The Solar Interface Region

我们的目的是研究太阳光球和日冕之间的界面区域。这个界面区由色球层和过渡层组成，将太阳光球层（温度约6000 K）和日冕层（温度数百万K）分开。等离子体加热和从光球到日冕的物质供应发生在这个界面区域，这一点目前还不清楚，也很难研究。小型探测任务IRIS（界面区域成像光谱仪）于2007年发射。2013年6月)专门观察这个区域。作为这次成像任务的补充，我们将从日出气球运载任务（12月12日发射）获得光球磁场矢量的高分辨率测量。2013年6月)。对这两个任务（以及来自SDO和Hinode的额外数据集）的数据集的分析，以及我们小组开发的先进磁场外推和等离子体建模技术，为我们提供了调查太阳大气质量和能量供应的独特机会。

Our aim is to study the interface region between the solar photosphere and solar corona. This interface region, which consists of the chromosphere and transition region, separates the solar photosphere (temperature about 6000 K) and the corona (temperature millions K). Plasma heating and mass supply from the photosphere to the corona take place in this interface region, which is not well understand and difficult to investigate. The small explorer mission IRIS (Interface Region Imaging spectrograph, launched 27. june 2013) is dedicated to observe this region. Complimentary to this imaging mission we will get high resolution measurements of the photospheric magnetic field vector from the balloon borne mission SUNRISE (launched 12. June 2013). An analysis of data sets from these two missions (and additional from SDO and Hinode) together with advanced magnetic field extrapolation and plasma modelling techniques developed in our group give us the unique opportunity to investigate the mass and energy supply of the solar atmosphere.