Physics of Space Weather Phenomena: a Review
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Fundamentals of Impulsive Energy Release in the Corona Heliophysics 2050 Workshop White Paper A
Heliophysics 2050 White Papers (2021) 4093.pdf Fundamentals of impulsive energy release in the corona Heliophysics 2050 Workshop white paper A. Y. Shih (NASA Goddard Space Flight Center), L. Glesener (UMN), S. Krucker (UCB), S. Guidoni (Amer. Univ.), S. Christe (GSFC), K. Reeves (SAO), S. Gburek (PAS), A. Caspi (SwRI), M. Alaoui (GSFC/CUA), J. Allred (GSFC), M. Battaglia (FHNW), W. Baumgartner (MSFC), B. Dennis (GSFC), J. Drake (UMD), K. Goetz (UMN), L. Golub (SAO), I. Hannah (Univ. of Glasgow), L. Hayes (GSFC/USRA), G. Holman (GSFC/Emeritus), A. Inglis (GSFC/CUA), J. Ireland (GSFC), G. Kerr (GSFC/CUA), J. Klimchuk (GSFC), D. McKenzie (MSFC), C. Moore (SAO), S. Musset (Univ. of Glasgow), J. Reep (NRL), D. Ryan (GSFC/AU), P. Saint-Hilaire (UCB), S. Savage (MSFC), R. Schwartz (GSFC/AU), D. Seaton (NOAA), M. Stęślicki (PAS), T. Woods (LASP) Introduction Solar eruptive events are the most energetic and geo-effective space-weather drivers. They originate in the corona near the Sun’s surface as a combination of solar flares (impulsive bursts of radiation across the entire electromagnetic spectrum) and coronal mass ejections (CMEs; expulsions of magnetized plasma into interplanetary space). The radiation and energetic particles they produce can damage satellites, disrupt telecommunications and GPS navigation, and endanger astronauts in space. Many of the processes involved in triggering, driving, and sustaining solar eruptive events–including magnetic reconnection, particle acceleration, plasma heating, and energy transport in magnetized plasmas–also play important roles in phenomena throughout the Universe, such as in magnetospheric substorms, gamma-ray bursts, and accretion disks. The Sun is a unique laboratory to better understand these fundamental physical processes. -
Effects of the Interplanetary Magnetic Field Y Component on the Dayside
Liou and Mitchell Geosci. Lett. (2019) 6:11 https://doi.org/10.1186/s40562-019-0141-3 RESEARCH LETTER Open Access Efects of the interplanetary magnetic feld y component on the dayside aurora K. Liou* and E. Mitchell Abstract A dawn–dusk asymmetry in many high-latitude ionospheric and magnetospheric phenomena, including the aurora, can be linked to the east–west (y) component of the interplanetary magnetic feld (IMF). Owing to the scarcity of observations in the Southern Hemisphere, most of the previous fndings are associated with the Northern Hemi- sphere. It has long been suspected that if the IMF By component also produces a dawn–dusk asymmetry and/or a mirror image in the Southern Hemisphere as predicted by some theories. The present study explores the efect of the IMF By component on the dayside aurora from both hemispheres by analyzing the auroral emission data from the Global UltraViolet scanning spectrograph Imager on board the Thermosphere Ionosphere Mesosphere Energetics and Dynamics mission spacecraft from 2002 to 2007. The data set comprises 28,774 partial images of the northern hemispheric oval and 29,742 partial images of the southern hemispheric oval, allowing for a statistical analysis. It is found that even though auroras in diferent regions of the dayside oval respond diferently to the orientation of the IMF By component, their responses are opposite between the two hemispheres. For example, at ~ 1400–1600 MLT in the Northern Hemisphere, where the so-called 1500 MLT auroral hot spots occur, peak auroral energy fux is larger for negative IMF By comparing to positive IMF By. -
And Type Ii Solar Outbursts
X-641-65-68 / , RADIO EMISSION FROM SHOCK WAVES - AND TYPE II SOLAR OUTBURSTS FEBRUARY 1965 \ -1 , GREENBELT, MARYLAND , X-641-65- 68 RADIO EMISSION FROM SHOCK WAVES AND TYPE II SOLAR OUTBURSTS bY Derek A. Tidman February 1965 NASA-Goddard Space Flight Center Greenbelt, Maryland * RADIO EMISSION FROM SHOCK WAVES AND TYPE 11 SOLAR OUTBURSTS Derek A. Tidman* NASA-Goddard Space Flight Center Greenbelt, Maryland ABSTRACT A model for Type 11 solar radio outbursts is discussed. The radiation is hypothesized to originate in the process of collective bremsstrahlung emitted by non-thermal electron and ion density fluctuations in a plasma containing a flux of energetic electrons. The source of radiation is assumed to be a collisionless plasma shock wave rising through the solar corona. It is also suggested that the collisionless bow shocks of the earth and planets in the solar wind might be similar but weaker sources of low frequency emission with a similar two- harmonic structure to Type 11 emission. * Permanent address: Institute for Fluid Dynamics and Applied Mathematics, University of Maryland, College Park, Maryland. iii RADIO EMISSION FROM SHOCK WAVES AND TYPE II SOLAR OUTBURSTS by Derek A. Tidman NASA-Goddard Space Flight Center Greenbelt, Maryland INTRODUCTION In a previous paper' we calculated the bremsstrahlung emitted from thermal plasmas which co-exist with a flux of energetic (suprathermal) electrons. It was found that under some circumstances the radiation emitted from such plasmas can be greatly increased compared to the emission from a Maxwellian plasma with no energetic particles present. The enhanced emission occurs at the funda- mental and second harmonic of the electron plasma frequency. -
NSF Current Newsletter Highlights Research and Education Efforts Supported by the National Science Foundation
March 2012 Each month, the NSF Current newsletter highlights research and education efforts supported by the National Science Foundation. If you would like to automatically receive notifications by e-mail or RSS when future editions of NSF Current are available, please use the links below: Subscribe to NSF Current by e-mail | What is RSS? | Print this page | Return to NSF Current Archive Robotic Surgery Systems Shipped to Medical Research Centers A set of seven identical advanced robotic-surgery systems produced with NSF support were shipped last month to major U.S. medical research laboratories, creating a network of systems using a common platform. The network is designed to make it easy for researchers to share software, replicate experiments and collaborate in other ways. Robotic surgery has the potential to enable new surgical procedures that are less invasive than existing techniques. The developers of the Raven II system made the decision to share it as the best way to move the field forward--though it meant giving competing laboratories tools that had taken them years to develop. "We decided to follow an open-source model, because if all of these labs have a common research platform for doing robotic surgery, the whole field will be able to advance more quickly," said Jacob Rosen, Students with components associate professor of computer engineering at the University of of the Raven II surgical California-Santa Cruz. Rosen and Blake Hannaford, director of the robotics systems. Credit: University of Washington Biorobotics Laboratory, led the team that Carolyn Lagattuta built the Raven system, initially with a U.S. -
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. -
Arxiv:1712.09051V1 [Astro-Ph.SR] 25 Dec 2017
Solar Physics DOI: 10.1007/•••••-•••-•••-••••-• Origin of a CME-related shock within the LASCO C3 field-of-view V.G.Fainshtein1 · Ya.I.Egorov1 c Springer •••• Abstract We study the origin of a CME-related shock within the LASCO C3 field-of-view (FOV). A shock originates, when a CME body velocity on its axis surpasses the total velocity VA + VSW , where VA is the Alfv´envelocity, VSW is the slow solar wind velocity. The formed shock appears collisionless, because its front width is manifold less, than the free path of coronal plasma charged particles. The Alfv´envelocity dependence on the distance was found by using characteristic values of the magnetic induction radial component and of the proton concentration in the Earth orbit, and by using the known regularities of the variations in these solar wind characteristics with distance. A peculiarity of the analyzed CME is its formation at a relatively large height, and the CME body slow acceleration with distance. We arrived at a conclusion that the formed shock is a bow one relative to the CME body moving at a super Alfv´envelocity. At the same time, the shock formation involves a steeping of the front edge of the coronal plasma disturbed region ahead of the CME body, which is characteristic of a piston shock. Keywords: Sun, Coronal Mass Ejection, Shock 1. Introduction The assumption that, ahead of solar material bunches that were earlier thought to be emitted during solar flares, a shock may emerge in the interplanetary space was already stated in 1950s (Gold, 1962). Based on observations of coronal mass ejections (CMEs) in 1973-1974 (Skylab era), Gosling et al., 1976 supposed that a bow shock should emerge ahead of sufficiently fast CEs. -
Analysis of Geomagnetic Storms in South Atlantic Magnetic Anomaly (SAMA)
Analysis of geomagnetic storms in South Atlantic Magnetic Anomaly (SAMA) Júlia Maria Soja Sampaio, Elder Yokoyama, Luciana Figueiredo Prado Copyright 2019, SBGf - Sociedade Brasileira de Geofísica Moreover, Dst and AE indices may vary according to the This paper was prepared for presentation during the 16th International Congress of the geomagnetic field geometry, such as polar to intermediate Brazilian Geophysical Society held in Rio de Janeiro, Brazil, 19-22 August 2019. latitudinal field variations. In this framework, fluctuations Contents of this paper were reviewed by the Technical Committee of the 16th in the geomagnetic field can occur under the influence of International Congress of the Brazilian Geophysical Society and do not necessarily represent any position of the SBGf, its officers or members. Electronic reproduction or the South Atlantic Magnetic Anomaly (SAMA). The SAMA storage of any part of this paper for commercial purposes without the written consent is a region of minimum geomagnetic field intensity values of the Brazilian Geophysical Society is prohibited. ____________________________________________________________________ at the Earth’s surface (Figure 1), and its dipole intensity is decreasing along the past 1000 years (Terra-Nova et. al., Abstract 2017). Geomagnetic storm is a major disturbance of Earth’s In this study we will compare the behavior of the types of magnetosphere resulted from the interaction of solar wind geomagnetic storms basis on AE and Dst indices. and the Earth’s magnetic field. This disturbance depends of the Earth magnetic field geometry, and varies in terms of intensity from the Poles to the Equator. This disturbance is quantified through geomagnetic indices, such as the Dst and the AE indices. -
Solar and Space Physics: a Science for a Technological Society
Solar and Space Physics: A Science for a Technological Society The 2013-2022 Decadal Survey in Solar and Space Physics Space Studies Board ∙ Division on Engineering & Physical Sciences ∙ August 2012 From the interior of the Sun, to the upper atmosphere and near-space environment of Earth, and outwards to a region far beyond Pluto where the Sun’s influence wanes, advances during the past decade in space physics and solar physics have yielded spectacular insights into the phenomena that affect our home in space. This report, the final product of a study requested by NASA and the National Science Foundation, presents a prioritized program of basic and applied research for 2013-2022 that will advance scientific understanding of the Sun, Sun- Earth connections and the origins of “space weather,” and the Sun’s interactions with other bodies in the solar system. The report includes recommendations directed for action by the study sponsors and by other federal agencies—especially NOAA, which is responsible for the day-to-day (“operational”) forecast of space weather. Recent Progress: Significant Advances significant progress in understanding the origin from the Past Decade and evolution of the solar wind; striking advances The disciplines of solar and space physics have made in understanding of both explosive solar flares remarkable advances over the last decade—many and the coronal mass ejections that drive space of which have come from the implementation weather; new imaging methods that permit direct of the program recommended in 2003 Solar observations of the space weather-driven changes and Space Physics Decadal Survey. For example, in the particles and magnetic fields surrounding enabled by advances in scientific understanding Earth; new understanding of the ways that space as well as fruitful interagency partnerships, the storms are fueled by oxygen originating from capabilities of models that predict space weather Earth’s own atmosphere; and the surprising impacts on Earth have made rapid gains over discovery that conditions in near-Earth space the past decade. -
Effect of the Solar Wind Density on the Evolution of Normal and Inverse Coronal Mass Ejections S
A&A 632, A89 (2019) Astronomy https://doi.org/10.1051/0004-6361/201935894 & c ESO 2019 Astrophysics Effect of the solar wind density on the evolution of normal and inverse coronal mass ejections S. Hosteaux, E. Chané, and S. Poedts Centre for mathematical Plasma-Astrophysics (CmPA), Celestijnenlaan 200B, KU Leuven, 3001 Leuven, Belgium e-mail: [email protected] Received 15 May 2019 / Accepted 11 September 2019 ABSTRACT Context. The evolution of magnetised coronal mass ejections (CMEs) and their interaction with the background solar wind leading to deflection, deformation, and erosion is still largely unclear as there is very little observational data available. Even so, this evolution is very important for the geo-effectiveness of CMEs. Aims. We investigate the evolution of both normal and inverse CMEs ejected at different initial velocities, and observe the effect of the background wind density and their magnetic polarity on their evolution up to 1 AU. Methods. We performed 2.5D (axisymmetric) simulations by solving the magnetohydrodynamic equations on a radially stretched grid, employing a block-based adaptive mesh refinement scheme based on a density threshold to achieve high resolution following the evolution of the magnetic clouds and the leading bow shocks. All the simulations discussed in the present paper were performed using the same initial grid and numerical methods. Results. The polarity of the internal magnetic field of the CME has a substantial effect on its propagation velocity and on its defor- mation and erosion during its evolution towards Earth. We quantified the effects of the polarity of the internal magnetic field of the CMEs and of the density of the background solar wind on the arrival times of the shock front and the magnetic cloud. -
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. -
On One Effect of Coronal Mass Ejections Influence on The
On one effect of coronal mass ejections influence on the envelopes of hot Jupiters Zhilkin A.G.,∗ Bisikalo D.V., Kaigorodov P.V. Institute of astronomy of the RAS, Moscow, Russia Abstract It is now established that the hot Jupiters have extensive gaseous (ionospheric) envelopes, which expanding far beyond the Roche lobe. The envelopes are weakly bound to the planet and affected by strong influence of stellar wind fluctuations. Also, the hot Jupiters are lo- cated close to the parent star and therefore the magnetic field of stellar wind is an important factor, determining the structure their magne- tosphere. At the same time, for a typical hot Jupiter, the velocity of stellar wind plasma, flowing around the atmosphere, is close to the Alfv´envelocity. This should result in stellar wind parameters fluctua- tions (density, velocity, magnetic field), that can affect the conditions of formation of bow shock waves around a hot Jupiter, i. e. to switch flow from sub-Alfv´ento super-Alfv´enmode and back. In this paper, based on the results of three-dimensional numerical MHD modeling, it is confirmed that in the envelope of hot Jupiter, which is in Alfv´en point vicinity of the stellar wind, both disappearance and appearance of the bow shock wave occures under the action of coronal mass ejec- tion. The paper also shows that this effect can influence the observa- tional manifestations of hot Jupiter, including luminosity in energetic part of the spectrum. arXiv:1911.02880v1 [astro-ph.EP] 7 Nov 2019 1 Introduction One of the most important tasks of modern astrophysics is to study the mechanisms of mass loss by hot Jupiters. -
Predicting the Magnetic Vectors Within Coronal Mass Ejections Arriving at Earth: 2
Space Weather RESEARCH ARTICLE Predicting the magnetic vectors within coronal mass ejections 10.1002/2015SW001171 arriving at Earth: 1. Initial architecture Key Points: N. P.Savani1,2, A. Vourlidas1, A. Szabo2,M.L.Mays2,3, I. G. Richardson2,4, B. J. Thompson2, • First architectural design to predict A. Pulkkinen2,R.Evans5, and T. Nieves-Chinchilla2,3 a CME’s magnetic vectors (with eight events) 1 2 • Modified Bothmer-Schwenn CME Goddard Planetary Heliophysics Institute (GPHI), University of Maryland, Baltimore County, Maryland, USA, NASA 3 initiation rule to improve reliability Goddard Space Flight Center, Greenbelt, Maryland, USA, Institute for Astrophysics and Computational Sciences (IACS), of chirality Catholic University of America, Washington, District of Columbia, USA, 4Department of Astronomy, University of • CME evolution seen by remote Maryland, College Park, Maryland, USA, 5College of Science, George Mason University, Fairfax, Vancouver, USA sensing triangulation is important for forecasting Abstract The process by which the Sun affects the terrestrial environment on short timescales is Correspondence to: predominately driven by the amount of magnetic reconnection between the solar wind and Earth’s N. P. Savani, magnetosphere. Reconnection occurs most efficiently when the solar wind magnetic field has a southward [email protected] component. The most severe impacts are during the arrival of a coronal mass ejection (CME) when the magnetosphere is both compressed and magnetically connected to the heliospheric environment. Citation: Unfortunately, forecasting magnetic vectors within coronal mass ejections remain elusive. Here we report Savani, N. P., A. Vourlidas, A. Szabo, M.L.Mays,I.G.Richardson,B.J. how, by combining a statistically robust helicity rule for a CME’s solar origin with a simplified flux rope Thompson, A.