Strong coronal channelling and interplanetary evolution of a solar storm up to Earth and Mars

Christian Möstl (), Tanja Rollett, Rudy A. Frahm, Ying D. Liu, David M. Long, Robin C. Colaninno, Martin A. Reiss, Manuela Temmer, Charles J. Farrugia, Arik Posner, Mateja Dumbović, Miho Janvier, Pascal Démoulin, Peter Boakes, Andy Devos, Emil Kraaikamp, Mona L. Mays and Bojan Vršnak
Additional contact information
Christian Möstl: Space Research Institute, Austrian Academy of Sciences
Tanja Rollett: Space Research Institute, Austrian Academy of Sciences
Rudy A. Frahm: Southwest Research Institute
Ying D. Liu: State Key Laboratory of Space Weather, National Space Science Center, Chinese Academy of Sciences
David M. Long: Mullard Space Science Laboratory, University College London
Robin C. Colaninno: Naval Research Laboratory
Martin A. Reiss: IGAM-Kanzelhöhe Observatory, Institute of Physics, University of Graz
Manuela Temmer: IGAM-Kanzelhöhe Observatory, Institute of Physics, University of Graz
Charles J. Farrugia: Space Science Center, University of New Hampshire
Arik Posner: NASA Headquarters
Mateja Dumbović: Hvar Observatory, Faculty of Geodesy, University of Zagreb
Miho Janvier: University of Dundee
Pascal Démoulin: Observatoire de Paris, LESIA, UMR 8109 (CNRS), F-92195 Meudon Principal, France
Peter Boakes: IGAM-Kanzelhöhe Observatory, Institute of Physics, University of Graz
Andy Devos: Solar-Terrestrial Center of Excellence - SIDC, Royal Observatory of Belgium
Emil Kraaikamp: Solar-Terrestrial Center of Excellence - SIDC, Royal Observatory of Belgium
Mona L. Mays: Catholic University of America
Bojan Vršnak: Hvar Observatory, Faculty of Geodesy, University of Zagreb

Nature Communications, 2015, vol. 6, issue 1, 1-10

Abstract: Abstract The severe geomagnetic effects of solar storms or coronal mass ejections (CMEs) are to a large degree determined by their propagation direction with respect to Earth. There is a lack of understanding of the processes that determine their non-radial propagation. Here we present a synthesis of data from seven different space missions of a fast CME, which originated in an active region near the disk centre and, hence, a significant geomagnetic impact was forecasted. However, the CME is demonstrated to be channelled during eruption into a direction +37±10° (longitude) away from its source region, leading only to minimal geomagnetic effects. In situ observations near Earth and Mars confirm the channelled CME motion, and are consistent with an ellipse shape of the CME-driven shock provided by the new Ellipse Evolution model, presented here. The results enhance our understanding of CME propagation and shape, which can help to improve space weather forecasts.

Date: 2015
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DOI: 10.1038/ncomms8135

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