CHARACTERISTICS OF KINEMATICS OF A CORONAL MASS EJECTION DURING THE 2010 AUGUST 1 CME–CME INTERACTION EVENT
CHARACTERISTICS OF KINEMATICS OF A CORONAL MASS EJECTION DURING THE 2010 AUGUST 1 CME–CME INTERACTION EVENT
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DOI：
10.1088/0004-637x/749/1/57
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发表时间：
2012-02
期刊：
影响因子：
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通讯作者：
M. Temmer;B. Vršnak;T. Rollett;B. Bein;C. A. de Koning;Y. Liu;E. Bosman;J. Davies;C. Möstl
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文献类型：
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作者：
M. Temmer;B. Vršnak;T. Rollett;B. Bein;C. A. de Koning;Y. Liu;E. Bosman;J. Davies;C. Möstl
利用STEREO/SECCHI COR和日球层成像仪(HI)资料研究了2010年8月1日事件期间两次连续的日冕物质抛射(CME)的相互作用。我们通过应用几种独立的重建方法得到了两个日冕物质抛射的运动方向，发现日冕物质抛射朝着相似的方向前进。这提供了证据，证明在HI1视场中可以观察到的两个日冕物质抛射之间发生了充分的相互作用。通过在1AU的CME的遥测和现场测量相结合，得到了从太阳到地球的更快的CME的完整反投影运动学。较快的CME(CME2；∼1200 KM S−1)的速度剖面显示出在到达较慢的、在前的CME(CME1；∼700 KM S−1)的距离范围内有强烈的减速。通过应用基于阻力的模型，我们能够再现CME2的运动学轮廓，这表明CME1代表着CME2的磁流体动力学障碍，并且在相互作用之后，合并的实体作为单一结构在安静的太阳风条件下典型的速度和密度的环境流中传播。观测事实表明，磁力可能对CME2的减速增强有贡献。我们推测，当CME2弯曲和压缩CME1的磁场线时，磁张力和磁压的增加增加了阻力的效率。
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.