The state of the space environment plays a significant role for forecasting of geomagnetic storms produced by disturbances of the solar wind (SW). Coronal mass ejections (CMEs) passing through the heliosphere often have a prolonged (up to several days) trail with declining speed, which affects propagation of the subsequent SW streams. We studied the CME and the post-eruption plasma flows behind the CME rear in the event on 2010 August 18 observed in quadrature by several space-based instruments. Observations of the eruption in the corona with EUV telescopes and coronagraphs revealed several discrete outflows followed by a continuous structureless post-eruption stream. The interplanetary coronal mass ejection (ICME), associated with this CME, was registered by PLAsma and SupraThermal Ion Composition (PLASTIC) instrument aboard the Solar TErrestrial RElations Observatory (STEREO-A) between August 20, 16:14 UT and August 21, 13:14 UT, after which the SW disturbance was present over 3 days. Kinematic consideration with the use of the gravitational and Drag-Based models has shown that the discrete plasma flows can be associated with the ICME, whereas the post-eruption outflow was arrived in the declining part of the SW transient. We simulated the Fe-ion charge distributions of the ICME and post-CME parts of SW using the plasma temperature and density in the ejection region derived from the Differential Emission Measure analysis. The results demonstrate that in the studied event the post-ICME trailing region was associated with the post-eruption flow from the corona, rather then with the ambient SW entrained by the CME.
The initiation of a solar streamer blowout coronal mass ejection arising from the streamer flank
流光爆发（SBO）日冕物质抛射（CME）是一类特殊的CME，其特征是上覆流光逐渐膨胀，缓慢的CME包含一个通量绳结构。从拖缆侧面产生的SBO CME属于SBO CME的一个特殊类别，包括在较高的拖缆拱廊下的三个较低的拱廊。然而，这类特殊的SBO日冕物质抛射的启动机制仍然难以捉摸，由于观测的局限性。在这里，我们报告的关键观测SBO日冕物质抛射与喷发的极冠灯丝，起源于流光侧翼。暗条随着扭动的运动，慢慢地向太阳赤道上升，在爆发前，它经历了一个突然的加速。有趣的是，在上升过程中，暗条场经历了逐渐的外部重连，这是证明了从一个光滑的凹的包络线结构的倾角形状的底部变化，缓慢的流入（$\sim$ 1.8 km s $^{-1}$）从暗条场和下面的日冕环，和持久的增亮之间的界面周围的暗条场和下面的日冕环。在暗条源处新形成的低圈和拉伸尾场中的Y形结构表明暗条爆发的内部重联。外部和内部重联的清晰特征揭示了SBO CME的启动机制。
Arrival time calculation for interplanetary coronal mass ejections with circular fronts and application to STEREO observations of the 2009 February 13 eruption
Origin and Ion Charge State Evolution of Solar Wind Transients during 4 -- 7 August 2011
我们目前的复杂事件的研究，包括几个太阳风瞬变探测器（ACE）在2011年8月4 - 7日，造成的磁暴Dst $=-$ 110 nT。2011年8月2日至4日，活动区（AR）11261发生了三次耀斑和日冕物质抛射（CME）。为了研究这些瞬变的太阳起源和形成，我们使用太阳动力学天文台/大气成像组件（SDO/AIA）EUV图像和差分发射测量（DEM）诊断研究了扩展日冕结构的运动学和热力学性质。日震和磁成像仪（HMI）的磁场图被用作三维磁流体动力学（MHD）模型的输入数据来描述磁绳喷射。我们的特点的早期阶段的磁通绳喷射在日冕，通常的三个组成部分CME结构形成。磁绳以约200 km s $^{-1}$的速度弹射到0.25 R $_{\odot}$的高度。模拟的日冕物质抛射锋的运动学与日地关系天文台（STEREO）的EUV测量结果吻合得很好。利用等离子体诊断和MHD模型的结果，我们计算了2011年8月2日CME的碳和氧的离子电荷比以及铁离子的平均电荷状态，考虑到加热，冷却，膨胀，电离和复合的过程中移动的等离子体在日冕冻结区域。我们估计了一个可能的加热速率的CME等离子体在低日冕通过匹配的CME的离子组成参数与现场测量的太阳风瞬变。我们还考虑了MHD模拟结果与观测结果之间的相似性和差异。
