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On the 3-D reconstruction of Coronal Mass Ejections using coronagraph data
1Institute of Geodynamics of the Romanian Academy, Bucharest, Romania
2Solar-Terrestrial Center of Excellence – SIDC, Royal Observatory of Belgium, Brussels, Belgium
3Max-Planck-Institut für Sonnensystemforschung, Katlenburg-Lindau, Germany
4Naval Research Laboratory, Washington, D.C., USA
5Laboratoire d'Astrophysique de Marseille, Marseille, France
6Signal Processing Institute, EPFL, Lausanne, Switzerland
7Astrophysics Research Group, School of Physics, Trinity College Dublin, Dublin 2, Ireland
8George Mason University, Fairfax, USA
9NASA – Goddard Space Flight Center, MD, USA
10CIRES-SWPC, University of Colorado, Boulder, CO, USA
11Air Force Research Laboratory, National Solar Observatory, Sunspot, NM 88349, USA
12Department of Space Studies, Southwest Research Institute, Boulder, CO 80302, USA
13Catholic University of America, Washington D.C., USA
14Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA
15Udaipur Solar Observatory, Physical Research Laboratory, Udaipur, India
16Interferometrics, Inc., Herndon, USA
17Kanzelhöhe Observatory/IGAM, Institute of Physics, University of Graz, Graz, Austria
18Universities of Space Research Association, Columbia, MD, USA
19Skobeltsyn Institute of Nuclear Physics, Moscow State University, Moscow, Russia
Abstract. Coronal Mass ejections (CMEs) are enormous eruptions of magnetized plasma expelled from the Sun into the interplanetary space, over the course of hours to days. They can create major disturbances in the interplanetary medium and trigger severe magnetic storms when they collide with the Earth's magnetosphere. It is important to know their real speed, propagation direction and 3-D configuration in order to accurately predict their arrival time at the Earth. Using data from the SECCHI coronagraphs onboard the STEREO mission, which was launched in October 2006, we can infer the propagation direction and the 3-D structure of such events. In this review, we first describe different techniques that were used to model the 3-D configuration of CMEs in the coronagraph field of view (up to 15 R⊙). Then, we apply these techniques to different CMEs observed by various coronagraphs. A comparison of results obtained from the application of different reconstruction algorithms is presented and discussed.
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Citation: Mierla, M., Inhester, B., Antunes, A., Boursier, Y., Byrne, J. P., Colaninno, R., Davila, J., de Koning, C. A., Gallagher, P. T., Gissot, S., Howard, R. A., Howard, T. A., Kramar, M., Lamy, P., Liewer, P. C., Maloney, S., Marqué, C., McAteer, R. T. J., Moran, T., Rodriguez, L., Srivastava, N., Cyr, O. C. St., Stenborg, G., Temmer, M., Thernisien, A., Vourlidas, A., West, M. J., Wood, B. E., and Zhukov, A. N.: On the 3-D reconstruction of Coronal Mass Ejections using coronagraph data, Ann. Geophys., 28, 203-215, 2010. Bibtex EndNote Reference Manager
