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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. -
Estimating Random Transverse Velocities in the Fast Solar Wind from EISCAT Interplanetary Scintillation Measurements
c Annales Geophysicae (2002) 20: 1265–1277 European Geophysical Society 2002 Annales Geophysicae Estimating random transverse velocities in the fast solar wind from EISCAT Interplanetary Scintillation measurements A. Canals1, A. R. Breen1, L. Ofman2, P. J. Moran1, and R. A. Fallows1 1Physics Department, University of Wales, Aberystwyth, Wales, UK 2The Catholic University of America and NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA Received: 17 October 2001 – Revised: 21 February 2002 – Accepted: 13 March 2002 Abstract. Interplanetary scintillation measurements can process of constructive and destructive interference change yield estimates of a large number of solar wind parameters, these phase variations into amplitude variations. As the ir- including bulk flow speed, variation in bulk velocity along regularities move out in the solar wind, the effect is to cast a the observing path through the solar wind and random varia- drifting diffraction pattern across the Earth. If the pattern is tion in transverse velocity. This last parameter is of particular sampled using two radio telescopes when the ray paths from interest, as it can indicate the flux of low-frequency Alfven´ the radio source to the antenna lie in the same radial plane – waves, and the dissipation of these waves has been proposed a plane passing through the center of the Sun – then a high as an acceleration mechanism for the fast solar wind. Anal- degree of correlation is present between the scintillation at ysis of IPS data is, however, a significantly unresolved prob- the two sites. The time lag for maximum correlation pro- lem and a variety of a priori assumptions must be made in in- vides a direct estimation of the scintillation drift velocity. -
Radio Scintillation Observations of the Solar Wind - Recent Results from Eiscat and Proposals for a New-Generation System
RADIO SCINTILLATION OBSERVATIONS OF THE SOLAR WIND - RECENT RESULTS FROM EISCAT AND PROPOSALS FOR A NEW-GENERATION SYSTEM A.R. Breen(1), G. Woan(2) (1)University of Wales Aberystwyth, Ceredigion SY23 3BZ, Wales, Email: [email protected] (2)University of Glasgow, Glasgow G12 8QQ, Scotland, Email: [email protected] ABSTRACT the spectral shape measured by a single antenna [2, 3] Measurements of radio scintillation which use the or – with greater accuracy, from the form of the cross- motion of ~100 km scale size density irregularities as spectra of the scintillation patterns measured at two flow tracers for solar wind speed (the technique of widely-separated sites at a time when the raypaths from Interplanetary Scintillation or IPS) have been used to source to antennas lie in a plane radial to the Sun [4, 5]. study the solar wind for many years. Recently Single antenna systems can make many more improvements to analysis methods have transformed observations but velocities derived from multi-site the capabilities of this technique and it has emerged as systems allow more accurate estimates of velocity [6]. a powerful tool for probing regions of the solar wind IPS measurements contain contributions from the which are hard to study by other means - particularly whole of the extended ray-path through the solar the region from ~25 solar radii (R) out to ~100 R. As atmosphere from the distant source to the receiving this is the region in which interaction between streams antenna(s). In earlier studies the inability to distinguish of solar wind and between mass ejections and the between contributions from different regions of the background wind determine the solar wind structure solar wind led to a "blurred" view of solar wind seen at Earth orbit good measurements of this region structure. -
Survey of Conditions for Artificial Aurora Experiments at EISCAT
Tsuda et al. Earth, Planets and Space (2018) 70:40 https://doi.org/10.1186/s40623-018-0805-9 TECHNICAL REPORT Open Access Survey of conditions for artifcial aurora experiments at EISCAT Tromsø using dynasonde data T. T. Tsuda1* , M. T. Rietveld2,3, M. J. Kosch4,5,6, S. Oyama7,8, K. Hosokawa1, S. Nozawa7, T. Kawabata7, A. Mizuno7 and Y. Ogawa8,9 Abstract We report a brief survey on conditions for artifcial aurora optical experiments in F region heating with O-mode at the EISCAT Tromsø site using dynasonde data from 2000 to 2017. The results obtained in our survey indicate the follow- ing: The possible conditions for conducting artifcial aurora experiments are concentrated in twilight hours in both evening and morning, compared with late-night hours; the possible conditions appear in fall, winter, and spring, while there is no chance in summer, and the month-to-month variation among fall, winter, and spring is not clear. The year- to-year variation is well correlated with the solar cycle, and experiments during the solar minimum would be almost hopeless. These fndings are useful for planning future artifcial aurora optical experiments. Keywords: Artifcial aurora, Ionospheric heating, EISCAT, Tromsø, Dynasonde Background heating experiments with O-mode polarization during Many researchers have been working on ionospheric nighttime to detect optical emissions in artifcial auro- heating experiments using high frequency (HF) radio ras (e.g., Gustavsson et al. 2005; Bryers et al. 2013; Kosch waves to understand phenomenon such as the interac- et al. 2014a, b; Blagoveshchenskaya et al. 2014). Tese tion processes between radio waves and plasma particles, published papers are obviously based on successful heat- which is an essential part of plasma physics. -
Observations of Polar Cap Patch Substructures by EISCAT Svalbard Radar
UNIVERSITY OF OSLO Department of Physics Observations of Polar Cap Patch Substructures by EISCAT Svalbard Radar Master Thesis Karina E. Bravo Ibáñez 1 May 2009 2 Preface The University in Oslo (UiO) gave me the opportunity to start a master in Space Physics. I am glad to have met many people related to space studies. I had the opportunity to take courses at the University centre in Svalbard (UNIS). Apart from the interesting theory background in space physics gained there, it was a great experience to live near the North Pole, and I will always have in mind the white mountains, the 24 hrs with darkness/sunlight, the exciting trips to the observatory stations, and of course the astonishing northern lights. I also had the chance to attend the International Space University Summer School Program (ISU SSP 2009) held in Barcelona thanks to the Norwegian Space Centre and, of course, to Ellen Osmundsen, Yvonne Rinne, Jøran Moen and Hans Pécseli for helping me with the application. I would like to thank my supervisors Jøran Moen and Kjellmar Oksavik for their help and guidance during this thesis, for their many interesting ideas on the subject and for always being available no matter the distance. I also thank Bjørn Lybekk and Espen Trondsen for technical assistance. I acknowledge the use of EISCAT data provided by the database in Kiruna, the use of ACE data provided by the ACE MAG and SWEPAM instruments teams, also the use of SuperDARN data provided by the John Hopkins University Applied Physics Laboratory. Thanks to Todd Pedersen who provided the scintillation data. -
Estimates of Magnetotail Reconnection Rate Based on IMAGE FUV and EISCAT Measurements
Annales Geophysicae (2005) 23: 123–134 SRef-ID: 1432-0576/ag/2005-23-123 Annales © European Geosciences Union 2005 Geophysicae Estimates of magnetotail reconnection rate based on IMAGE FUV and EISCAT measurements N. Østgaard1, J. Moen2,3, S. B. Mende1, H. U. Frey1, T. J. Immel1, P. Gallop4, K. Oksavik2, and M. Fujimoto5 1Space Sciences Laboratory, University of California, Berkeley, California, USA 2Department of Physics, University of Oslo, Norway 3University Centre on Svalbard, Longyearbyen, Norway 4Rutherford Appleton Laboratory, Oxfordshire, UK 5Department of Earth and Planetary Sciences, Tokyo Institute of Technology, Japan Received: 16 September 2003 – Revised: 15 March 2004 – Accepted: 30 March 2004 – Published: 31 January 2005 Part of Special Issue “Eleventh International EISCAT Workshop” Abstract. Dayside merging between the interplanetary and additional lower frequencies, 0.5 and 0.8 mHz, that might be terrestrial magnetic fields couples the solar wind electric field modulated by solar wind pressure variations. to the Earth’s magnetosphere, increases the magnetospheric Key words. Magnetospheric physics (magnetotail; electric convection and results in efficient transport of solar wind en- fields; magnetosphere - ionosphere interaction; solar wind - ergy into the magnetosphere. Subsequent reconnection of the magnetosphere interaction). Space plasma physics (magnetic lobe magnetic field in the magnetotail transports energy into reconnection) the closed magnetic field region. Combining global imag- ing and ground-based radar measurements, we estimate the reconnection rate in the magnetotail during two days of an EISCAT campaign in November-December 2000. Global 1 Introduction images from the IMAGE FUV system guide us to identify ionospheric signatures of the open-closed field line bound- A fundamental element of the open magnetosphere model ary observed by the two EISCAT radars in Tromsø (VHF) first suggested by Dungey (1961) is that dayside merging and on Svalbard (ESR). -
EISCAT Observation of Wave‐Like Fluctuations in Vertical Velocity Of
View metadata, citation and similar papers at core.ac.uk brought to you by CORE provided by Munin - Open Research Archive Journal of Geophysical Research: Space Physics RESEARCH ARTICLE EISCAT Observation of Wave-Like Fluctuations in Vertical 10.1029/2018JA025399 Velocity of Polar Mesospheric Summer Echoes Key Points: Associated With a Geomagnetic Disturbance • Vertical velocity of PMSE was observed to oscillate at near- Young-Sook Lee1 , Yong Ha Kim1 , Kyung-Chan Kim2 , Young-Sil Kwak3,4 , buoyancy period of mesosphere after 5 5 6 the onset of substorm Timothy Sergienko , Sheila Kirkwood , and Magnar G. Johnsen • Variation of PMSE intensity is well 1 2 correlated with that of E region Department of Astronomy and Space Science, Chungnam National University, Daejeon, South Korea, Division of Science electron density Education, College of Education, Daegu University, Gyeongsan, South Korea, 3Korea Astronomy and Space Science • Initial creation of PMSE is induced by Institute, Daejeon, South Korea, 4Department of Astronomy and Space Science, University of Science and Technology, both particle precipitation and air Daejeon, South Korea, 5Swedish Institute of Space Physics, Kiruna, Sweden, 6Tromsø Geophysical Observatory, UiT-The updraft that was observed as large upward velocity Arctic University of Norway, Tromsø, Norway Supporting Information: Abstract By analyzing a data set from the European Incoherent SCATter (EISCAT) Very High Frequency • Supporting Information S1 (VHF) radar at Tromsø, we find that both radar reflectivity and upward ion velocity in a polar mesospheric • Figure S1 summer echo (PMSE) layer simultaneously increased at the commencement of a local geomagnetic disturbance, which occurred at midnight on 9 July 2013. The onset of the upward velocity was followed by Correspondence to: Y. -
Rumba, Salsa, Smaba and Tango in the Magnetosphere
ESCOUBET 24-08-2001 13:29 Page 2 r bulletin 107 — august 2001 42 ESCOUBET 24-08-2001 13:29 Page 3 the cluster quartet’s first year in space Rumba, Salsa, Samba and Tango in the Magnetosphere - The Cluster Quartet’s First Year in Space C.P. Escoubet & M. Fehringer Solar System Division, Space Science Department, ESA Directorate of Scientific Programmes, Noordwijk, The Netherlands P. Bond Cranleigh, Surrey, United Kingdom Introduction Launch and commissioning phase Cluster is one of the two missions – the other When the first Soyuz blasted off from the being the Solar and Heliospheric Observatory Baikonur Cosmodrome on 16 July 2000, we (SOHO) – constituting the Solar Terrestrial knew that Cluster was well on the way to Science Programme (STSP), the first recovery from the previous launch setback. ‘Cornerstone’ of ESA’s Horizon 2000 However, it was not until the second launch on Programme. The Cluster mission was first 9 August 2000 and the proper injection of the proposed in November 1982 in response to an second pair of spacecraft into orbit that we ESA Call for Proposals for the next series of knew that the Cluster mission was truly back scientific missions. on track (Fig. 1). In fact, the experimenters said that they knew they had an ideal mission only The four Cluster spacecraft were successfully launched in pairs by after switching on their last instruments on the two Russian Soyuz rockets on 16 July and 9 August 2000. On 14 fourth spacecraft. August, the second pair joined the first pair in highly eccentric polar orbits, with an apogee of 19.6 Earth radii and a perigee of 4 Earth radii. -
Small-Scale Flux Transfer Events Formed in the Reconnection Exhaust Region Between Two X Lines
Journal of Geophysical Research: Space Physics RESEARCH ARTICLE Small-Scale Flux Transfer Events Formed in the Reconnection 10.1029/2018JA025611 Exhaust Region Between Two X Lines Key Points: K.-J. Hwang1 , D. G. Sibeck2 , J. L. Burch1 , E. Choi1 , R. C. Fear3 , B. Lavraud4 , • fl MMS observation of ion-scale ux 2 2 5 6 7 ropes in the reconnection outflow B. L. Giles , D. Gershman , C. J. Pollock , J. P. Eastwood , Y. Khotyaintsev , 8 9 10 11 12 region Philippe Escoubet ,H.Fu , S. Toledo-Redondo , R. B. Torbert , R. E. Ergun , • The initial X line is embedded in the W. R. Paterson2 , J. C. Dorelli2 , L. Avanov2,13 , C. T. Russell14 , and R. J. Strangeway14 exhaust region downstream of a second X line 1Southwest Research Institute, San Antonio, TX, USA, 2NASA Goddard Space Flight Center, Greenbelt, MD, USA, 3Physics • Flux transfer events (FTE) are formed 4 between the two X lines due to and Astronomy, University of Southampton, Southampton, UK, Institut de Recherche en Astrophysique et Planétologie, 5 6 tearing instability CNRS, UPS, CNES, Université de Toulouse, Toulouse, France, Denali Scientific, LLC, Fairbanks, AK, USA, Imperial College, London, UK, 7Swedish Institute of Space Physics, Uppsala, Sweden, 8European Space Agency, Noordwijk, Netherlands, 9School of Space and Environment, Beihang University, Beijing, China, 10European Space Agency, ESAC, Madrid, Spain, 11Space Science Center, University of New Hampshire, Durham, NH, USA, 12Laboratory for Atmospheric and Space Physics, Correspondence to: University of Colorado Boulder, Boulder, CO, USA, 13The Goddard Planetary Heliophysics Institute, Baltimore, MD, USA, K.-J. Hwang, 14 [email protected] Institute of Geophysics and Planetary Physics, University of California, Los Angeles, CA, USA Citation: Abstract We report MMS observations of the ion-scale flux transfer events (FTEs) that may involve two Hwang, K.-J., Sibeck, D. -
Solar Wind Magnetic Field Components
Characteristics of a HSS-driven magnetic storm in the high-latitude ionosphere N. Ellahouny, A. Aikio, M. Pedersen, H. Vanhamäki, I. Virtanen, J. Norberg, M. Grandin, Al.Kozlovsky, T. Raita, K. Kauristie, A. Marchaudon, P.-L. Blelly, S.-I. Oyama 1) Ionospheric Physics Research Unit, University of Oulu, Finland, 2) Finnish Meteorological Institute, Helsinki, 3) CoE in Sustainable Space, University of Helsinki 4) Sodankylä Geophysical Observatory, Finland, 5) IRAP, University of Tolouse, France,6) Institute for Space-Earth Environmental Research, Nagoya University, Nagoya, Japan Email: [email protected] SS1 SS2 SS3 SS4 SS5 SS6 SS7 SS8 SS9 SS10 SS11 SS12 SS13 (a) 1. Introduction Solar wind high-speed streams (HSSs) >400 km/s that (b) emanate from Solar coronal holes have a significant impact on the geomagnetic activity during the declining phase of the solar cycle [Gonzalez et al., 1999; Tsurutani et al.,2006]. When HSSs catch up the preceding slow solar wind, they (c) create a compressed plasma region, called co-rotating interaction region (CIR). HSSs can induce geomagnetic storms that last for several days [Borovsky and Denton, (d) 2006] and affect the ionospheric behavior, specially at the high latitudes [Grandin et al., 2015; Marchaudon et al., 2018]. When a magnetospheric substorm takes place, (e) injection of electrons and protons occur. In this poster, we present one of the longest storms in the current solar cycle (24) that occurred on 14th of March 2016. (f) 2. Data and initial results 2.1 Solar wind driver Figure 2 Solar wind parameters and magnetic indices during (14-22 March 2016). -
Observing and Analysing Structures in Active Aurora with the ASK Optical Instrument and EISCAT Radar
Motivating talk on exciting work with EISCAT: Observing and analysing structures in active aurora with the ASK optical instrument and EISCAT radar. EISCAT Summer School part I - 31st July 2007 Hanna Dahlgren (KTH, Sweden) & Daniel Whiter (University of Southampton, UK) 1 (25) Auroral Spatial Scales Oval up to 1000 km Large-Scale Inverted-V 100 km Inverted-V Arc 10 km 100 km Filaments 1 km o v a l 1 arcs 5-20 km 0 0 0 k m DMSP auroralauroral rays rays Black auroral auroral fine- curls: 1 km widths structure < 1 km 2 (25) Ground-based observations of the fine-scale aurora Examples of discrete auroral structures 0.1 to 1 km wide T.Trondsen (Univ of Calgary) Few instruments can measure it well Few theoretical models can account for it 3 (25) Our Motivation • Optical data provides information on morphology of the aurora. • Simultaneous radar measurements give additional information on ionospheric properties. • We focus on the smallest structures seen, by using high-resolution imagers, equipped with different filters to measure specific emissions. - The EISCAT radars give us information on the condition of the ionosphere at the time, electric fields and flows. This is used in our modelling of the ionosphere. 4 (25) ASK Auroral Structure and Kinetics Instrument to study small scale structure of the aurora, at high temporal and spatial resolution. Three narrow FOV cameras for simultaneous imaging in three spectral bands: + - ASK1a: 5620 Å → O2 (E-region, high energy e ) - ASK1b: 6730 Å → N2 (E-region, high energy e ) ASK2a: 7320 Å → O+ (F-region, -
The UV Aurora and Ionospheric Flows During Flux Transfer Events D
The UV aurora and ionospheric flows during flux transfer events D. A. Neudegg, S. W. H. Cowley, K. A. Mcwilliams, M. Lester, T. K. Yeoman, J. B. Sigwarth, G. Haerendel, W. Baumjohann, U. Auster, G.-H. Fornacon, et al. To cite this version: D. A. Neudegg, S. W. H. Cowley, K. A. Mcwilliams, M. Lester, T. K. Yeoman, et al.. The UV aurora and ionospheric flows during flux transfer events. Annales Geophysicae, European Geosciences Union, 2001, 19 (2), pp.179-188. hal-00316762 HAL Id: hal-00316762 https://hal.archives-ouvertes.fr/hal-00316762 Submitted on 1 Jan 2001 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. c Annales Geophysicae (2001) 19: 179–188 European Geophysical Society 2001 Annales Geophysicae The UV aurora and ionospheric flows during flux transfer events D. A. Neudegg1,*, S. W. H. Cowley1, K. A. McWilliams1, M. Lester1, T. K. Yeoman1, J. Sigwarth2, G. Haerendel3, W. Baumjohann3, U. Auster4, K.-H. Fornacon4, and E. Georgescu5 1Department of Physics and Astronomy, Leicester University, Leicester LE1 7RH, UK 2Department of Physics, University of Iowa, USA 3Max-Planck Institut für Extraterrestrische Physik, Garching, Germany 4Technische Universität von Braunschweig, Braunschweig, Germany 5Institute of Space Science, Bucharest, Romania *Now at: Rutherford-Appleton Laboratory, Oxfordshire OX11 0QX, UK Received: 24 July 2000 – Revised: 11 December 2000 – Accepted: 12 December 2000 Abstract.