. Murgia, L. Feretti, F. Finelli, G. Giovannini, D. Guidetti, G. Brunetti, D. Paoletti 105 7 Stellar Astronomy 111 7.1 Stellar Radio Emission in the SKA Era G. Umana, C. Trigilio, C. Buemi and P. Leto 111 7.2 Pulsar astrophysics with SKA A. Possenti 114 7.3 Supernovae and GRB-Supernovae M. Della Valle 119 7.4 Gamma Ray Bursts G. Ghirlanda, S. Campana, S. Covino, P. D’Avanzo, G. Ghisellini, A. Melandri, R. Salvaterra, G. Tagliaferri, A. Wolter 121 7.5 Radio investigation of Ultra-Luminous X-ray Sources A. Wolter, L. Zampieri 127 7.6 Tidal Disruption Events: Synergies between SKA and LOFT I. Donnarumma, E.M. Rossi, L. Stella, M. Feroci 129 8 Interstellar Medium, Solar System, Planetary Science, Bioastronomy 134 8.1 High-Mass Star Formation M. Beltrán, S. Molinari, R. Cesaroni 134 8.2 Complex organic molecules in protostellar environments C. Codella, F. Fontani, P. Caselli, C. Ceccarelli, M.T. Beltra´n,J.R. Brucato, M.E. Palumbo 136 8.3 Galactic foregrounds versus Galactic astronomy C. Burigana 139 8.4 SETI C. Maccone 141 III Appendices 145 A Telescope Specifications 146 B Bibliography 149 Preface Radio astronomy is in the midst of a transformation. State-of-the-art technology, together with devel- opments in high-speed digital signal processing and broad-band optical fibre links between antennas, have enabled a ten-fold sensitivity boosts to existing radio facilities (e.g. e-MERLIN, JVLA, ATCA- CABB, eEVN, APERTIF), and are leading to next-generation radio telescopes (e.g. LOFAR, MWA, ASKAP, MeerKAT). All these e↵orts will ultimately lead to a new global facility, the Square Kilo- metre Array (SKA), a revolutionary, gigantic, radio telescope with a total collective area of 1 square km. These upgraded/next-generation facilities (referred to as SKA pathfinders and/or precursors) are or are becoming soon operational, and are essential technological and scientific test-beds for the first phase of the SKA, expected to start scientific observations in 2020. The expected advances in sen- sitivity, field-of-view, frequency range and spectral resolution will yield transformational science in many research fields, from cosmology to astrophysics. Italy is one of the founding members of the SKA Organization, an independent body that will seek funding and will coordinate the design phase of the SKA project. Thanks to their internationally recognized expertise, several Italian researchers are already involved in major legacy projects planned for SKA pathfinders/precursors, in some cases with leading roles. Moreover, the scientific interest to the SKA is rapidly growing in the Italian community as a whole. This Book represents the first Italian SKA-driven coordinated e↵ort to exploit existing synergies and scientific expertise/excellence in a variety of research fields, to build an Italian science roadmap to the SKA. This Book briefly presents SKA–driven scientific activities currently on-going in Italy, and a collection of science cases and/or topics, in which the Italian community has strong expertise, where SKA, in its various phases of implementation (from SKA pathfinfders and precursors to SKA phase 1 and 2), is expected to play a major role.
Recommended publications
  • ASU Colloquium

    ASU Colloquium

    New Frontiers in Artifact SETI: Waste Heat, Alien Megastructures, and "Tabby's Star" Jason T Wright Penn State University SESE Colloquium Arizona State University October 4, 2017 Contact (Warner Bros.) What is SETI? • “The Search for Extraterrestrial Intelligence” • A field of study, like cosmology or planetary science • SETI Institute: • Research center in Mountain View, California • Astrobiology, astronomy, planetary science, radio SETI • Runs the Allen Telescope Array • Berkeley SETI Research Center: • Hosted by the UC Berkeley Astronomy Department • Mostly radio astronomy and exoplanet detection • Runs SETI@Home • Runs the $90M Breakthrough Listen Project Communication SETI The birth of Radio SETI 1960 — Cocconi & Morrison suggest interstellar communication via radio waves Allen Telescope Array Operated by the SETI Institute Green Bank Telescope Operated by the National Radio Astronomy Observatory Artifact SETI Dyson (1960) Energy-hungry civilizations might use a significant fraction of available starlight to power themselves Energy is never “used up”, it is just converted to a lower temperature If a civilization collects or generates energy, that energy must emerge at higher entropy (e.g. mid-infrared radiation) This approach is general: practically any energy use by a civilization should give a star (or galaxy) a MIR excess IRAS All-Sky map (1983) The discovery of infrared cirrus complicated Dyson sphere searches. Credit: NASA GSFC, LAMBDA Carrigan reported on the Fermilab Dyson Sphere search with IRAS: Lots of interesting red sources:
  • University of Iowa Instruments in Space

    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.
  • Information Summaries

    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
  • Astrobiology and the Search for Life Beyond Earth in the Next Decade

    Astrobiology and the Search for Life Beyond Earth in the Next Decade

    Astrobiology and the Search for Life Beyond Earth in the Next Decade Statement of Dr. Andrew Siemion Berkeley SETI Research Center, University of California, Berkeley ASTRON − Netherlands Institute for Radio Astronomy, Dwingeloo, Netherlands Radboud University, Nijmegen, Netherlands to the Committee on Science, Space and Technology United States House of Representatives 114th United States Congress September 29, 2015 Chairman Smith, Ranking Member Johnson and Members of the Committee, thank you for the opportunity to testify today. Overview Nearly 14 billion years ago, our universe was born from a swirling quantum soup, in a spectacular and dynamic event known as the \big bang." After several hundred million years, the first stars lit up the cosmos, and many hundreds of millions of years later, the remnants of countless stellar explosions coalesced into the first planetary systems. Somehow, through a process still not understood, the laws of physics guiding the unfolding of our universe gave rise to self-replicating organisms − life. Yet more perplexing, this life eventually evolved a capacity to know its universe, to study it, and to question its own existence. Did this happen many times? If it did, how? If it didn't, why? SETI (Search for ExtraTerrestrial Intelligence) experiments seek to determine the dis- tribution of advanced life in the universe through detecting the presence of technology, usually by searching for electromagnetic emission from communication technology, but also by searching for evidence of large scale energy usage or interstellar propulsion. Technology is thus used as a proxy for intelligence − if an advanced technology exists, so to does the ad- vanced life that created it.
  • The Radio Search for Technosignatures in the Decade 2020–2030

    The Radio Search for Technosignatures in the Decade 2020–2030

    Astro2020 Science White Paper The radio search for technosignatures in the decade 2020–2030 Background photo: central region of the Galaxy by Yuri Beletsky, Carnegie Las Campanas Observatory Thematic Area: Planetary Systems Principal Author: Name: Jean-Luc Margot Institution: University of California, Los Angeles Email: [email protected] Phone: 310.206.8345 Co-authors: Steve Croft (University of California, Berkeley), T. Joseph W. Lazio (Jet Propulsion Laboratory), Jill Tarter (SETI Institute), Eric J. Korpela (University of California, Berkeley) March 11, 2019 1 Scientific context Are we alone in the universe? This question is one of the most profound scientific questions of our time. All life on Earth is related to a common ancestor, and the discovery of other forms of life will revolutionize our understanding of living systems. On a more philosophical level, it will transform our perception of humanity’s place in the cosmos. Observations with the NASA Kepler telescope have shown that there are billions of habitable worlds in our Galaxy [e.g., Borucki, 2016]. The profusion of planets, coupled with the abundance of life’s building blocks in the universe, suggests that life itself may be abundant. Currently, the two primary strategies for the search for life in the universe are (1) searching for biosignatures in the Solar System or around nearby stars and (2) searching for technosignatures emitted from sources in the Galaxy and beyond [e.g., National Academies of Sciences, Engineer- ing, and Medicine, 2018]. Given our present knowledge of astrobiology, there is no compelling reason to believe that one strategy is more likely to succeed than the other.
  • Ionospheric Cusp Flows Pulsed by Solar Wind Alfvén Waves

    Ionospheric Cusp Flows Pulsed by Solar Wind Alfvén Waves

    c Annales Geophysicae (2002) 20: 161–174 European Geophysical Society 2002 Annales Geophysicae Ionospheric cusp flows pulsed by solar wind Alfven´ waves P. Prikryl1, G. Provan2, K. A. McWilliams2, and T. K. Yeoman2 1Communications Research Centre, Ottawa, Ontario K2H 8S2, Canada 2Department of Physics and Astronomy, University of Leicester, UK Received: 7 February 2001 – Revised: 24 August 2001 – Accepted: 10 September 2001 Abstract. Pulsed ionospheric flows (PIFs) in the cusp foot- bow shock were the source of magnetopause surface waves print have been observed by the SuperDARN radars with inducing reconnection. periods between a few minutes and several tens of minutes. Key words. Interplanetary physics (MHD waves and PIFs are believed to be a consequence of the interplanetary turbulence) – Magnetospheric physics (magnetosphere- magnetic field (IMF) reconnection with the magnetospheric ionosphere interactions; solar wind-magnetosphere interac- magnetic field on the dayside magnetopause, ionospheric tions) signatures of flux transfer events (FTEs). The quasiperiodic PIFs are correlated with Alfvenic´ fluctuations observed in the upstream solar wind. It is concluded that on these occasions, the FTEs were driven by Alfven´ waves coupling to the day- 1 Introduction side magnetosphere. Case studies are presented in which the dawn-dusk component of the Alfven´ wave electric field mod- Ionospheric dynamics near the cusp footprint attest to pro- ulates the reconnection rate as evidenced by the radar obser- cesses at the dayside magnetopause and in particular, to vations of the ionospheric cusp flows. The arrival of the IMF pulsed magnetic reconnection (Cowley et al., 1991; Lock- southward turning at the magnetopause is determined from wood et al., 1993).
  • Photographs Written Historical and Descriptive

    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.
  • The Effect of Ionospheric Conductivity on Magnetospheric Dynamics

    The Effect of Ionospheric Conductivity on Magnetospheric Dynamics

    University of New Hampshire University of New Hampshire Scholars' Repository Doctoral Dissertations Student Scholarship Fall 2018 THE EFFECT OF IONOSPHERIC CONDUCTIVITY ON MAGNETOSPHERIC DYNAMICS Benjamin Joseph Jensen University of New Hampshire, Durham Follow this and additional works at: https://scholars.unh.edu/dissertation Recommended Citation Jensen, Benjamin Joseph, "THE EFFECT OF IONOSPHERIC CONDUCTIVITY ON MAGNETOSPHERIC DYNAMICS" (2018). Doctoral Dissertations. 2414. https://scholars.unh.edu/dissertation/2414 This Dissertation is brought to you for free and open access by the Student Scholarship at University of New Hampshire Scholars' Repository. It has been accepted for inclusion in Doctoral Dissertations by an authorized administrator of University of New Hampshire Scholars' Repository. For more information, please contact [email protected]. THE EFFECT OF IONOSPHERIC CONDUCTIVITY ON MAGNETOSPHERIC DYNAMICS BY JOSEPH B. JENSEN BS, Physics, Utah State University, Logan UT, 2013 DISSERTATION Submitted to the University of New Hampshire in Partial Fulfillment of the Requirements for the Degree of Doctor of Philosophy in Physics September 2018 ALL RIGHTS RESERVED ©2018 Joseph B. Jensen This dissertation has been examined and approved in partial fulfillment of the requirements for the degree of Doctor of Philosophy in Physics by: Dissertation Advisor, Joachim Raeder, Professor, Department of Physics University of New Hampshire Lynn Kistler, Professor,Department of Physics University of New Hampshire Kai Germaschewski, Associate Professor, Department of Physics University of New Hampshire Marc Lessard, Associate Professor, Department of Physics University of New Hampshire Simon G. Shepherd, Associate Professor of Engineering Thayer School of Engineering at Dartmouth College on 6 July 2018. Original approval signatures are on file with the University of New Hampshire Graduate School.
  • Plasma Wave Turbulence at the Magnetopause&Colon

    Plasma Wave Turbulence at the Magnetopause&Colon

    VOL. 84, NO. A12 JOURNAL OF GEOPHYSICAL RESEARCH DECEMBER 1, 1979 Plasma Wave Turbulence at the Magnetopause: Observations From ISEE 1 and 2 D. A. GURNETT,l R. R. ANDERSON,l B. T. TSURUTANI,2 E. J. SMITH,2 G. PASCHMANN,3 G. HAERENDEL,3 $. J. BAME,4 AND C. T. RUSSELLs In this paper we investigateplasma wave electric and magnetic fields in the vicinity of the magneto- pauseby usingrecent measurements from the ISEE 1 and 2 spacecraft.Strong electric and magneticfield turbulenceis often observedat the magnetopause.The electricfield spectrumof this turbulencetypically extendsover an extremelylarge frequencyrange, from lessthan a few hertz to above 100 kHz, and the magneticfield turbulencetypically extends from a few hertz to about 1 kHz. The maximum intensities usually occur in the magnetopausecurrent layer and plasmaboundary layer. Somewhatsimilar turbu- lence spectraare also sometimesobserved in associationwith flux transfer events and possible'in- clusions'of boundarylayer plasma in the magnetosphere.In addition to the broad-bandelectric and magneticfield turbulence,narrow-band electrostatic emissions are occasionallyobserved near the elec- tron plasmafrequency in the vicinity of the magnetopause.Two possibleplasma instabilities, the elec- trostaticion-cyclotron instability and the lower-hybrid-driftinstability, are consideredthe primary can- didatesfor explaining the broad-bandelectric field turbulence.The narrow-bandelectrostatic emissions near the local electron plasma frequency are believed to be either plasma oscillationsor electrostatic wavesnear the upper-hybrid-resonancefrequency. 1. INTRODUCTION waves. Although the magnetopauseis known to be very tur- bulent in the low-frequency MHD portion of the spectrum, Becauseof the many important questionswhich have been relatively little is known about the plasma wave intensitiesat raised recently concerning the physical processeswhich occur higher frequenciesin the region of primary importance for at the earth's magnetopauseboundary [Heikkila, 1975; Hae- microscopicplasma processes.Neugebauer et al.
  • Citation and Similar Papers at Core.Ac.Ukw

    Citation and Similar Papers at Core.Ac.Ukw

    4 https://ntrs.nasa.gov/search.jsp?R=19670007176 2020-03-16T18:43:02+00:00Z View metadata, citation and similar papers at core.ac.ukw .. -. brought to you by CORE I provided by NASA Technical Reports Server 1 . National Aeronautics and STace Administration Goddard Space Flight Center C ont r ac t No NAS -5 -f 7 60 THE OUTERMOST BELT OF CFLARGED PARTICLES _- .- - by K. I, Grin,yaue t: M, 2. I~alOkhlOV cussa 3 GPO PRICE $ CFSTI PRICE(S) $ 17 NOVEbI3ER 1965 Hard copy (HC) .J d-0 Microfiche (M F) ,J3’ ff 853 July 85 Issl. kosniicheskogo prostrznstva by K. N. Gringaua Trudy Vsesoyuzrloy koneferentsii & M. z. Khokhlov po kosaiches?%inlucham, 467 - 482 Noscon, June 1965. This report deals with the result of the study of a eone of char- ged pxticles with comparatively low ener-ies (from -100 ev to 10 - 4Okev), situated beyond the outer rzdiation belt (including the new data obtained on Ilectron-2 and Zond-2). 'The cutkors review, first of all, an2 in chronolo~icalorder, the space probes on which data on soft electrons 'and protons were obtained beyond the rsdistion belts. A brief review is given of soae examples of regis- tration of soft electrons at high geominetic latitudes by Mars-1 and Elec- tron-2. It is shown that here, BS in other space probes, the zones of soft electron flwcys are gartly overlap7inr with the zones of trapped radiation. The spatial distributio;: of fluxcs of soft electrons is sixdied in liqht of data oStziined fro.1 various sFnce probes, such as Lunik-1, Explorer-12, Explorer-18, for the daytime rerion along the map-etosphere boundary &om the sumy side.
  • Nasa and the Search for Technosignatures

    Nasa and the Search for Technosignatures

    NASA AND THE SEARCH FOR TECHNOSIGNATURES A Report from the NASA Technosignatures Workshop NOVEMBER 28, 2018 NASA TECHNOSIGNATURES WORKSHOP REPORT CONTENTS 1 INTRODUCTION .................................................................................................................................................................... 1 What are Technosignatures? .................................................................................................................................... 2 What Are Good Technosignatures to Look For? ....................................................................................................... 2 Maturity of the Field ................................................................................................................................................... 5 Breadth of the Field ................................................................................................................................................... 5 Limitations of This Document .................................................................................................................................... 6 Authors of This Document ......................................................................................................................................... 6 2 EXISTING UPPER LIMITS ON TECHNOSIGNATURES ....................................................................................................... 9 Limits and the Limitations of Limits ...........................................................................................................................
  • BREAKTHROUGH LISTEN Searching for Signatures of Technology

    BREAKTHROUGH LISTEN Searching for Signatures of Technology

    BREAKTHROUGH LISTEN Searching for Signatures of Technology Howard Isaacson, Andrew Siemion & the Breakthrough Listen Team Overview Search Results Instrumentation Breakthrough Listen (BL) is the most comprehensive At radio frequencies, the capability of the data recording search for signs of extraterrestrial technology ever In the first analysis of BL data, including 30 minute cycles of observations of system directly determines survey speed, and given a undertaken. Using some of the most powerful 692 targets from our stellar sample, we find that none of the observed systems fixed observing time and spectral coverage, they telescopes in the world, combined with an host high-duty-cycle radio transmitters emitting between 1.1 to 1.9 GHz with an determine survey sensitivity as well. Breakthrough Listen unprecedented capability to record, archive and EIRP of 1013 watts, a luminosity readily achievable by our own civilization. This has the ability to write data to disk at the rate of 24 GB analyze the incoming data, Breakthrough Listen is comprehensive search over hundreds of stars represents only a small piece of per second. Using commodity servers and consumer humanity’s best hope of detecting evidence for the ever growing data set being compiled by Breakthrough Listen. class hard drives, the BL backend can record 6 GHz of technological civilizations beyond the Earth. BL his bandwidth at 8 bits for two polarizations. In a typical 6 currently observing a focused target list consisting hour session, the raw data recorded to disk can exceed ~1700 nearby stars and ~150 nearby galaxies. Our 350 TB. Using GPU processors the data volume is observing strategy is expressly designed to to allow Target Selection reduced to 2% of the raw data volume in less than 6 us to to effectively work through the mountains of hours.