Characteristics of Kinematics of a Coronal Mass Ejection During the 2010 August 1 Cme–cme Interaction Event

Abstract

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.

The 2010 August 1 Type Ii Burst: A Cme-Cme Interaction and Its Radio and White-Light Manifestations

“…between STEREO-B and Wind ), which is about the same angular separation derived by the direction-finding technique. The obtained propagation direction is in agreement with finding of Temmer et al (2011) and Liu et al (2011).…”

“…The period 2010 July 31 to August 2 was characterized by increased solar activity, exhibiting small flares, filament eruptions and coronal mass ejections (Schrijver and Title 2011;Temmer et al 2011;Liu et al 2011). Of particular interest here is the time during which two CMEs (one slow(CME1), erupted at 02:00UT and one fast(CME2), erupted at 07:00UT) interacted with each other, resulting in a low frequency type II radio burst observed on 2010 August 1 at about 09:00 UT).…”

Propagation and Interaction Properties of Successive Coronal Mass Ejections in Relation to a Complex Type II Radio Burst

“…Interactions with other CMEs can change both the speed and propagation direction of the interacting events (e.g., Gopalswamy et al 2001b;Farrugia & Berdichevsky 2004;Liu et al 2012Liu et al , 2014bLugaz et al 2012;Temmer et al 2012;Shen et al 2012;Mishra et al 2015). Almost all studies of CME-CME interactions have focused on the interaction between two events.…”

A Numerical Study of Long-Range Magnetic Impacts During Coronal Mass Ejections

“…Such interactions may significantly modify the structure of the CME-driven shock wave and the properties of the interplanetary CME (ICME), and therefore affect the potential of space weather effects (e.g., Liu et al 2012Liu et al , 2014aMöstl et al 2012). Interactions between CMEs from the same AR have often been discussed (e.g., Lugaz et al 2005bLugaz et al , 2007Lugaz et al , 2013Xiong et al 2006), but CMEs can be spatially extended and those from distant regions may also interact, adding complexity to solar wind data (e.g., Temmer et al 2012). It is also possible that sympathetic events may play a role in SEP events observed at widely separate locations (e.g., Richardson et al 2014;Gómez-Herrero et al 2015).…”