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The role of streamers in the deflection of coronal mass ejections

Published online by Cambridge University Press:  05 July 2012

F. P. Zuccarello ,
A. Bemporad ,
C. Jacobs ,
M. Mierla ,
S. Poedts  and
F. Zuccarello
F. P. Zuccarello
Affiliation:
Centre for Plasma Astrophysics, K.U. Leuven, Belgium. INAF - Osservatorio Astrofisico di Catania, via S. Sofia 78, 95123 Catania, Italy. Dipartimento di Fisica e Astronomia, Sezione Astrofisica, Via S. Sofia 78, 95123 Catania, Italy.
A. Bemporad
Affiliation:
Istituto Nazionale di Astrofisica (INAF), Osservatorio Astronomico di Torino, Strada Osservatorio 20, 10025 Pino Torinese, Torino, Italy.
C. Jacobs
Affiliation:
Centre for Plasma Astrophysics, K.U. Leuven, Belgium.
M. Mierla
Affiliation:
Institute of Geodynamics of the Romanian Academy, Bucharest, Romania. Royal Observatory of Belgium, Brussels, Belgium.
S. Poedts
Affiliation:
Centre for Plasma Astrophysics, K.U. Leuven, Belgium.
F. Zuccarello
Affiliation:
Dipartimento di Fisica e Astronomia, Sezione Astrofisica, Via S. Sofia 78, 95123 Catania, Italy.
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Abstract

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On 2009 September 21, a filament eruption and the associated Coronal Mass Ejection (CME) was observed by the STEREO spacecraft. The CME originated from the southern hemisphere and showed a deflection of about 15° towards the heliospheric current sheet (HCS) during its propagation in the COR1 field-of-view (FOV). The aim of this paper is to provide a physical explanation for the strong deflection of the CME. We first use the STEREO observations in order to reconstruct the three dimensional (3D) trajectory of the CME. Starting from a magnetic configuration that closely resembles the potential field extrapolation for that date, we performed numerical magneto-hydrodynamics (MHD) simulations. By applying localized shearing motions, a CME is initiated in the simulation, showing a similar non-radial evolution, structure, and velocity as the observed event. The CME gets deflected towards the current sheet of the larger northern helmet streamer, due to an imbalance in the magnetic pressure and tension forces and finally it gets into the streamer and propagates along the heliospheric current sheet.

Keywords

Sun: coronal mass ejections (CMEs)methods: numericalSun: coronaSun: magnetic fields
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 7 , Symposium S286: Comparative Magnetic Minima: Characterizing quiet times in the Sun and Stars , October 2011 , pp. 134 - 138
Copyright
Copyright © International Astronomical Union 2012

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