Abstract
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.
Highlights
Coronal mass ejections (CMEs) are transient events where coronal plasma is ejected by the Sun at velocities ranging from less than 200 km s−1 to more than 2000 km s−1 (e.g. Yurchyshyn et al, 2005)
15 May 2007 Coronal Mass ejections (CMEs) as found by Temmer et al (2009) differ by 20◦ from that obtained by Mierla et al (2008) who used the 3-D height-time technique (3D-HT) method to determine the kinematic properties for a localized blob of plasma which could be identified within the CME cloud (Table 2)
By applying different reconstruction techniques the longitude of this event was estimated to be −88◦ (LE) using the inverse reconstruction combined with Forward modeling (FM) (Antunes et al, 2009); −86◦ from triangulation of a feature on the leading edges (LE) (Temmer et al, 2009); −80◦ from the FM of Thernisien et al (2009); −100◦ from mass constraints (Colaninno and Vourlidas, 2009); −94◦ from geometric localization technique; −94◦ from tiepointing plus triangulation of the LE (Liewer et al, 2009b)
Summary
Coronal mass ejections (CMEs) are transient events where coronal plasma is ejected by the Sun at velocities ranging from less than 200 km s−1 to more than 2000 km s−1 (e.g. Yurchyshyn et al, 2005). Yurchyshyn et al, 2005) They play an important role for space weather, as they can induce severe magnetic storms when they interact with the Earth’s magnetosphere. M. Mierla et al.: CME reconstruction an apparent width of around 360◦ in a coronagraph field of view) directed towards the Earth have been known to produce strong geomagnetic storms (Gosling et al, 1990; Srivastava and Venkatakrishnan, 2002, 2004). In addition to the speed of the CME, the magnetic field orientation of the interplanetary CME (ICME) plays an important role. The stereoscopic images obtained by the Sun Earth Connection Coronal and Heliospheric Investigation (SECCHI) instrument suite (Howard et al, 2008) aboard STEREO allow us to make 3-D estimations of the structure and kinematic parameters of CMEs
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