An Integrated Data-Driven Solar Wind – CME Numerical Framework for Space Weather Forecasting
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O + Escape During the Extreme Space Weather Event of 4-10 September
O + Escape During the Extreme Space Weather Event of 4-10 September 2017 Audrey Schillings, Hans Nilsson, Rikard Slapak, Peter Wintoft, Masatoshi Yamauchi, Magnus Wik, Iannis Dandouras, Chris Carr To cite this version: Audrey Schillings, Hans Nilsson, Rikard Slapak, Peter Wintoft, Masatoshi Yamauchi, et al.. O + Es- cape During the Extreme Space Weather Event of 4-10 September 2017. Journal of Space Weather and Space Climate, EDP sciences, 2018, 16 (9), pp.1363-1376. 10.1029/2018SW001881. hal-02408153 HAL Id: hal-02408153 https://hal.archives-ouvertes.fr/hal-02408153 Submitted on 12 Dec 2019 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. SPACE WEATHER, VOL. ???, XXXX, DOI:10.1002/, + 1 O escape during the extreme space weather event of 2 September 4–10, 2017 Audrey Schillings,1,2 Hans Nilsson,1,2 Rikard Slapak,3 Peter Wintoft,4 Masatoshi Yamauchi,1 Magnus Wik,4 Iannis Dandouras,5 and Chris M. Carr,6 Corresponding author: Audrey Schillings, Swedish Institute of Space Physics, Kiruna, Sweden. ([email protected]) 1Swedish Institute of Space Physics, Kiruna, Sweden. 2Division of Space Technology, Lule˚a University of Technology, Kiruna, Sweden. -
A Three-Dimensional Time-Dependent Model of the Polar Wind
JOURNAL OF G EOPHYSICAL RESE ARCH. VO L. 94 . NO . A7. PAG E 8973-8991 , J ULY I. 1989 A Three-Dimensional Time-Dependent Model of the Polar Wind R. W. SCHUNK AND J. J. SOJKA Center for Atmospheric and Space Sciences, Utah State University, Logan A time-dependent global model of the polar wind was used to study transient polar wind per turbations during changing magnetospheric conditions. The model calculates three-dimensional distributions for the NO+, ot, Nt, N+ and 0 + densities and the ion and electron tempera tures from diffusion and heat conduction equations at altitudes between 120 and 800 km. At altitudes above 500 km, the time-dependent nonlinear hydrodynamic equations for 0 + and H+ are solved self-consistently with the ionospheric equations. The model takes account of supersonic ion outflow, shock formation, and ion energization during a plasma expansion event. During the simulation, the magnetic activity level changed from quiet to active and back to quiet again over a 4.5-hour period. The study indicates the following: (1) Plasma pressure changes due to Te , Ti or electron density variations produce perturbations in the polar wind. In particular, plasma flux tube motion through the auroral oval and high electric field regions produces transient large-scale ion upflows and downflows. At certain times and in certain regions both inside and outside the auroral oval, H+-O+ counterstreaming can occur, (2) The density structure in the polar wind is considerably more complicated than in the ionosphere because of both horizontal plasma convec tion and changing vertical propagation speeds due to spatially varying ionospheric temperatures, (3) During increasing magnetic activity, there is an overall increase in Te , Ti and the electron density in the F-region, but there is a time delay in the buildup of the electron density that is . -
Geomagnetic Disturbance Intensity Dependence on the Universal Timing of the Storm Peak
Geomagnetic disturbance intensity dependence on the universal timing of the storm peak R.M. Katus1,3,2, M.W. Liemohn2, A.M. Keesee3, T.J. Immel4, R. Ilie2, D. T. Welling2, N. Yu. Ganushkina5,2, N.J. Perlongo2, and A. J. Ridley2 1. Department of Mathematics, Eastern Michigan University, Ypsilanti, MI, USA 2. Department of Climate and Space Sciences and Engineering, University of Michigan, Ann Arbor, MI, USA 3. Department of Physics and Astronomy, West Virginia University, Morgantown, WVU, USA 4. Space Sciences Laboratory, University of California, Berkeley, CA, USA 5. Finnish Meteorological Institute, Helsinki, Finland Submitted to: Journal of Geophysical Research Corresponding author email: [email protected] AGU index terms: 2730 Magnetosphere: inner 2788 Magnetic storms and substorms (4305, 7954) 4305 Space weather (2101, 2788, 7900) 4318 Statistical analysis (1984, 1986) 7954 Magnetic storms (2788) Keywords: Geomagnetic indices, ground-based magnetometers, Longitudinal dependence, magnetic storms, space weather Key points: • We statistically examine storm-time solar wind and geophysical data as a function of UT of the storm peak. • There is a significant UT dependence to large storms; larger storms occur with a peak near 02 UT. • The difference in storm magnitude is caused by substorm activity and not by solar wind driving. This is the author manuscript accepted for publication and has undergone full peer review but has not been through the copyediting, typesetting, pagination and proofreading process, which may lead to differences between this version and the Version of Record. Please cite this article as doi: 10.1002/2016JA022967 This article is protected by copyright. All rights reserved. -
Ionospheric Response to Traveling Convection Twin Vortices
GEOPHYSICAL RESEARCH LETTERS, VOL. 21, NO. 17, PAGES 1759-1762, AUGUST 15,1994 JonoS heric response to traveling convection twin vortices It W. Schunk, L. Zhu, and J. J. Sojka Center for Atmo pheric and Space Sciences, Utah State University, Logan, Utah 84322-4405 Abstract. Traveling convection twin vortices have been move in the antisunward direction for a period of several hours, bserved for everal years. At ionospheric altitudes, the twin with about a 15-minute time interval between vortices. ~ortiCes correspond to spatially localized, transient structures Mounting evidence indicates that the twin vortices occur on embedded in large-scale background convection pattern. The closed magnetic field lines and most likely those field lines convection vortices are typically observed in the morning and that connect to the low-latitude boundary layers (LLBL) evening regions. They are aligned predominantly in the east [Heikkila et ai., 1989; McHenry et ai., 1990a]. At present, the west direction and have a horizontal extent of from 500-1000 prevailing view is that the twin vortices are not a result of flux km. Associated with the twin vortices are enhanced electric transfer events at the dayside magnetopause, but their exact fields, particle precipitation, and an upward/downward field cause is still controversial. Friis-Christensen et ai. [1988] aligned cu rrent pair. Once formed, the twin vortex structures suggested that the traveling vortices are due to sudden changes propagate in the tail ward direction at speeds of several km/s, in the solar wind dynamic pressure or the interplanetary but they weaken as they propagate and only last for about 10- magnetic field (lMF). -
The Maunder Minimum and the Variable Sun-Earth Connection
The Maunder Minimum and the Variable Sun-Earth Connection (Front illustration: the Sun without spots, July 27, 1954) By Willie Wei-Hock Soon and Steven H. Yaskell To Soon Gim-Chuan, Chua Chiew-See, Pham Than (Lien+Van’s mother) and Ulla and Anna In Memory of Miriam Fuchs (baba Gil’s mother)---W.H.S. In Memory of Andrew Hoff---S.H.Y. To interrupt His Yellow Plan The Sun does not allow Caprices of the Atmosphere – And even when the Snow Heaves Balls of Specks, like Vicious Boy Directly in His Eye – Does not so much as turn His Head Busy with Majesty – ‘Tis His to stimulate the Earth And magnetize the Sea - And bind Astronomy, in place, Yet Any passing by Would deem Ourselves – the busier As the Minutest Bee That rides – emits a Thunder – A Bomb – to justify Emily Dickinson (poem 224. c. 1862) Since people are by nature poorly equipped to register any but short-term changes, it is not surprising that we fail to notice slower changes in either climate or the sun. John A. Eddy, The New Solar Physics (1977-78) Foreword By E. N. Parker In this time of global warming we are impelled by both the anticipated dire consequences and by scientific curiosity to investigate the factors that drive the climate. Climate has fluctuated strongly and abruptly in the past, with ice ages and interglacial warming as the long term extremes. Historical research in the last decades has shown short term climatic transients to be a frequent occurrence, often imposing disastrous hardship on the afflicted human populations. -
The Exosphere, Leading to a Much More Descriptive Science
UNCLASSIFIED 1070 SSPPAACCEE EENNVVIIIRROONNMMEENNTT TTEECCHHNNOOLLOO GGIIIEESS GEOCORONA IN LYMAN Contract F19628 Contract Justin Technologies public distribution Notice: This document is released for May 2012 EXOSPHERIC HYDROGEN EXOSPHERIC J. J. OBSERVATIONS OF THE OF OBSERVATIONS Bailey ATOM DISTRIBUTIONS ATOM . THREE - 03 by by - C Space Space Environment - OBTAINED FROM OBTAINED 0076 SET TR 2012 - DIMENSIONAL - - 001 ALPHA THREE-DIMENSIONAL EXOSPHERIC HYDROGEN ATOM DISTRIBUTIONS OBTAINED FROM OBSERVATIONS OF THE GEOCORONA IN LYMAN-ALPHA by Justin J. Bailey A Dissertation Presented to the FACULTY OF THE USC GRADUATE SCHOOL UNIVERSITY OF SOUTHERN CALIFORNIA In Partial Fulfillment of the Requirements for the Degree DOCTOR OF PHILOSOPHY (ASTRONAUTICAL ENGINEERING) May 2012 Copyright 2012 Justin J. Bailey for my wife, Natalie, a bona fide yogini who at times had to wrap her hands around my head to keep my brain from falling out ii Acknowledgements My opportunity to contribute in this field was established and supported by many different people. After finishing with an M.S. in Astronautical Engineering, I walked into Professor Mike Gruntman’s office hoping to learn more about space physics and aeronomy. He proceeded to draw the geocorona in assorted colors on a whiteboard, and it was then that the content of this dissertation was born. Of course, none of this research would have been possible were it not for his expertise and guidance. I would like to thank my advisory committee (Professors Daniel Erwin, Joseph Kunc, W. Kent Tobiska, and Darrell Judge) for their many insightful observations. I am especially indebted to Dr. Tobiska for numerous opportunities to learn more about the solar output and how it drives the exosphere, leading to a much more descriptive science discussion in the relevant sections. -
On the Effect of the Background Wind on the Evolution of Interplanetary Shock Waves
A&A 430, 1099–1107 (2005) Astronomy DOI: 10.1051/0004-6361:20041676 & c ESO 2005 Astrophysics On the effect of the background wind on the evolution of interplanetary shock waves C. Jacobs, S. Poedts, B. Van der Holst, and E. Chané Centre for Plasma Astrophysics, K.U. Leuven, Celestijnenlaan 200B, 3001, Leuven, Belgium e-mail: [email protected] Received 16 July 2004 / Accepted 20 September 2004 Abstract. The propagating shock waves in the solar corona and interplanetary (IP) space caused by fast Coronal Mass Ejections (CMEs) are simulated numerically and their structure and evolution is studied in the framework of ideal magnetohydrodynamics (MHD). Due to the presence of three characteristic velocities and the anisotropy induced by the magnetic field, the CME shocks generated in the lower corona can have a complex structure and topology including secondary shock fronts, over-compressive and compound shocks, etc. The evolution of these CME shocks is followed during their propagation in IP space up to r = 30 R. Here, particular attention is given to the effect of the background solar wind on the evolution parameters of the fast CME shocks, i.e. shock speed, deformation of the leading shock front and the CME plasma, stand-off distance of the leading shock front, direction, spread angle, etc. First, different “frequently used” solar wind models are reconstructed with the same numerical code, the same numerical technique on exactly the same numerical grid (and thus the same numerical dissipation), the same boundary conditions, and the same normalization. Then, a simple CME model is superposed on three different solar wind models, again using exactly the same initial conditions. -
Validation for Global Solar Wind Prediction Using Ulysses Comparison: Multiple Coronal and Heliospheric Models Installed at the Community Coordinated Modeling Center
Validation for Global Solar Wind Prediction Using Ulysses Comparison: Multiple Coronal and Heliospheric Models Installed at the Community Coordinated Modeling Center L.K. Jian (1,2), P.J. MacNeice (2), M.L. Mays (3,2), A. Taktakishvili (3,2), D. Odstrcil (4,2), B. Jackson (5), H.-S. Yu (5), P. Riley (6), I.V. Sokolov (7) 1. Department of Astronomy, University of Maryland, College Park, Maryland, USA 2. Heliophysics Science Division, NASA Goddard Space Flight Center, Greenbelt, Maryland, USA 3. Department of Physics, Catholic University of America, Washington, District of Columbia, USA 4. School of Physics, Astronomy, and Computational Sciences, George Mason University, Fairfax, Virginia, USA 5. Center for Astrophysics and Space Sciences, University of California, San Diego, La Jolla, California, USA 6. Predictive Science Inc., San Diego, California, USA 7. Department of Atmospheirc, Oceanic, and Space Sciences, University of Michigan, Ann Arbor, Michigan, USA Abstract The prediction of the background global solar wind is a necessary part of space weather forecasting. Several coronal and heliospheric models have been installed and/or recently upgraded at the Community Coordinated Modeling Center (CCMC), including the Wang- Sheely-Arge (WSA)-Enlil model, MHD-Around-a-Sphere (MAS)-Enlil model, Space Weather Modeling Framework (SWMF), and heliospheric tomography using interplanetary scintillation (IPS) data. Ulysses recorded the last fast latitudinal scan from southern to northern poles in 2007. By comparing the modeling results with Ulysses observations over seven Carrington rotations, we have extended our third-party validation from the previous near-Earth solar wind to mid-to- high latitudes, in the same late declining phase of solar cycle 23. -
The Polar Wind Modulated by the Spatial Inhomogeneity of the Strength of the Earth's Magnetic Field
Originally published as: Li, K., Förster, M., Rong, Z., Haaland, S., Kronberg, E., Cui, J., Chai, L., Wei, Y. (2020): The Polar Wind Modulated by the Spatial Inhomogeneity of the Strength of the Earth's Magnetic Field. - Journal of Geophysical Research: Space Physics, 125, 4, e2020JA027802. https://doi.org/10.1029/2020JA027802 RESEARCH ARTICLE The Polar Wind Modulated by the Spatial Inhomogeneity 10.1029/2020JA027802 of the Strength of the Earth's Magnetic Field Key Points: Kun Li1 , Matthias Förster2,3, Zhaojin Rong4,5 , Stein Haaland2,6, Elena Kronberg2,7 , • The density and the particle flux of 1,8 4,5 4,5 the polar wind are revealed to be Jun Cui , Lihui Chai , and Yong Wei anticorrelated with the strength of 1 the Earth's magnetic field Planetary Environmental and Astrobiological Research Laboratory (PEARL), School of Atmospheric Sciences, Sun • The polar rain can be the main Yat‐sen University, Zhuhai, China, 2Max Planck Institute for Solar System Research, Göttingen, Germany, 3German energy source of the polar wind in Research Centre for Geosciences, Helmholtz Centre Potsdam, Potsdam, Germany, 4Institute of Geology and Geophysics, the southern hemisphere during Chinese Academy of Sciences, Beijing, China, 5College of Earth and Planetary Sciences, University of Chinese Academy of periods of high solar activity levels 6 7 • A strong magnetic field diminishes Sciences, Beijing, China, Birkeland Centre for Space Science, University of Bergen, Bergen, Norway, Department of energy depositions in the polar cap Earth and Environmental Sciences, Ludwig Maximilian University of Munich, Munich, Germany, 8Chinese Academy of and thus controls the density and Sciences, Key Laboratory of Lunar and Deep Space Exploration, National Astronomical Observatories, Beijing, China particle flux of the polar wind Abstract When the geomagnetic field is weak, the small mirror force allows precipitating charged fl Correspondence to: particles to deposit energy in the ionosphere. -
Multiple Transpolar Auroral Arcs Reveal Insight About Coupling Processes in the Earth's Magnetotail
Multiple transpolar auroral arcs reveal insight about coupling processes in the Earth’s magnetotail Qing-He Zhanga,1, Yong-Liang Zhangb, Chi Wangc, Michael Lockwoodd, Hui-Gen Yange, Bin-Bin Tangc, Zan-Yang Xinga, Kjellmar Oksavikf,g, Larry R. Lyonsh, Yu-Zhang Maa, Qiu-Gang Zongi, Jøran Idar Moenj,g, and Li-Dong Xiaa aShandong Provincial Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment, Institute of Space Sciences, Shandong University, Weihai, Shandong, 264209, China; bThe Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723; cState Key Laboratory of Space Weather, Center for Space Science and Applied Research, Chinese Academy of Sciences, Beijing, 100190, China; dDepartment of Meteorology, University of Reading, Reading, RG6 6BB, United Kingdom; eMinistry of Natural Resources Key Laboratory of Polar Science, Polar Research Institute of China, Shanghai, 200136, China; fDepartment of Physics and Technology, Birkeland Centre for Space Science, University of Bergen, Bergen, N-5020, Norway; gArctic Geophysics Department, The University Centre in Svalbard, Longyearbyen, N-9171, Norway; hDepartment of Atmospheric and Oceanic Sciences, University of California, Los Angeles, CA 90095; iSchool of Earth and Space Sciences, Peking University, Beijing, 100871, China; and jDepartment of Physics, University of Oslo, Blindern, Oslo 0371, Norway Edited by Lennard A. Fisk, University of Michigan, Ann Arbor, MI, and approved May 26, 2020 (received for review January 11, 2020) A distinct class of aurora, called transpolar auroral arc (TPA) (in twisting of the magnetotail due to IMF variations (3, 21, 22). some cases called “theta” aurora), appears in the extremely high- These processes could result in plasma sheet bifurcation, fila- latitude ionosphere of the Earth when interplanetary magnetic mentary extent into the lobes, or hot plasma trapped in the tail field (IMF) is northward. -
Solar Illumination Control of the Polar Wind 10.1002/2017JA024615 L
Journal of Geophysical Research: Space Physics RESEARCH ARTICLE Solar Illumination Control of the Polar Wind 10.1002/2017JA024615 L. Maes1,2 , R. Maggiolo1 ,J.DeKeyser1,3 , M. André4 , A. I. Eriksson4 , Key Points: S. Haaland2,5 ,K.Li6,7 , and S. Poedts3 • Polar wind flux density exhibits a dependence on the solar zenith angle 1Royal Belgian Institute for Space Aeronomy, Brussels, Belgium, 2Max Planck Institute for Solar System Research, • Both density and velocity in the polar 3 4 wind show similar but weaker solar Göttingen, Germany, Center for Mathematical Astrophysics, KU Leuven, Leuven, Belgium, Swedish Institute for Space zenith angle dependence Physics, Uppsala, Sweden, 5Department of Physics and Technology, University of Bergen, Bergen, Norway, 6Key • Seasonal variations are observed in Laboratory of Earth and Planetary Physics, Institute of Geology and Geophysics, Chinese Academy of Sciences, Beijing, the polar wind flux density China, 7State Key Laboratory of Space Weather, Chinese Academy of Sciences, Beijing, China Supporting Information: • Supporting Information S1 Abstract Polar wind outflow is an important process through which the ionosphere supplies plasma • Figure S1 to the magnetosphere. The main source of energy driving the polar wind is solar illumination of the ionosphere. As a result, many studies have found a relation between polar wind flux densities and solar EUV Correspondence to: intensity, but less is known about their relation to the solar zenith angle at the ionospheric origin, certainly L. Maes, at higher altitudes. The low energy of the outflowing particles and spacecraft charging means it is very [email protected] difficult to measure the polar wind at high altitudes. -
Good Science, Bad Science: Teaching Evolution in the States. INSTITUTION Thomas B
DOCUMENT RESUME ED 447 099 SP 039 576 AUTHOR Lerner, Lawrence S. TITLE Good Science, Bad Science: Teaching Evolution in the States. INSTITUTION Thomas B. Fordham Foundation, Washington, DC. PUB DATE 2000-09-00 NOTE 66p. AVAILABLE FROM Thomas B. Fordham Foundation, 1627 K Street, N.W., Suite 600, Washington, DC 20006; Tel: 202-223-5452 or 888-TBF-7474 (toll-free); Fax: 202-223-9226; Web site: http://www.edexcellence.net. PUB TYPE Reports Descriptive (141) EDRS PRICE MF01/PC03 Plus Postage. DESCRIPTORS *Academic Standards; Biological Influences; Creationism; Elementary Secondary Education; *Evolution; Public Schools; *Science Education; *State Standards ABSTRACT This report discusses evolution in science education, evaluating the state-by-state treatment of evolution in science standards. It explains the role of evolution as an organizing principle for all the historical sciences. Seven sections include: "Introduction" (the key role of evolution in the sciences); "How Do Good Standards Treat Biological Evolution?" (controversial versus consensual knowledge and why students should learn about evolution); "Extrascientific Issues" (e.g., the diversity of anti-evolutionists, why anti-evolutionism persists, and how science standards reflect creationist pressures); "Evaluation of State Standards" (very good to excellent, good, satisfactory, unsatisfactory, useless or absent, and disgraceful); "Sample Standards"; "Further Analysis" (grades for science standards as a whole); and "Conclusions." Overall, 31 states do at least a satisfactory job of handling the central organizing principle of the historical sciences, 10 states do an excellent or very good job of presenting evolution, and 21 states do a good or satisfactory job. More than one-third of states do not do a satisfactory job.