论文标题
星际冠状质量弹出在0.3至2.2 Au之间的多飞机运动物观察结果
Multi-Spacecraft Observations of the Evolution of Interplanetary Coronal Mass Ejections Between 0.3 and 2.2 AU: Conjunctions with the Juno Spacecraft
论文作者
论文摘要
我们提出了朱诺航天器观察到的35个星际冠状质量弹出(ICMES)的目录,并在其前往木星的巡航阶段至少有一个其他航天器。我们确定了Messenger,Venus Express,Wind和Stereo所观察到的磁性特征所观察到的事件,这些特征可以与Juno观察到的事件明确匹配。进行了0.3至2.2 AU之间的ICME性质的多飞机运研究:我们首先通过跟踪磁场强度的变化,随着单个ICME事件的地震距离的增加,通过跟踪磁场强度的变化来研究全局膨胀,发现与统计趋势相比,单个事件的磁场关系显着差异。随着1 AU的等离子数据的可用性,可以将1 AU处的局部扩展与1 AU和Juno之间的全球膨胀率进行比较。尽管遵循了预期的趋势,但本地和全球的扩张率只是较弱的相关性。最后,对于那些具有清晰可识别的磁通绳的事件,我们研究了通量绳轴传播时的方向。我们发现,有64%的事件显示出随着地中心度距离的增加而显示的倾向下降,而40%的事件在向Juno传播时会发生显着变化。这项研究中生产的多飞机运动物目录提供了内部地球内ICME观测值与1 au之外的有价值的联系,从而提高了我们对ICME进化的理解。
We present a catalogue of 35 interplanetary coronal mass ejections (ICMEs) observed by the Juno spacecraft and at least one other spacecraft during its cruise phase to Jupiter. We identify events observed by MESSENGER, Venus Express, Wind, and STEREO with magnetic features that can be matched unambiguously with those observed by Juno. A multi-spacecraft study of ICME properties between 0.3 and 2.2 AU is conducted: we firstly investigate the global expansion by tracking the variation in magnetic field strength with increasing heliocentric distance of individual ICME events, finding significant variability in magnetic field relationships for individual events in comparison with statistical trends. With the availability of plasma data at 1 AU, the local expansion at 1 AU can be compared with global expansion rates between 1 AU and Juno. Despite following expected trends, the local and global expansion rates are only weakly correlated. Finally, for those events with clearly identifiable magnetic flux ropes, we investigate the orientation of the flux rope axis as they propagate; we find that 64% of events displayed a decrease in inclination with increasing heliocentric distance, and 40% of events undergo a significant change in orientation as they propagate towards Juno. The multi-spacecraft catalogue produced in this study provides a valuable link between ICME observations in the inner heliosphere and beyond 1 AU, thereby improving our understanding of ICME evolution.