Dynamic response of the solar corona to heating driven by photospheric motions

冷恒星被加热到几百万开尔文的热日冕所包围。被广泛认为与恒星磁场有关的加热过程，不仅导致外层大气的温度远远超过恒星表面，而且还导致等离子体的高度动态响应，诱发流和波。要研究这些过程，太阳是一个关键的兴趣点，因为在这里我们可以在空间上解析日冕中的单个结构。在这个提议中，我们将利用新的3D MHD数值模拟，结合前所未有的新观测质量来研究日冕对加热过程的动态响应。新日野空间天文台上的极紫外成像光谱仪提供了具有高时间节奏的发射线剖面的大空间地图，这将首次允许研究例如活动区域大部分的多普勒频移波动。这将为日冕的3D MHD模型提供一种新的测试方法，这种模型是最近几年才出现的。这些3D模型和新的观测结果将为日冕地震学的研究开辟新的可能性，并有助于推断在日冕中发现的各种结构的物理参数。

Cool stars are surrounded by hot coronae which are heated to some million degrees Kelvin. The heating processes, widely proposed to be related to the stellar magnetic field, lead not only to temperatures in the outer atmosphere well in excess of the stellar surface, but result also in a highly dynamic response of the plasma, inducing flows and waves. To study these processes the Sun is of pivotal interest because here we can spatially resolve individual structures in the corona.In this proposal we will utilize new 3D MHD numerical simulations in combination with new observations of unprecedented quality to investigate the dynamic response of the corona to the heating process. The Extreme ultraviolet Imaging Spectrometer on the new Hinode space observatory provides large spatial maps of emission line profiles with high time cadence, which will allow for the first time to study e.g. the Doppler shift fluctuations of a large part of an active region. This will provide a new test for the 3D MHD models of the corona which became available only in recent years. These 3D models together with the new observations will also open possibilities for investigations of coronal seismology, and help to infer the physical parameters in various structures found in the solar corona.