标题： 爆发后相的耀斑相关日冕物质抛射的统计研究 显示英文标题

标题： A statistical study of the post-impulsive-phase acceleration of flare-associated coronal mass ejections

摘要： 现在普遍认为，日冕物质抛射（CME）在内日冕中的脉冲加速与相关太阳耀斑的主要能量释放在时间上密切相关。 在本文中，我们详细研究了CME在外日冕中的后脉冲阶段加速，这是CME主要脉冲加速之后的演化阶段；这一阶段被认为对应于相关耀斑的衰减阶段。 这项观测研究基于1996年至2006年间与M级和X级GOES软X射线耀斑相关的247个CME的统计样本。 我们发现，从许多事件的例子来看，与长衰减时间（或所谓的长时间耀斑）相关的CME往往具有正的后脉冲阶段加速，尽管其中一些CME在脉冲加速结束时已经获得了较高的速度，但并未表现出由于背景太阳风的空气动力学拖曳而预期的减速。 另一方面，与短衰减时间耀斑相关的CME往往表现出显著的减速。 在所有事件的散点图中，CME的后脉冲阶段加速与耀斑衰减时间之间存在弱相关性。 偏离一般趋势的CME大多是与短衰减时间耀斑相关的慢速或弱CME；这种偏离是由于这些事件的相对较强的太阳风拖曳力造成的。 我们的结果对CME动力学和CME-耀斑关系的含义进行了讨论。 显示英文摘要

摘要： It is now generally accepted that the impulsive acceleration of a coronal mass ejection (CME) in the inner corona is closely correlated in time with the main energy release of the associated solar flare. In this paper, we examine in detail the post-impulsive-phase acceleration of a CME in the outer corona, which is the phase of evolution immediately following the main impulsive acceleration of the CME; this phase is believed to correspond to the decay phase of the associated flare. This observational study is based on a statistical sample of 247 CMEs that are associated with M- and X-class GOES soft X-ray flares from 1996 to 2006. We find that, from many examples of events, the CMEs associated with flares with long-decay time (or so-called long-duration flares) tend to have positive post-impulsive-phase acceleration, even though some of them have already obtained a high speed at the end of the impulsive acceleration but do not show a deceleration expected from the aerodynamic dragging of the background solar wind. On the other hand, the CMEs associated with flares of short-decay time tend to have significant deceleration. In the scattering plot of all events, there is a weak correlation between CME post-impulsive-phase acceleration and flare decay time. The CMEs deviated from the general trend are mostly slow or weak ones associated with flares of short-decay time; the deviation is caused by the relatively stronger solar wind dragging force for these events. The implications of our results on CME dynamics and CME-flare relations are discussed.