Themis Time History of Events and Macroscale Interactions During Substorms
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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 -
A Future Mars Environment for Science and Exploration
Planetary Science Vision 2050 Workshop 2017 (LPI Contrib. No. 1989) 8250.pdf A FUTURE MARS ENVIRONMENT FOR SCIENCE AND EXPLORATION. J. L. Green1, J. Hol- lingsworth2, D. Brain3, V. Airapetian4, A. Glocer4, A. Pulkkinen4, C. Dong5 and R. Bamford6 (1NASA HQ, 2ARC, 3U of Colorado, 4GSFC, 5Princeton University, 6Rutherford Appleton Laboratory) Introduction: Today, Mars is an arid and cold world of existing simulation tools that reproduce the physics with a very thin atmosphere that has significant frozen of the processes that model today’s Martian climate. A and underground water resources. The thin atmosphere series of simulations can be used to assess how best to both prevents liquid water from residing permanently largely stop the solar wind stripping of the Martian on its surface and makes it difficult to land missions atmosphere and allow the atmosphere to come to a new since it is not thick enough to completely facilitate a equilibrium. soft landing. In its past, under the influence of a signif- Models hosted at the Coordinated Community icant greenhouse effect, Mars may have had a signifi- Modeling Center (CCMC) are used to simulate a mag- cant water ocean covering perhaps 30% of the northern netic shield, and an artificial magnetosphere, for Mars hemisphere. When Mars lost its protective magneto- by generating a magnetic dipole field at the Mars L1 sphere, three or more billion years ago, the solar wind Lagrange point within an average solar wind environ- was allowed to directly ravish its atmosphere.[1] The ment. The magnetic field will be increased until the lack of a magnetic field, its relatively small mass, and resulting magnetotail of the artificial magnetosphere its atmospheric photochemistry, all would have con- encompasses the entire planet as shown in Figure 1. -
And Ground-Based Observations of Pulsating Aurora
University of New Hampshire University of New Hampshire Scholars' Repository Doctoral Dissertations Student Scholarship Spring 2010 Space- and ground-based observations of pulsating aurora Sarah Jones University of New Hampshire, Durham Follow this and additional works at: https://scholars.unh.edu/dissertation Recommended Citation Jones, Sarah, "Space- and ground-based observations of pulsating aurora" (2010). Doctoral Dissertations. 597. https://scholars.unh.edu/dissertation/597 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]. SPACE- AND GROUND-BASED OBSERVATIONS OF PULSATING AURORA BY SARAH JONES B.A. in Physics, Dartmouth College 2004 DISSERTATION Submitted to the University of New Hampshire in Partial Fulfillment of the Requirements for the Degree of Doctor of Philosophy in Physics May, 2010 UMI Number: 3470104 All rights reserved INFORMATION TO ALL USERS The quality of this reproduction is dependent upon the quality of the copy submitted. In the unlikely event that the author did not send a complete manuscript and there are missing pages, these will be noted. Also, if material had to be removed, a note will indicate the deletion. UMT Dissertation Publishing UMI 3470104 Copyright 2010 by ProQuest LLC. All rights reserved. This edition of the work is protected against unauthorized copying under Title 17, United States Code. ProQuest LLC 789 East Eisenhower Parkway P.O. Box 1346 Ann Arbor, Ml 48106-1346 This dissertation has been examined and approved. -
Observations of Solar Wind Penetration Into the Earth's Magnetosphere: the Plasma Mantle
ENNIO R. SANCHEZ, CHING-I. MENG, and PATRICK T. NEWELL OBSERVATIONS OF SOLAR WIND PENETRATION INTO THE EARTH'S MAGNETOSPHERE: THE PLASMA MANTLE The large database provided by the continuous coverage of the Defense Meteorological Satellite Pro gram polar orbiting satellites constitutes an important source of information on particle precipitation in the ionosphere. This information can be used to monitor and map the Earth's magnetosphere (the cavity around the Earth that forms as the stream of particles and magnetic field ejected from the Sun, known as the solar wind, encounters the Earth's magnetic field) and for a large variety of statistical studies of its morphology and dynamics. The boundary between the magnetosphere and the solar wind is pre sumably open in some places and at some times, thus allowing the direct entry of solar-wind plasma into the magnetosphere through a boundary layer known as the plasma mantle. The preliminary results of a statistical study of the plasma-mantle precipitation in the ionosphere are presented. The first quan titative mapping of the ionospheric region where the plasma-mantle particles precipitate is obtained. INTRODUCTION Polar orbiting satellites are very useful platforms for studying the properties of the environment surrounding the Earth at distances well above the ionosphere. This article focuses on a description of the enormous poten tial of those platforms, especially when they are com bined with other means of measurement, such as ground-based stations and other satellites. We describe in some detail the first results of the kind of study for which the polar orbiting satellites are ideal instruments. -
Jets Downstream of Collisionless Shocks
Space Sci Rev (2018) 214:81 https://doi.org/10.1007/s11214-018-0516-3 Jets Downstream of Collisionless Shocks Ferdinand Plaschke1,2 · Heli Hietala3 · Martin Archer4 · Xóchitl Blanco-Cano5 · Primož Kajdicˇ5 · Tomas Karlsson6 · Sun Hee Lee7 · Nojan Omidi8 · Minna Palmroth9,10 · Vadim Roytershteyn11 · Daniel Schmid12 · Victor Sergeev13 · David Sibeck7 Received: 19 December 2017 / Accepted: 2 June 2018 / Published online: 21 June 2018 © The Author(s) 2018 Abstract The magnetosheath flow may take the form of large amplitude, yet spatially local- ized, transient increases in dynamic pressure, known as “magnetosheath jets” or “plasmoids” among other denominations. Here, we describe the present state of knowledge with respect to such jets, which are a very common phenomenon downstream of the quasi-parallel bow shock. We discuss their properties as determined by satellite observations (based on both case and statistical studies), their occurrence, their relation to solar wind and foreshock con- ditions, and their interaction with and impact on the magnetosphere. As carriers of plasma and corresponding momentum, energy, and magnetic flux, jets bear some similarities to bursty bulk flows, which they are compared to. Based on our knowledge of jets in the near Earth environment, we discuss the expectations for jets occurring in other planetary and B F. Plaschke [email protected] 1 Space Research Institute, Austrian Academy of Sciences, Graz, Austria 2 Present address: Institute of Physics, University of Graz, Graz, Austria 3 Department of -
THEMIS Telescope Images Analysed for Space Weather Traces
EPSC Abstracts Vol. 14, EPSC2020-1022, 2020 https://doi.org/10.5194/epsc2020-1022 Europlanet Science Congress 2020 © Author(s) 2021. This work is distributed under the Creative Commons Attribution 4.0 License. THEMIS telescope images analysed for space weather traces Melinda Dósa1, Valeria Mangano2, Zsofia Bebesi1, Stefano Massetti2, Anna Milillo2, and Anna Görgei3 1Wigner Research Centre for Physics, Space Physics and Space Technology, Budapest, Hungary ([email protected]) 2INAF/IAPS, Istituto Nazionale di Astrofisica, Roma, Italy 3Eötvös Loránd University, Institute of Physics The THEMIS solar telescope operating on Tenerife (Canary islands) has observed Mercury’s Na exosphere along several campaigns since 2007. A dataset of images taken between 2009 and 2013 are analysed here in relation with propagated solar wind data. A small subset of the images shows a low level of correlation between Na-emission and solar wind dynamic pressure. The amount of data at present is not sufficient to make a clear statement on whether the correlation is a coincidence or can be explained by other factors (position of Mercury and Earth, solar activity, etc.). Nevertheless, the authors present a comprehensive study taking into account all possible factors. Sodium plays a special role in Mercury’s exosphere: due to its strong resonance line it has been observed and monitored by Earth-based telescopes for decades. Different and highly variable patterns of Na-emission have been identified, the most common and recurrent being the high latitude double-peak pattern [1]. It is clear that the exosphere is linked to the surface and influenced by the interstellar medium and the solar wind deviated by the magnetosphere, but the role and weight of the single processes are still under discussion [2]. -
On Magnetic Storms and Substorms
ILWS WORKSHOP 2006, GOA, FEBRUARY 19-24, 2006 On magnetic storms and substorms G. S. Lakhina, S. Alex, S. Mukherjee and G. Vichare Indian Institute of Geomagnetism, New Panvel (W), Navi Mumbai-410218, India Abstract. Magnetospheric substorms and storms are indicators of geomagnetic activity. Whereas the geomagnetic index AE (auroral electrojet) is used to study substorms, it is common to characterize the magnetic storms by the Dst (disturbance storm time) index of geomagnetic activity. This talk discusses briefly the storm-substorms relationship, and highlights some of the characteristics of intense magnetic storms, including the events of 29-31 October and 20-21 November 2003. The adverse effects of these intense geomagnetic storms on telecommunication, navigation, and on spacecraft functioning will be discussed. Index Terms. Geomagnetic activity, geomagnetic storms, space weather, substorms. _____________________________________________________________________________________________________ 1. Introduction latitude magnetic fields are significantly depressed over a Magnetospheric storms and substorms are indicators of time span of one to a few hours followed by its recovery geomagnetic activity. Where as the magnetic storms are which may extend over several days (Rostoker, 1997). driven directly by solar drivers like Coronal mass ejections, solar flares, fast streams etc., the substorms, in simplest terms, are the disturbances occurring within the magnetosphere that are ultimately caused by the solar wind. The magnetic storms are characterized by the Dst (disturbance storm time) index of geomagnetic activity. The substorms, on the other hand, are characterized by geomagnetic AE (auroral electrojet) index. Magnetic reconnection plays an important role in energy transfer from solar wind to the magnetosphere. Magnetic reconnection is very effective when the interplanetary magnetic field is directed southwards leading to strong plasma injection from the tail towards the inner magnetosphere causing intense auroras at high-latitude nightside regions. -
Diffuse Electron Precipitation in Magnetosphere-Ionosphere- Thermosphere Coupling
EGU21-6342 https://doi.org/10.5194/egusphere-egu21-6342 EGU General Assembly 2021 © Author(s) 2021. This work is distributed under the Creative Commons Attribution 4.0 License. Diffuse electron precipitation in magnetosphere-ionosphere- thermosphere coupling Dong Lin1, Wenbin Wang1, Viacheslav Merkin2, Kevin Pham1, Shanshan Bao3, Kareem Sorathia2, Frank Toffoletto3, Xueling Shi1,4, Oppenheim Meers5, George Khazanov6, Adam Michael2, John Lyon7, Jeffrey Garretson2, and Brian Anderson2 1High Altitude Observatory, National Center for Atmospheric Research, Boulder CO, United States of America 2Applied Physics Laboratory, Johns Hopkins University, Laurel MD, USA 3Department of Physics and Astronomy, Rice University, Houston TX, USA 4Bradley Department of Electrical and Computer Engineering, Virginia Tech, Blacksburg VA, USA 5Astronomy Department, Boston University, Boston MA, USA 6Goddard Space Flight Center, NASA, Greenbelt MD, USA 7Department of Physics and Astronomy, Dartmouth College, Hanover NH, USA Auroral precipitation plays an important role in magnetosphere-ionosphere-thermosphere (MIT) coupling by enhancing ionospheric ionization and conductivity at high latitudes. Diffuse electron precipitation refers to scattered electrons from the plasma sheet that are lost in the ionosphere. Diffuse precipitation makes the largest contribution to the total precipitation energy flux and is expected to have substantial impacts on the ionospheric conductance and affect the electrodynamic coupling between the magnetosphere and ionosphere-thermosphere. -
Cmes, Solar Wind and Sun-Earth Connections: Unresolved Issues
CMEs, solar wind and Sun-Earth connections: unresolved issues Rainer Schwenn Max-Planck-Institut für Sonnensystemforschung, Katlenburg-Lindau, Germany [email protected] In recent years, an unprecedented amount of high-quality data from various spaceprobes (Yohkoh, WIND, SOHO, ACE, TRACE, Ulysses) has been piled up that exhibit the enormous variety of CME properties and their effects on the whole heliosphere. Journals and books abound with new findings on this most exciting subject. However, major problems could still not be solved. In this Reporter Talk I will try to describe these unresolved issues in context with our present knowledge. My very personal Catalog of ignorance, Updated version (see SW8) IAGA Scientific Assembly in Toulouse, 18-29 July 2005 MPRS seminar on January 18, 2006 The definition of a CME "We define a coronal mass ejection (CME) to be an observable change in coronal structure that occurs on a time scale of a few minutes and several hours and involves the appearance (and outward motion, RS) of a new, discrete, bright, white-light feature in the coronagraph field of view." (Hundhausen et al., 1984, similar to the definition of "mass ejection events" by Munro et al., 1979). CME: coronal -------- mass ejection, not: coronal mass -------- ejection! In particular, a CME is NOT an Ejección de Masa Coronal (EMC), Ejectie de Maså Coronalå, Eiezione di Massa Coronale Éjection de Masse Coronale The community has chosen to keep the name “CME”, although the more precise term “solar mass ejection” appears to be more appropriate. An ICME is the interplanetry counterpart of a CME 1 1. -
Solar Wind Magnetosphere Coupling
Solar Wind Magnetosphere Coupling F. Toffoletto, Rice University Figure courtesy T. W. Hill with thanks to R. A. Wolf and T. W. Hill, Rice U. Outline • Introduction • Properties of the Solar Wind Near Earth • The Magnetosheath • The Magnetopause • Basic Physical Processes that control Solar Wind Magnetosphere Coupling – Open and Closed Magnetosphere Processes – Electrodynamic coupling – Mass, Momentum and Energy coupling – The role of the ionosphere • Current Status and Summary QuickTime™ and a YUV420 codec decompressor are needed to see this picture. Introduction • By virtue of our proximity, the Earth’s magnetosphere is the most studied and perhaps best understood magnetosphere – The system is rather complex in its structure and behavior and there are still some basic unresolved questions – Today’s lecture will focus on describing the coupling to the major driver of the magnetosphere - the solar wind, and the ionosphere – Monday’s lecture will look more at the more dynamic (and controversial) aspect of magnetospheric dynamics: storms and substorms The Solar Wind Near the Earth Solar-Wind Properties Observed Near Earth • Solar wind parameters observed by many spacecraft over period 1963-86. From Hapgood et al. (Planet. Space Sci., 39, 410, 1991). Solar Wind Observed Near Earth Values of Solar-Wind Parameters Parameter Minimum Most Maximum Probable Velocity v (km/s) 250 370 2000× Number density n (cm-3) 683 Ram pressure rv2 (nPa)* 328 Magnetic field strength B 0 6 85 (nanoteslas) IMF Bz (nanoteslas) -31 0¤ 27 * 1 nPa = 1 nanoPascal = 10-9 Newtons/m2. Indicates at least one interval with B < 0.1 nT. ¤ Mean value was 0.014 nT, with a standard deviation of 3.3 nT. -
Space Weather and Real-Time Monitoring
Data Science Journal, Volume 8, 30 March 2009 SPACE WEATHER AND REAL-TIME MONITORING S Watari National Institute of Information and Communications Technology, 4-2-1 Nukuikita, Koganei, Tokyo 184-8795, Japan Email: [email protected] ABSTRACT Recent advance of information and communications technology enables to collect a large amount of ground-based and space-based observation data in real-time. The real-time data realize nowcast of space weather. This paper reports a history of space weather by the International Space Environment Service (ISES) in association with the International Geophysical Year (IGY) and importance of real-time monitoring in space weather. Keywords: Space Weather, Real-time Monitoring, International Space Environment Service (ISES) 1 INTRODUCTION The International Geophysical Year (IGY) took place between 1957 and 1958. In the IGY, the first artificial satellite, Sputnik 1, was launched on 4 October, 1957. After approximately 50 years since the Sputnik, now we use many satellites for communication, broadcast, navigation, meteorological observation, and so on. After several failures of satellites, we notice that we can not neglect the space environment, which affects manmade technology systems. It is called “space weather.” Researches of space weather are on going all over the world now. During the IGY, the information of Alert and Special World Interval (SWI) was exchanged among participated institutes for coordinated observations of the Sun and geophysical environment. The Alert was distributed whenever solar activity is unusually high and significant geomagnetic, auroral, ionospheric or cosmic ray effects are probable. The SWI was distributed whenever a possibility of an outstanding geomagnetic storm is high during the period of the Alert. -
Read Book ^ Titans: Atlas, Titan, Rhea, Helios, Eos, Prometheus, Hecate
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