Dome C的太阳物理学和太阳-恒星联系
Solar Physics and the Solar-Stellar Connection at Dome C
摘要：
太阳磁场在许多时间尺度上演化，例如，太阳22年磁周期中磁通量的产生、迁移和消散。活跃区域在数周内发展和衰退。活跃区域的磁剪切的积累可以在不到一天的时间内发生。在最短的时间尺度上，磁场拓扑结构可以在几分钟内迅速变化，这是耀斑、暗条爆发和日冕物质抛射等爆发事件的结果。Dome C独特的日间视觉特征，即，在几乎整个南极洲的夏天，连续的非常好的时期，使我们能够解决许多与太阳磁场演变有关的顶级科学案例。我们介绍了先进的太阳光度成像仪和辐射实验，并提出了在圆顶C天气太阳观测的科学案例。此外，在拟议的国际康科迪亚探索者望远镜的背景下讨论了有关太阳-恒星连接的常见科学案例。
英文摘要：
Solar magnetic fields evolve on many time-scales, e.g., the generation, migration, and dissipation of magnetic flux during the 22-year magnetic cycle of the Sun. Active regions develop and decay over periods of weeks. The build-up of magnetic shear in active regions can occur within less than a day. At the shortest time-scales, the magnetic field topology can change rapidly within a few minutes as the result of eruptive events such as flares, filament eruptions, and coronal mass ejections. The unique daytime seeing characteristics at Dome C, i.e., continuous periods of very good to excellent seeing during almost the entire Antarctic summer, allow us to address many of the top science cases related to the evolution of solar magnetic fields. We introduce the Advanced Solar Photometric Imager and Radiation Experiment and present the science cases for synoptic solar observations at Dome C. Furthermore, common science cases concerning the solar-stellar connection are discussed in the context of the proposed International Concordia Explorer Telescope.
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