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

凉爽的恒星被炽热的日冕包围着，日冕被加热到几百万开尔文。被广泛认为与恒星磁场有关的加热过程不仅导致外部大气中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，诱发流动和波动。为了研究这些过程，太阳是非常重要的，因为我们可以在空间上解析日冕中的单个结构。在这个方案中，我们将利用新的3D MHD数值模拟结合前所未有的质量的新观测来研究日冕对加热过程的动态响应。新的Hinode空间观测站上的极端紫外线成像光谱仪提供了高时间步调的发射线轮廓的大空间地图，这将使首次能够研究活动区域大部分的多普勒频移波动。这将为最近几年才出现的日冕3D MHD模型提供新的测试。这些3D模型和新的观测也将为日冕地震学的研究打开可能性，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.