Solar flare effect on the geomagnetic field and ionosphere
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 me...
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2009
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| LEADER | 12991caa a22012017a 4500 | ||
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| 001 | PAPER-8600 | ||
| 003 | AR-BaUEN | ||
| 005 | 20250924081517.0 | ||
| 008 | 190411s2009 xx ||||fo|||| 00| 0 eng|d | ||
| 024 | 7 | |2 scopus |a 2-s2.0-67650552849 | |
| 040 | |a Scopus |b spa |c AR-BaUEN |d AR-BaUEN | ||
| 100 | 1 | |a Meza, A. | |
| 245 | 1 | 0 | |a Solar flare effect on the geomagnetic field and ionosphere |
| 260 | |c 2009 | ||
| 270 | 1 | 0 | |m Meza, A.; Facultad de Cs. Astronómicas y Geofísicas, Universidad Nacional de La Plata, La Plata, Argentina; email: ameza@fcaglp.fcaglp.unlp.edu.ar |
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| 506 | |2 openaire |e Política editorial | ||
| 520 | 3 | |a 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, vTEC V , 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 vTEC V is related to the local time and the δB to the intensity and position of the ionospheric currents. The vTEC V ′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 vTEC V 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. © 2009 Elsevier Ltd. All rights reserved. |l eng | |
| 536 | |a Detalles de la financiación: Kyoto University | ||
| 536 | |a Detalles de la financiación: Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata | ||
| 536 | |a Detalles de la financiación: Universidad de Buenos Aires | ||
| 536 | |a Detalles de la financiación: Consejo Nacional de Investigaciones Científicas y Técnicas | ||
| 536 | |a Detalles de la financiación: Universidad Nacional de La Plata, UNLP | ||
| 536 | |a Detalles de la financiación: Facultad de Ciencias Físicas y Matemáticas | ||
| 536 | |a Detalles de la financiación: The authors are very grateful to world data centres for the free availability of the data: WDC-C Kyoto University, Japan; Service International des Indices Geomagnetiques, Bureau des Publications SIIG, France; Consejo Nacional de Investigaciones Científicas y Técnicas, Argentina; Facultad de Ciencias Exactas y Naturales (Universidad de Buenos Aires), Argentina; and Facultad de Ciencias Astronómicas y Geofísicas (Universidad Nacional de La Plata), Argentina. | ||
| 593 | |a Facultad de Cs. Astronómicas y Geofísicas, Universidad Nacional de La Plata, La Plata, Argentina | ||
| 593 | |a Consejo Nacional de Investigaciones Científicas y Técnicas (CONICET), Buenos Aires, Argentina | ||
| 593 | |a Facultad de Ciencias Exactas y Naturales, Universidad de Buenos Aires, Argentina | ||
| 593 | |a Instituto de Astronomía y Física del Espacio (IAFE), Buenos Aires, Argentina | ||
| 690 | 1 | 0 | |a GEOMAGNETIC FIELD |
| 690 | 1 | 0 | |a GPS |
| 690 | 1 | 0 | |a SOLAR FLARE EFFECT |
| 690 | 1 | 0 | |a TEC |
| 690 | 1 | 0 | |a GEOMAGNETIC CONDITIONS |
| 690 | 1 | 0 | |a GEOMAGNETIC FIELD |
| 690 | 1 | 0 | |a GEOMAGNETIC FIELD VARIATIONS |
| 690 | 1 | 0 | |a GEOMAGNETIC FIELDS |
| 690 | 1 | 0 | |a GEOMAGNETIC VARIATION |
| 690 | 1 | 0 | |a GEOSTATIONARY OPERATIONAL ENVIRONMENTAL SATELLITES |
| 690 | 1 | 0 | |a GPS |
| 690 | 1 | 0 | |a IONOSPHERIC CURRENT |
| 690 | 1 | 0 | |a IONOSPHERIC TOTAL ELECTRON CONTENT |
| 690 | 1 | 0 | |a LOCAL TIME |
| 690 | 1 | 0 | |a MAXIMUM VALUES |
| 690 | 1 | 0 | |a QUALITATIVE RELATION |
| 690 | 1 | 0 | |a SOLAR FLARE |
| 690 | 1 | 0 | |a SOLAR FLARE EFFECT |
| 690 | 1 | 0 | |a SOLAR ZENITH ANGLE |
| 690 | 1 | 0 | |a SUBSOLAR POINTS |
| 690 | 1 | 0 | |a TEC |
| 690 | 1 | 0 | |a TEMPORAL EVOLUTION |
| 690 | 1 | 0 | |a X RAY INTENSITY |
| 690 | 1 | 0 | |a BUILDINGS |
| 690 | 1 | 0 | |a GEOSTATIONARY SATELLITES |
| 690 | 1 | 0 | |a GLOBAL POSITIONING SYSTEM |
| 690 | 1 | 0 | |a IONOSPHERE |
| 690 | 1 | 0 | |a IONOSPHERIC MEASUREMENT |
| 690 | 1 | 0 | |a OBSERVATORIES |
| 690 | 1 | 0 | |a SATELLITE OBSERVATORIES |
| 690 | 1 | 0 | |a SCANNING |
| 690 | 1 | 0 | |a GEOMAGNETISM |
| 700 | 1 | |a Van Zele, M.A. | |
| 700 | 1 | |a Rovira, Marta Graciela | |
| 773 | 0 | |d 2009 |g v. 71 |h pp. 1322-1332 |k n. 12 |p J. Atmos. Sol.-Terr. Phys. |x 13646826 |w (AR-BaUEN)CENRE-5432 |t Journal of Atmospheric and Solar-Terrestrial Physics | |
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