The role of streamers in the deflection of coronal mass ejections

被引：0

作者：

Zuccarello, F. P. ^{[1
,2
,3
]}

Bemporad, A. ^{[4
]}

Jacobs, C. ^{[1
]}

Mierla, M. ^{[5
,6
]}

Poedts, S. ^{[1
]}

Zuccarello, F. ^{[3
]}

机构：

[1] Katholieke Univ Leuven, Ctr Plasma Astrophys, Leuven, Belgium

[2] Osserv Astrofis Catania, INAF, I-95123 Catania, Italy

[3] Sez Astrofis, Dipartimento Fis & Astron, I-95123 Catania, Italy

[4] Osserv Astron Torino, Ist Nazl Astrofis INAF, I-10025 Pino Torinese, Italy

[5] Romanian Acad, Inst Geodynam, Bucharest, Romania

[6] Royal Observ Belgium, Brussels, Belgium

来源：

COMPARATIVE MAGNETIC MINIMA: CHARACTERIZING QUIET TIMES IN THE SUN AND STARS | 2012年 / 286期

关键词：

Sun: coronal mass ejections (CMEs); methods: numerical; Sun: corona; Sun: magnetic fields;

D O I：

10.1017/S1743921312004747

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

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 (TICS) 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.

引用

页码：134 / +

页数：2

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