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How Does Large Flaring Activity from the Same Active Region Produce Oppositely Directed Magnetic Clouds? |
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| Authors: | Louise K Harra Nancy U Crooker Cristina H Mandrini Lidia van Driel-Gesztelyi Sergio Dasso Jingxiu Wang Heather Elliott Gemma Attrill Bernard V Jackson Mario M Bisi |
| Institution: | (1) Mullard Space Science Laboratory, University College London, Holmbury St. Mary, Dorking, Surrey, RH5 6NT, UK;(2) Center for Space Physics, Boston University, Boston, MA, USA;(3) Instituto de Astronomía y Física del Espacio, CONICET-UBA, CC. 67, Suc. 28, 1428 Buenos Aires, Argentina;(4) Observatoire de Paris, LESIA, FRE 2461 (CNRS), 92195 Meudon Principal Cedex, France;(5) Konkoly Observatory of the Hungarian Academy of Sciences, Budapest, Hungary;(6) National Astronomical Observatory, Chinese Academy of Sciences, Beijing, China;(7) Departamento de Física, Facultad de Ciencias Exactas y Naturales, Universidad de Buenos Aires, 1428 Buenos Aires, Argentina;(8) Southwest Research Institute, 6220 Culebra Road, San Antonio, TX 78238, USA;(9) Center for Astrophysics and Space Sciences, University of California, San Diego, La Jolla, CA, USA |
| Abstract: | We describe the interplanetary coronal mass ejections (ICMEs) that occurred as a result of a series of solar flares and eruptions from 4 to 8 November 2004. Two ICMEs/magnetic clouds occurring from these events had opposite magnetic orientations. This was despite the fact that the major flares related to these events occurred within the same active region that maintained the same magnetic configuration. The solar events include a wide array of activities: flares, trans-equatorial coronal loop disappearance and reformation, trans-equatorial filament eruption, and coronal hole interaction. The first major ICME/magnetic cloud was predominantly related to the active region 10696 eruption. The second major ICME/magnetic cloud was found to be consistent with the magnetic orientation of an erupting trans-equatorial filament or else a rotation of 160° of a flux rope in the active region. We discuss these possibilities and emphasize the importance of understanding the magnetic evolution of the solar source region before we can begin to predict geoeffective events with any accuracy. |
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