Equatorial ionospheric responses in relation to the occurrence of main phase of intense geomagnetic storms in the local dusk sector |
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| Authors: | R Hajra SK Chakraborty |
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| Institution: | 1. Photoelectric and Energy Device Application Lab & Department of Electrical Engineering, Incheon National University, Incheon 406772, Republic of Korea;2. Korea Photonics Technology Institute (KOPTI), 9 Chemdan venture-ro, Buk-gu, Gwangju 500460, Republic of Korea;3. Department of Photonic Engineering, Chosun University, 309 Pilmun-daero, Dong-gu, Gwangju 501759, Republic of Korea;1. Institute of Geophysics and Planetary Physics, University of California Los Angeles, Los Angeles, CA, USA;2. Department of Earth, Planetary, and Space Sciences, University of California Los Angeles, Los Angeles, CA, USA;3. Johns Hopkins University Applied Physics Laboratory, Laurel, MD, USA;1. The Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA;2. Data Analysis Center for Geomagnetism and Space Magnetism, Kyoto University, Kyoto, Japan;3. Department of Geophysics, Graduate School of Science, Kyoto University, Kyoto, Japan;1. Instituto de Astronomía y Física del Espacio, Av. Cantilo 2620 Pabellón IAFE (cp 1428), CABA, Buenos Aires, Argentina;2. Departamento de Física, FCEN, UBA, Buenos Aires, Argentina;3. Institut de Recherche en Astrophysique et Planétologie, Toulouse, France;4. Space and Atmospheric Physics, The Blackett Laboratory, Imperial College, London, United Kingdom;1. Instituto Nacional de Pesquisas Espaciais (INPE), Av. dos Astronautas, 1758, Sao Jose dos Campos, SP 12227-010, Brazil;2. Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive Pasadena, California 91109, Pasadena, CA, USA |
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| Abstract: | During five intense geomagnetic storms with main phases occurring around local dusk sector, equatorial ionosonde and electrojet data, VHF/UHF scintillation data of Calcutta, and several solar wind parameters are investigated to ascertain the polarity of prompt penetration electric field (PPEF). Abrupt increases in AE, ASY-H and/or sharp decreases in Dst/SYM-H with strong southward IMF Bz may symbolize eastward PPEF to equatorial latitude leading to evolution of density irregularities if the period is associated with arrival and sustenance of large magnetospheric shock compression. On the contrary, westward PPEF is more feasible if the shock reduces suddenly or fluctuates with small values. |
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