TY - JOUR
T1 - Characteristics of Kinematics of a Coronal Mass Ejection during the 2010 August 1 CME-CME Interaction Event
AU - Temmer, Manuela
AU - Vršnak, Bojan
AU - Rollett, Tanja
AU - Bein, Bianca
AU - de Koning, Curt A.
AU - Lui, Ying
AU - Bosman, Eckhard
AU - Davies, Jackie A.
AU - Möstl, Christian
AU - Žic, Tomislav
AU - Veronig, Astrid M.
AU - Bothmer, Volker
AU - Harrison, Richard A.
AU - Nitta, Nariaki
AU - Bisi, M.
AU - Flor, Olga
AU - Eastwood, Jonathan P.
AU - Odstrcil, Dusan
AU - Forsyth, Robert
PY - 2012/4/1
Y1 - 2012/4/1
N2 - We study the interaction of two successive coronal mass ejections (CMEs) during the 2010 August 1 events using STEREO/SECCHI COR and heliospheric imager (HI) data. We obtain the direction of motion for both CMEs by applying several independent reconstruction methods and find that the CMEs head in similar directions. This provides evidence that a full interaction takes place between the two CMEs that can be observed in the HI1 field of view. The full de-projected kinematics of the faster CME from Sun to Earth is derived by combining remote observations with in situ measurements of the CME at 1 AU. The speed profile of the faster CME (CME2; ~1200 km s–1) shows a strong deceleration over the distance range at which it reaches the slower, preceding CME (CME1; ~700 km s–1). By applying a drag-based model we are able to reproduce the kinematical profile of CME2, suggesting that CME1 represents a magnetohydrodynamic obstacle for CME2 and that, after the interaction, the merged entity propagates as a single structure in an ambient flow of speed and density typical for quiet solar wind conditions. Observational facts show that magnetic forces may contribute to the enhanced deceleration of CME2. We speculate that the increase in magnetic tension and pressure, when CME2 bends and compresses the magnetic field lines of CME1, increases the efficiency of drag.
AB - We study the interaction of two successive coronal mass ejections (CMEs) during the 2010 August 1 events using STEREO/SECCHI COR and heliospheric imager (HI) data. We obtain the direction of motion for both CMEs by applying several independent reconstruction methods and find that the CMEs head in similar directions. This provides evidence that a full interaction takes place between the two CMEs that can be observed in the HI1 field of view. The full de-projected kinematics of the faster CME from Sun to Earth is derived by combining remote observations with in situ measurements of the CME at 1 AU. The speed profile of the faster CME (CME2; ~1200 km s–1) shows a strong deceleration over the distance range at which it reaches the slower, preceding CME (CME1; ~700 km s–1). By applying a drag-based model we are able to reproduce the kinematical profile of CME2, suggesting that CME1 represents a magnetohydrodynamic obstacle for CME2 and that, after the interaction, the merged entity propagates as a single structure in an ambient flow of speed and density typical for quiet solar wind conditions. Observational facts show that magnetic forces may contribute to the enhanced deceleration of CME2. We speculate that the increase in magnetic tension and pressure, when CME2 bends and compresses the magnetic field lines of CME1, increases the efficiency of drag.
KW - Sun: corona
KW - Sun: coronal mass ejections (CMEs)
UR - http://hdl.handle.net/2160/9242
U2 - 10.1088/0004-637X/749/1/57
DO - 10.1088/0004-637X/749/1/57
M3 - Article
SN - 0004-637X
VL - 749
SP - 57
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 1
ER -