行星际热通道初尝滋味
First Taste of Hot Channel in Interplanetary Space
摘要：
热通道（HC）是由\textit{Solar Dynamics Observatory}上的大气成像组件（AIA）首次揭示的内日冕高温（$\sim$ 10 MK）结构。HC的爆发常与耀斑和日冕物质抛射有关。以往的研究表明，HC是一个很好的替代磁通量绳（MFR）的内日冕，除了另一个众所周知的MFR候选者，有一个正常的日冕温度（$\sim$ 1-2 MK）的磁共振腔结构。本文报道了HC爆发引起的行星际日冕物质抛射中的高温结构（HTS，$\sim$ 1.5 MK）。根据对双向电子、高温高密度、强磁场以及激波、鞘层和等离子体堆积区的观测，我们认为高温超导体是HC的行星际对应体。高温超导体的尺度约为14 R $_\odot$，即使在1 AU处也保持着比背景太阳风高得多的温度。它与典型的磁云（MC）有很大的不同，后者通常具有更低的温度。我们的研究表明，在HC前面存在一个共转相互作用区，形成一个磁容器，抑制HC膨胀和冷却到低温。
英文摘要：
Hot channel (HC) is a high temperature ($\sim$10 MK) structure in the inner corona revealed first by Atmospheric Imaging Assembly (AIA) on board \textit{Solar Dynamics Observatory}. Eruption of HC is often associated with flare and coronal mass ejection. Previous studies suggest that HC is a good proxy of magnetic flux rope (MFR) in the inner corona, in addition to another well-known MFR candidate, the prominence-cavity structure that is with a normal coronal temperature ($\sim$1-2 MK). In this paper, we report a high temperature structure (HTS, $\sim$1.5 MK) contained in an interplanetary coronal mass ejection induced by an HC eruption. According to the observations of bidirectional electrons, high temperature and density, strong magnetic field, and its association with the shock, sheath, and plasma pile-up region, we suggest that the HTS is the interplanetary counterpart of the HC. The scale of the measured HTS is around 14 R$_\odot$, and it maintained a much higher temperature than the background solar wind even at 1 AU. It is significantly different from the typical magnetic clouds (MCs), which usually have a much lower temperature. Our study suggests that the existence of a corotating interaction region ahead of the HC formed a magnetic container to inhibit the HC expansion and cooling down to a low temperature.
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