Solar flare effect on the geomagnetic field and ionosphere |
| |
| Authors: | A Meza MA Van Zele M Rovira |
| |
| Institution: | 1. Facultad de Cs. Astronómicas y Geofísicas, Universidad Nacional de La Plata, La Plata, Argentina;2. Consejo Nacional de Investigaciones Científicas y Técnicas (CONICET), Buenos Aires, Argentina;3. Facultad de Ciencias Exactas y Naturales, Universidad de Buenos Aires, Argentina;4. Instituto de Astronomía y Física del Espacio (IAFE), Buenos Aires, Argentina;1. South-Center University for Nationalities, Wuhan 430074;2. National Satellite Meteorology Center for Space Weather, China Meteorological Administration, Beijing 100081;3. Nanjing University of Information Science and Technology, Nanjing 210044;1. Scientific Research Center “Kosmos”, MoD, Moscow, Russia;2. Central Research Institute of Machine Building (TsNIIMash), Korolev, Moscow Region, Russia;3. Institute of Geosphere Dynamics, RAS, Moscow, Russia;4. Institute of Monitoring of Climatic and Ecological System, SB RAS, Tomsk, Russia;1. Parthenope University of Napoli, Department of Sciences and Technologies, Centro Direzionale, Isola C4, I-80143 Napoli, Italy;2. Università degli Studi di Torino, Dipartimento di Fisica, Via P. Giuria 1, I-10125 Torino, Italy;1. Department of Physics and Astronomy, George Mason University, Fairfax, Virginia, USA;2. Institute of Atmospheric Physics, Czech Academy of Sciences, Czech Republic;3. Bulgarian Academy of Sciences, Department of Space Weather, Bulgaria;4. University of New Brunswick, Canada;1. Graz University of Technology, Graz, Austria;2. Space Research Institute, Austrian Academy of Sciences, Graz, Austria |
| |
| Abstract: | This paper studies the ionospheric and geomagnetic response to an X6.2 solar flare recorded at 14:30 UT on December 13, 2001, in quiet geomagnetic conditions which allow the variations in the geomagnetic field and ionosphere measurements to be easily related to the solar flare radiation.By using measurements from the global positioning system (GPS) and geomagnetic observatories, the temporal evolution of ionospheric total electron content variation, vTECV, and geomagnetic field variations, δB, as well as their rates of variation, were obtained around the subsolar point at different solar zenith angles. The enhancement of both parameters was recorded one to three minutes later than the Geostationary Operational Environmental Satellite (GOES) programme recording; such delay tends to depend on the latitude, longitude, and solar zenith angle of the observatory's observations.The vTECV is related to the local time and the δB to the intensity and position of the ionospheric currents.The vTECV′s maximum value is always recorded later than the maximum values reached by δB and the X-ray intensity. The maximum δB is larger in the local morning than in the afternoon.The rates of vTECV and δB have two maximum values at the same time as the maximum values recorded by Hα (for each ribbon).This work shows the quantitative and qualitative relations between a solar flare and the ionospheric and geomagnetic variations that it produces. |
| |
| Keywords: | |
| 本文献已被 ScienceDirect 等数据库收录！ |
|
