A study of the meridional structure of the equatorial red arcs in the night-time ionosphere from the ISIS-II satellite |
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| Institution: | 1. Fachbereich Mathematik und Technik, RheinAhrCampus, Koblenz University of Applied Sciences, Remagen, Germany;2. School of Biology, University of St Andrews, St Andrews, U.K.;1. Zuva Energy, New York, USA;2. Department of Photonics Engineering, Technical University of Denmark, Roskilde, Denmark;3. Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), Madrid, Spain;4. National Renewable Energy Laboratory, Golden, USA;5. Laboratório Fotovoltaica/UFSC, Universidade Federal de Santa Catarina, Florianópolis, Brazil;6. Key Laboratory of Solar Energy Utilization & Energy Saving Technology of Zhejiang Province, China;7. Departamento de Física, Universidad de Santiago de Chile, Santiago, Chile;8. Commonwealth Scientific and Industrial Research Organisation (CSIRO) Energy, Newcastle, Australia;9. FOSS Research Centre for Sustainable Energy, University of Cyprus, Cyprus;10. Florida Solar Energy Center (FSEC), Cocoa, USA;11. Research and Development Center, Dubai Electricity and Water Authority (DEWA), MBR Solar Park, Dubai UAE;12. School of Renewable Energy and Smart Grid Technology, Naresuan University, Thailand;13. Universidad de Huelva, Huelva, Spain;14. Institute for Renewable Energy, Eurac Research, Bolzano, Italy;15. Council for Scientific and Industrial Research (CSIR), Pretoria, South Africa;p. Department of Electrical and Electronic Engineering, Ritsumeikan University, Kusatsu, Japan;q. Center for Energy, Austrian Institute of Technology - AIT, Vienna, Austria;r. Brazilian National Institute for Space Research (INPE), São José dos Campos, SP, Brazil;s. IDEA Research Group, Center for Advanced Studies in Earth Science, Energy and Environment (CEACTEMA), University of Jaén, Jaén, Spain;t. University of Agder, Faculty of Engineering and Sciences, Grimstad, Norway;u. Natural Resources Canada, Ottawa, Canada;v. Solar Energy Research Institute of Singapore (SERIS), National University of Singapore (NUS), Singapore;w. Utrecht University, Copernicus Institute of Sustainable Development, Utrecht, Netherlands;x. Departamento de Ciencias, Sección Física, Pontificia Universidad Católica Del Perú, Lima, Peru;y. Sandia National Laboratories, Albuquerque, USA;z. Helmholtz-Zentrum Berlin, Berlin, Germany;11. Key Laboratory of Middle Atmosphere and Global Environment Observation (LAGEO), Institute of Atmospheric Physics, Chinese Academy of Sciences, Beijing, China;22. Instituto de Astronomia, Geofísica e Ciências Atmosféricas, Universidade de São Paulo, São Paulo, Brazil;1. Graduate School of Engineering, Chiba University, Chiba 263-8522, Japan;2. Molecular Chirality Research Centre, Chiba University, Chiba 263-8522, Japan;3. Institute for Advanced Academic Research, Chiba University, Chiba 263-8522, Japan;1. Department of Aerospace Engineering, Khalifa University of Science and Technology, Abu Dhabi P.O. Box 127788, United Arab Emirates;2. Centre Internacional de Mètodes Numèrics en Enginyeria (CIMNE), Gran Capità s/n, 08034 Barcelona, Spain |
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| Abstract: | Equatorial 6300 Å arcs observed by the ISIS—II satellite close to the magnetic equator over the African and Asian zones are studied for night-time conditions from 21:00 h to 02:00 h local time in the summer and spring of 1972–1974 and 1976, respectively. Case studies of the arcs have been made for quiet geomagnetic conditions and for minor storms. Sometimes very intense arcs with intensities of 1–2 kR are observed. Arcs of moderate intensities (300–400 R) are observed during geomagnetically disturbed periods. It is confirmed that these intensities can be fully accounted for theoretically by the dissociative recombination of molecular oxygen ions. Since the emission intensities are found to be sensitive to the geomagnetic activity, the influence of the latter has been taken into account and discussed.Equatorial spread-F (ESF)/bubble conditions are usually present at these local times. The data presented here show a correlation between the 6300 Å emission rate at one of the anomaly crests, the gradient in h (the lowest scaled real height from topside ionosonde trace) and the existence of ESF and gravity waves. This correlation is consistent with the scenario put forward by Maruyama and Matuura that the occurrence of ESF requires a symmetrical electron density distribution around the magnetic equator, so that a transequatorial wind causes an asymmetry and inhibits the formation of ESF.For the ISIS data we conclude that where strong transequatorial winds exist the 6300 Å emission rate at one of the anomaly crests is very large and there is a steep gradient in h. When these winds are weak, the 6300 Å emission is low and the gradient in h is also small. In the latter case, gravity waves of wavelength 200–400 km were present as well, which suggests that ESF is promoted by the existence of gravity waves. However, the magnetic disturbance level was higher during these orbits, which offers another source of gravity waves. |
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