Full-disk observations of the Sun to investigate flow structures in the chromosphere

像我们的太阳这样的冷恒星被一百万K的热日冕所包围。色球层是连接光球层和日冕层的纽带，它是日冕结构的根源，因日食时色球层的颜色变化而得名。色球层在1微米以下的长度尺度上显示出小的结构，例如比太阳表面的对流模式小的亮点，可以延伸超过100微米的日冕或冕洞，即太阳半径的相当大的一部分。因此，各种色球研究都需要将良好的空间分辨率与非常大的视场相结合的观测。Kiepenheuer-Institut的全圆盘望远镜ChroTel提供了这样的观测，本项目的目标是主要通过使用He I三重态在1083 nm处的多普勒图来研究色球层中的流动结构。通过这一点，我们将提供新的信息的动态响应的色球光球驱动，大规模的结构，如双折射和它们的干扰，以及在冕洞的快速太阳风的色球源。

Cool stars like our Sun are surrounded by a million K hot corona. The chromosphere, named after the colorful appearance during solar eclipses, is the connection from the photosphere to the corona and can be considered as the root of the coronal structures. The chromosphere shows small structures on length scales below 1 Mm, e.g. bright points which are smaller than the convection pattern at solar surface, to prominences or coronal holes which can stretch over more than 100 Mm, i.e. a sizable fraction of the solar radius. Therefore observations combining a good spatial resolution with a very large field of view are needed for various chromospheric studies. The full-disk telescope ChroTel of the Kiepenheuer-Institut provides just such observations.The goal of the present project is to investigate the flow structures in the chromosphere, predominantly through the use of Doppler maps in the He I triplet at 1083 nm. Through this we will provide new information on the dynamic response of the chromosphere to photospheric driving, on large scale structures such as prominences and their disturbances as well as on the chromospheric source of the fast solar wind in coronal holes.