DOCSLIB.ORG

(SW) and Interplanetary Magnetic Field (IMF) Control of Magnetospheric Electrodynamics

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
(SW) and Interplanetary Magnetic Field (IMF) Control of Magnetospheric Electrodynamics J. Geomag. Geoelectr., 38, 1115-1141, 1986 Interplanetary Control of High Latitude Electrodynamics William J. BURKE1 and Mary Anne DoYLE2 1Air Force Geophysi cs Laboratory, Hanscom AFB, Massachusetts 01731, U.S.A. 2Regis College , Weston, Massachusetts 02193, U.S.A. (Received November 7, 1985; Revised January 28, 1986) This paper reviews recent observational developments concerning the influence of the solar wind (SW) and the interplanetary magnetic (IMF) field on magneto- spheric processes. Examples are chosen to demonstrate that the influence of the SW/IMF is global in scope. Subsequent to sudden compressions of the magneto- sphere observed by the Dynamics Explorer satellite the entire auroral oval is bombarded by previously trapped particles. Whether this is followed by a main phase storm or a theta aurora depends on the north-south polarity of the IMF . The potential drop across the polar cap is shown to correlate with the interplanetary electric field. However the potential across the polar cap is much less than the potential across the magnetosphere in the solar wind. The influence of the azimuthal component and ionospheric conductivity on the polar cap convection pattern is discussed in terms of recent observations from the Dynamics Explorer satellite. During periods of northward IMF, regions of sunward convection, with an attendant field-aligned current system, are found in the sunlit ionosphere on the day side of the magnetic dawn-dusk meridian. On the night side of this meridian and in the darkened polar cap, electric fields and field-aligned currents show filamentary structures. Electron precipitation in the polar cap varies from nearly uniform polar rain during periods of southward IMF to structured polar rain and sun-aligned arcs when the IMF has a northward component. The theta aurora detected by the imaging system on Dynamics Explorer appears in regions of sunward convection accompanied by downcoming O+ ions. This suggests that the lobes of the magnetotail are bifurcated by closed, plasma sheet field lines. At lower magnetic latitudes the systematics of the equatorward boundary of auroral electron precipitation are indirectly controlled by the interplanetary electric field. For low to moderate levels of KP, reasonable estimates of the polar cap potential may be derived from the positions of this boundary. 1. Introduction The topic assigned for this review concerns solar wind (SW) and interplanetary magnetic field (IMF) control of magnetospheric electrodynamics. This is a very broad topic with several possible meanings. Many magnetospheric processes correlate with the dynamics of the SW/IMF. At high latitudes the SW/IMF affects the location and width of the dayside cusps (BURCH, 1973), the cross polar cap potential, the patterns of convection, the conditions for substorm onset and the structure of the plasma- pause. Even changes in the direction and intensity of the equatorial electrojet (GoNZALESet al., 1983) and the local time of equatorial spread Fcan be controlled by effects of the SW/IMF. In this paper we restrict our attention to high-latitude 1115 1116 W. J. BuRKE and M. A. DoYLE electrodynamic coupling effects observed in the polar cap and near the equatorward boundary of auroral precipitation. Other papers presented in this symposium address a broader spectrum of SW/IMF effects on the magnetosphere. It is useful to distinguish between processes in which the transfer of mass, momentum and energy between the SW/IMF and the magnetosphere are direct, from those that are mediated by internal magnetospheric processes. The cross-polar cap potential and the structure of the plasmapause are examples of direct and indirect coupling, respectively. Here, however, a word of caution should be interjected, as diagnostic sensors evolve and new regions of space are explored, observations are showing that there are very few pure transfer processes. Rather there are only true coupling processes in which one of the partners plays a relatively dominant role. During the 1960's and early 1970's two global models of the coupling between the magnetosphere and SW/IMF competed for the hearts and minds of magnetospheric physicists. The model of AXFORDand HiNEs (1961) postulated that magnetosheath plasma exerts a viscous force on a layer of unspecified thickness inside the magnetopause. Magnetic field lines threading this layer are dragged in the anti-solar direction, and are stretched to great distances in the magnetotail. As elongated flux tubes move out of the viscous layer they snap back toward more Bipolar shapes. In the rest frame of the earth, this motion of magnetic field appears as an electric field that drives magnetospheric convection and high-latitude, ionospheric current systems. The second model, originally proposed by DUNGEY(1961), postulates that the weak magnetic field converted in and by the solar wind strongly interacts via magnetic merging with the magnetosphere. In this model the magnetosphere is made up of two distinct topologies: closed field lines with two feet tied to the earth and open field lines with one foot tied to the earth and the other to the IMF. Many studies showed that indeed the level of activity in the magnetosphere correlates with the southward component of the IMF. The second phase of the model postulates that magnetic reconnection, which must occur in the magnetotail offers a plausible energy source for substorms. Observations from satellites in the magnetosphere suggest that both models contribute to magnetospheric electrodynamics. Through the low-latitude boundary layer (EASTMANet al., 1976) the magnetosheath plasma exerts tangential stresses on closed field lines. Direct evidence for dayside merging as steady (GOSLINGet al., 1982) and sporadic (RUSSELLand ELPHIC, 1979) processes have been directly measured by instrumentation on the ISEE 1 and 2 satellites. The purpose of this brief report is to summarize our present understanding of electrical coupling between the SW/IMF and the magnetosphere. This is done through a series of illustrative examples. The first example was chosen to show the global nature of the interaction as observed by the imaging system on DE-1 satellite. In the next section we consider the direct effects of electrical coupling of the SW/ IMF to the polar cap ionosphere. This section is divided into three parts dealing with the polar cap potential, the effects of IMF Br on high-latitude convection patterns and the effects of northward IMF on convection, field-aligned currents and electron precipitation in the polar cap. The final section examines indirect effects of SW/IMF coupling to the magnetosphere as illustrated by the systematics of auroral electron precipitation boundaries. Interplanetary Control of High Latitude Electrodynamics 1117 2. Global Effects of the SWl IMF The basic intuition of both the Axford-Hines and the Dungey models is that the solar wind interaction with the magnetosphere is global in scale. However, ground and satellite observational studies of the interactions are spatially restricted. In the observational sense, global models have historically been created piece-meal. Our situation has been radically altered by the imaging system of the Dynamics Explorer 1 satellite. For the first time we are able to witness the evolution of geomagnetic processes on a global scale. Plates 1 and 2 present a series of images taken over the northern high latitude ionosphere on 20 and 22 October 1981 (CRAVEN etal., 1985). Both days were marked by sudden commencements (SC) event at 1309 UT on 20 October and 0525 UT on 22 October due to rapid increases in the dynamic pressure of the solar wind. During the 20 (22) October event the IMF was strongly southward (northward) both prior to and after the discontinuity. Within the 12 minute resolution of the DE imager the SC's were immediately followed by brightenings of the auroral oval at all local times. Within Alfven travel times, the effects of the sudden compressions on the global magnetosphere are probably instantaneous. In the case of the southward IMF the SC was quickly followed by a main phase storm (Dst=-190 nT) marked by bright auroral oval emissions seen in the last four images of Plate 1. Subsequent to the initial oval brightening in the northward IMF case, optical emissions from the auroral oval remained at constant, moderate levels. However, a well-defined theta auroral (FRANK et al., 1982) developed across the polar cap. It is interesting to note that several hours after the second SC the IMF turned southward and a -190nT main phase occurred. 3. Direct SW/IMF Effects on Polar Cap Electrodynamics The direct effects of SW/IMF coupling to the magnetosphere are reflected in near earth space through the dynamics of the polar cap. A growing body of empirical evidence suggests that most of the magnetic flux in the polar cap is open. That is, one foot is tied to earth and the other to the interplanetary medium. This section is divided into three parts in which we consider: (1) the relationship between the cross polar cap potential and the orientation and magnitude of the interplanetary electric field, (2) the effects of IMF BY on high-latitude convection patterns and (3) the effects of northward IMF on convection, field-aligned currents and electron precipitation in the polar cap. 3.1 The polar cap potential The polar cap potential Φpc is the most direct parameter for SW/IMF coupling with the magnetosphere. It measures the rate at which magnetic flux is transferred from the day to the night side of the earth (SISCOE, 1982). The potential drop across the auroral oval ΦA give the rates of flux return. While on the average ΦPC=ΦA currently held models of substorms suggest that this need not be true on an instantaneous basis. Despite the fundamental nature of ΦPC relatively few measure- ments have been reported in the literature. This scarcity reflects the inherent difficulty of making electric field measurements, as well as frequently unfavorable orbital 1118 W.
Load more

Recommended publications
  • 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.
    [Show full text]
  • VLF Wave Injection Into the Magnetosphere from Siple Station
    VOL. 79, NO. 16 JOURNAL OF GEOPHYSICAL RESEARCH JUNE I, 1974 VLF Wave Injection Into the MagnetosphereFrom Siple Station, Antarctica R. A. HELLIWELL AND J.P. KATSUFRAKIS RadioscienceLaboratory, Stanford University,Stanford, California 94305 Radio signalsin the 1.5- to 16-kHz range transmittedfrom Siple Station, Antarctica (L = 4), are used to control wave-particleinteractions in the magnetosphere.Observations at the conjugatepoint show signalgrowth and triggeredemissions including risers, failers, and hooks. Growth ratesof the order of 100 dB/s and total gainsup to 30 dB are observed.Triggered emissions may be cut off or havetheir fre- quencyrate of changealtered by Siplepulses. Similar effectsoccur in associationwith harmonicsfrom the Canadianpower system. The observedtemporal growth is predictedby a recentlyproposed feedback model of cyclotroninteraction. Plasma instability theories predicting only spatialgrowth are not in ac- cord with these observations.Possible applications include study of nonlinear plasma instability phenomena,diagnostic measurements of energeticparticles trapped in the magnetosphere,modification of the ionosphere through control of precipitation, and VLF communication through the magnetosphere. This is a report of the first resultsof a new experimentto plasma instability. To obtain further experimental data, a control wave-particleinteractions in the magnetosphere,us- transmitter was neededthat could operate at lower frequen- ing VLF waves.Coherent whistlermode signalswere injected cies and whose power, pulse length, and frequency could into the magnetospherein the 1.5- to 16.0-kHz range from a easily be varied. 100-kW transmitter located at Siple Station, Antarctica. The The next step was constructionof a 33.6-km-long horizon- output signalswere observedat the Sipleconjugate point near tal dipole at Byrd Station (L = 7.25) in 1965 [Guy, 1966].
    [Show full text]
  • A Three-Dimensional Ring Current Decay Model I 5£
    A Three-Dimensional Ring Current Decay Model Mei-Ching Fok* and Thomas E. Moore Space Sciences Laboratory NASA / Marshall Space Flight Center Huntsville, AL 35812 Janet U. Kozyra Space Physics Research Laboratory Department of Atmospheric, Oceanic and Space Sciences ^ The University of Michigan & ^ Ann Arbor, MI 48109 *l rS—o u5n vO O "0 o c o George C. Ho and Douglas C. Hamilton z => ° i Department of Physics, University of Maryland ^o College Park, MD 20742 £ 0) o 1 a. ! K </> ! UJ r- QC r- ! DC 13 i 5£ ; O tO Revised Version i 2 ^ a < QC • _i «/> tn :** < < ,0 Z Z ir~ o •*"-< , o >—i u f-4 V) 0) l^H Z -J -P >H LU LU C * ! I 3C 0 0) NAS/NRC Resident Research Associate s: «-< a u , K o s: III ** i < uj > x: w uu < en I < QC U — z x uu •- -^ I— o a. This work is an extension of a previous ring current decay model. In the previous work, a two-dimensional kinetic model was constructed to study the temporal variations of the equatorially mirroring ring current ions, considering charge exchange and Coulomb drag losses along drift paths in a magnetic dipole field. In this work, particles with arbitrary pitch angle are considered. By bounce averaging the kinetic equation of the phase space density, information along magnetic field lines can be inferred from the equator. The three-dimensional model is used to simulate the recovery phase of a model great magnetic storm, similar to that which occurred in early February 1986.
    [Show full text]
  • The Correlation of Solar Microwave and Soft X-Ray Radiation. Part 1-The
    General Disclaimer One or more of the Following Statements may affect this Document This document has been reproduced from the best copy furnished by the organizational source. It is being released in the interest of making available as much information as possible. This document may contain data, which exceeds the sheet parameters. It was furnished in this condition by the organizational source and is the best copy available. This document may contain tone-on-tone or color graphs, charts and/or pictures, which have been reproduced in black and white. This document is paginated as submitted by the original source. Portions of this document are not fully legible due to the historical nature of some of the material. However, it is the best reproduction available from the original submission. Produced by the NASA Center for Aerospace Information (CASI) U. of Iowa 69-17 Dlstrloutlon ocTNTi -go's vinont Is unllmlted. -s i ^,,4 Vr- IT q D "06VNDED ISb~ ft 1VG9 s' 240 , a=IACCE6LI014^. NUMBZR) ITMRU)I 1 UIE ! lC EI a u /^v (' 71q IN1 A h h 5 MX-'J,04 AU NUMULN) ICATEDORY) I Department of Physics and Astronomy THE UNIVFftSITY OF IOWA Iowa City, Iowa 11 T , of 'T'. 't 1 ,. I The Correlation of Solar Microwave and Soft X-Ray Radiation 1. The Solar Cycle and Slowly varying Components -X-x Charles D. Wende Department of Physics and Astronomy The University of Iowa Iowa City, Iowa 521240 March 1969 This research was supported in part by the Office of Naval Resea,7ch under contract Nonr 1509(06), by the National Aeronautics and Space Administration under grant(NsG 233-62'.
    [Show full text]
  • NASA Astronauts
    PUBLISHED BY Public Affairs Divisio~l Washington. D.C. 20546 1983 IColor4-by-5 inch transpar- available free to information lead and sent to: Non-informstionmedia may obtain identical material for a fee through a photographic contractor by using the order forms in the rear of this book. These photqraphs are government publications-not subject to copyright They may not be used to state oiimply the endorsement by NASA or by any NASA employee of a commercial product piocess or service, or used in any other manner that might mislead. Accordingly, it is requested that if any photograph is used in advertising and other commercial promotion. layout and copy be submitted to NASA prior to release. Front cover: "Lift-off of the Columbia-STS-2 by artist Paul Salmon 82-HC-292 82-ti-304 r 8arnr;w u vowzn u)rorr ~ nsrvnv~~nrnno................................................ .-- Seasat .......................................................................... 197 Skylab 1 Selected Pictures .......................................................150 Skylab 2 Selected Pictures ........................................................ 151 Skylab 3 Selected Pictures ........................................................152 Skylab 4 Selected Pictures ........................................................ 153 SpacoColony ...................................................................183 Space Shuttle ...................................................................171 Space Stations ..................................................................198 \libinn 1 1f.d Apoiio 17/Earth 72-HC-928 72-H-1578 Apolb B/Earth Rise 68-HC-870 68-H-1401 Voyager ;//Saturn 81-HC-520 81-H-582 Voyager I/Ssturian System 80-HC-647 80-H-866 Voyager IN~lpiterSystem 79-HC-256 79-H-356 Viking 2 on Mars 76-HC-855 76-H-870 Apollo 11 /Aldrin 69-HC-1253 69-H-682 Apollo !I /Aldrin 69-HC-684 69-H-1255 STS-I /Young and Crippen 79-HC-206 79-H-275 STS-1- ! QTPLaunch of the Columbia" 82-HC-23 82-H-22 Major Launches NAME UUNCH VEHICLE MISSIONIREMARKS 1956 VANGUARD Dec.
    [Show full text]
  • Articles Entered and Propagated in the Magnetosphere to Form the Ring Current
    CMYK RGB Hist. Geo Space Sci., 3, 131–142, 2012 History of www.hist-geo-space-sci.net/3/131/2012/ Geo- and Space doi:10.5194/hgss-3-131-2012 © Author(s) 2012. CC Attribution 3.0 License. Access Open Sciences Advances in Science & Research Open Access Proceedings The ring current: a short biography Drinking Water Drinking Water Engineering and Science Engineering and Science A. Egeland1 and W. J. Burke2 Open Access Access Open Discussions 1Department of Physics, University of Oslo, P.O. Box 1048, Blindern, 0316 Oslo, Norway 2Boston College, Institute for Scientific Research, Chestnut Hill, MA, USA Discussions Correspondence to: A. Egeland ([email protected]) Earth System Earth System Received: 27 March 2012 – Revised: 26 June 2012 – Accepted: 3 July 2012 – Published: 6 August 2012Science Science Abstract. Access Open The “ring current” grows in the inner magnetosphere during magnetic storms and contributesAccess Open Data sig- Data nificantly to characteristic perturbations to the Earth’s field observed at low-latitudes. This paper outlines how understanding of the ring current evolved during the half-century intervals before and after humans gained Discussions direct access to space. Its existence was first postulated in 1910 by Carl Størmer to explain the locations and equatorward migrations of aurorae under stormtime conditions. In 1917 Adolf Schmidt applied Størmer’s ring-current hypothesis to explain the observed negative perturbations in the Earth’s magnetic field.Social More than Social another decade would pass before Sydney Chapman and Vicenzo Ferraro argued for its necessity to explain Access Open Geography Open Access Open Geography magnetic signatures observed during the main phases of storms.
    [Show full text]
  • Table of Artificial Satellites Launched in 1971
    This electronic version (PDF) was scanned by the International Telecommunication Union (ITU) Library & Archives Service from an original paper document in the ITU Library & Archives collections. La présente version électronique (PDF) a été numérisée par le Service de la bibliothèque et des archives de l'Union internationale des télécommunications (UIT) à partir d'un document papier original des collections de ce service. Esta versión electrónica (PDF) ha sido escaneada por el Servicio de Biblioteca y Archivos de la Unión Internacional de Telecomunicaciones (UIT) a partir de un documento impreso original de las colecciones del Servicio de Biblioteca y Archivos de la UIT. (ITU) ﻟﻼﺗﺼﺎﻻﺕ ﺍﻟﺪﻭﻟﻲ ﺍﻻﺗﺤﺎﺩ ﻓﻲ ﻭﺍﻟﻤﺤﻔﻮﻇﺎﺕ ﺍﻟﻤﻜﺘﺒﺔ ﻗﺴﻢ ﺃﺟﺮﺍﻩ ﺍﻟﻀﻮﺋﻲ ﺑﺎﻟﻤﺴﺢ ﺗﺼﻮﻳﺮ ﻧﺘﺎﺝ (PDF) ﺍﻹﻟﻜﺘﺮﻭﻧﻴﺔ ﺍﻟﻨﺴﺨﺔ ﻫﺬﻩ .ﻭﺍﻟﻤﺤﻔﻮﻇﺎﺕ ﺍﻟﻤﻜﺘﺒﺔ ﻗﺴﻢ ﻓﻲ ﺍﻟﻤﺘﻮﻓﺮﺓ ﺍﻟﻮﺛﺎﺋﻖ ﺿﻤﻦ ﺃﺻﻠﻴﺔ ﻭﺭﻗﻴﺔ ﻭﺛﻴﻘﺔ ﻣﻦ ﻧﻘﻼ ً◌ 此电子版（PDF版本）由国际电信联盟（ITU）图书馆和档案室利用存于该处的纸质文件扫描提供。 Настоящий электронный вариант (PDF) был подготовлен в библиотечно-архивной службе Международного союза электросвязи путем сканирования исходного документа в бумажной форме из библиотечно-архивной службы МСЭ. © International Telecommunication Union A COSMOS-428 1971 57A E 0 COSMOS-429 1971 61A COSMGS-430 1971 62A COSMOS-431 1971 65A APOLLO-14 1971 8A COSMOS-432 1971 66A EOLE 1971 71A OAR-901 1971 67C APOLLO-15 1971 63A COSMOS-433 1971 68A EXPLORER-43 1971 19A CAR-907 1971 67D APOLLO-15 CSUB•SAT 3 1971 63D COSMOS-434 1971 69A EXPLORER-44 1971 58A OREOL-1 1971 119A ARIEL-4 1971 109A COSMOS-435 1971 72A EXPLORER-45 1971 96A OSO- 7 1971 83A COSMOS-436
    [Show full text]
  • National Academy of Sciences National Research Council
    NATIONAL ACADEMY OF SCIENCES NATIONAL RESEARCH COUNCIL of the UNITED STATES OF AMERICA UNITED STATES NATIONAL COMMITTEE International Union of Radio Science I ( 1975 Annual Meeting October 20-23 Sponsored by USNC/URSI in cooperation with Institute of Electrical and Electronics Engineers University of Colorado Boulder, Colorado Price $3.00 URSI/USNC 1975 Annual Meeting Condensed Technical Program Sunday, October 19 2000-2400 U.S. National Committee Meeting Sheraton Monda October 20 II-1 M~ning Communications UMC 159 III-1 Ionospheric Radio Scintillations - I UMC 156 IV-1 VLF/ELF Active and Passive Probing UMC 157 V-1/I, II, VII Extra-Terrestrial Techniques for Measuring Crustal Motions and Satellite Ranging UMC W Blrm 0900-1200 VI-1 Scattering - I RB Aud. VI-2 Antennas RB 1107 VIII-1/I Noise and Interference Measurements UMC F.R. B-la/I Auditory Effects UMC E Blrm B-lb/I Microwave Cataractogenisis UMC E Blrm 1330-1700 Combined Session UMC C Blrm 2000-2200 Evening Lecture UMC C Blrm Tuesda October 21 II-2 Sub-Surface Propagation and Communications UMC 159 1 II-3 Radio Oceanography Seasat "A ' UMC F.R. III-2 Ionospheric Radio Scintillations - II UMC 157 IV-2 Plasma Instabilities in the Magnetosphere - I UMC 158 V-2 Millimeter Wavelength Techniques UMC 156 0830-1200 VI-3 Numerical Techniques RB 1107 VI-4 Integrated and Fiber Optics - I RB Aud. VIII-2/VI Noise and Interference Models and Radio System Planning RB 1103 B-2a/I Therapeutic Applications UMC W Blrm B-2b/I Diagnostic Applications UMC W Blrm B-3/I Field Survey Instruments UMC E Blrm I-1 Measurements and Techniques RB 1103 IV-3 Plasma Instabilities in the Magnetosphere - II UMC 158 V-3/III, VIII Interference to Radio Astronomy and CCIR 1330-1700 Related Topics UMC 156 VI-5 Integrated and Fiber Optics - II RB Aud.
    [Show full text]
  • View Served (See the Review of Paschmann Et Al
    Antonova et al. Earth, Planets and Space (2015) 67:166 DOI 10.1186/s40623-015-0336-6 LETTER Open Access Problems with mapping the auroral oval and magnetospheric substorms E. E. Antonova1*, V. G. Vorobjev2, I. P. Kirpichev3, O. I. Yagodkina2 and M. V. Stepanova4 Abstract Accurate mapping of the auroral oval into the equatorial plane is critical for the analysis of aurora and substorm dynamics. Comparison of ion pressure values measured at low altitudes by Defense Meteorological Satellite Program (DMSP) satellites during their crossings of the auroral oval, with plasma pressure values obtained at the equatorial plane from Time History of Events and Macroscale Interactions during Substorms (THEMIS) satellite measurements, indicates that the main part of the auroral oval maps into the equatorial plane at distances between 6 and 12 Earth radii. On the nightside, this region is generally considered to be a part of the plasma sheet. However, our studies suggest that this region could form part of the plasma ring surrounding the Earth. We discuss the possibility of using the results found here to explain the ring-like shape of the auroral oval, the location of the injection boundary inside the magnetosphere near the geostationary orbit, presence of quiet auroral arcs in the auroral oval despite the constantly high level of turbulence observed in the plasma sheet, and some features of the onset of substorm expansion. Findings example, Hones et al. 1996, Weiss et al. 1997, Antonova Introduction et al. 2006, Xing et al. 2009). Accurate mapping of the auroral oval onto the equatorial Exclusion of a number of current systems from the geo- plane is necessary in determining the locations of sub- magnetic field models serves to constrain the accurate storm expansion phase onsets.
    [Show full text]
  • IBM CICS Explorer
    Front cover IBM CICS Explorer CICS Explorer is the new modern face of CICS CICS Deployment Assistant is the new way to manage CICS Explorer real-life usage scenarios included Chris Rayns George Bogner Nicholas Bingell Gordon Keehn Lisa Fellows Tommy Joergensen Erhard Woerner ibm.com/redbooks International Technical Support Organization IBM CICS Explorer December 2010 SG24-7778-01 Note: Before using this information and the product it supports, read the information in “Notices” on page xi. Second Edition (December 2010) This edition applies to Version 4, Release 1, CICS Transaction Server. © Copyright International Business Machines Corporation 2010. All rights reserved. Note to U.S. Government Users Restricted Rights -- Use, duplication or disclosure restricted by GSA ADP Schedule Contract with IBM Corp. Contents Notices . xi Trademarks . xii Preface . xiii The team who wrote this book . xiii Now you can become a published author, too! . xv Comments welcome. xv Stay connected to IBM Redbooks . xvi Summary of changes . xvii August 2010, Second Edition . xvii Part 1. CICS Explorer Introductions . 1 Chapter 1. CICS Explorer introduction . 3 1.1 Overview . 4 1.2 Base Explorer capabilities . 5 1.3 Plug-ins and RCP . 9 1.3.1 Eclipse concepts . 9 Chapter 2. Getting started with CICS Explorer. 19 2.1 Using CICS Explorer with CICS TS 4.1. 20 2.2 CICS Explorer connection to CICS . 20 2.2.1 Connecting CICS Explorer to a CICS region . 20 2.2.2 Connecting CICS Explorer to CICSPlex SM . 21 2.3 Setting up single-server access . 22 2.4 Setting up CICSPlex SM for CICS Explorer .
    [Show full text]
  • NASA Is Not Archiving All Potentially Valuable Data
    ‘“L, United States General Acchunting Office \ Report to the Chairman, Committee on Science, Space and Technology, House of Representatives November 1990 SPACE OPERATIONS NASA Is Not Archiving All Potentially Valuable Data GAO/IMTEC-91-3 Information Management and Technology Division B-240427 November 2,199O The Honorable Robert A. Roe Chairman, Committee on Science, Space, and Technology House of Representatives Dear Mr. Chairman: On March 2, 1990, we reported on how well the National Aeronautics and Space Administration (NASA) managed, stored, and archived space science data from past missions. This present report, as agreed with your office, discusses other data management issues, including (1) whether NASA is archiving its most valuable data, and (2) the extent to which a mechanism exists for obtaining input from the scientific community on what types of space science data should be archived. As arranged with your office, unless you publicly announce the contents of this report earlier, we plan no further distribution until 30 days from the date of this letter. We will then give copies to appropriate congressional committees, the Administrator of NASA, and other interested parties upon request. This work was performed under the direction of Samuel W. Howlin, Director for Defense and Security Information Systems, who can be reached at (202) 275-4649. Other major contributors are listed in appendix IX. Sincerely yours, Ralph V. Carlone Assistant Comptroller General Executive Summary The National Aeronautics and Space Administration (NASA) is respon- Purpose sible for space exploration and for managing, archiving, and dissemi- nating space science data. Since 1958, NASA has spent billions on its space science programs and successfully launched over 260 scientific missions.
    [Show full text]
  • 7 July 2019 General Comment the Review Written by the Author And
    Anonymous Referee #2 Received and published: 7 July 2019 General comment The review written by the author and published last year in the journal Space Science Reviews (SSR) concluded that there is a need for the development of radiation belt heavy ion empirical models. The submitted paper gathers available heavy ion measurements obtained all over the space age and tries to pave the way for the development of such models. To do so, invariant parameters (that are constant over a given range of L) are detailed and available measurements are shown on Figures and discussed in detail. The solar cycle variation of heavy ion fluxes is for the first time explored in the submitted article. Finally, the presented measurement database is important to explore the physical mechanisms that govern the heavy ion radiation belts, what is done by the author in sections 3 and 4. Comparative lessons with what is known for the protons are drawn. There is no doubt that the work presented here is important and may contribute to advances in our understanding and prediction of the heavy ion radiation belts. The submitted article may therefore, according to the reviewer, be ultimately published after several clarifications. The article needs to first be edited for English, in order to make it easily understandable so that it would have an impact on the work of others. There viewer is then wondering: what is new in this article, compared in particular with there view published in SSR last year (see specific comments)? I recommend the article to be revised and reviewed again to see if, after English proof and clarifications, the article would be suitable for publication in Annales Geophysicae.
    [Show full text]