邀请团队:　抚仙湖太阳观测站 & 太阳活动和CME理论研究团组

摘要:　　　The Solar atmosphere extends from the photosphere to the expanding into the Solar Wind Corona. Huge amounts of energy are released in the Solar atmosphere. They heat the coronal plasma to millions of degrees Kelvin and blow the heated plasma into the solar wind. They are also released by huge material outbursts -coronal mass ejections. But what is driving the Solar atmosphere? Observations tell us that the complex and dynamically evolving photospheric magnetic field and plasma motion is the power behind. But even the best available remote observations of the Sun do not resolve the typical scales of the underlying physical processes. Hence appropriate mathematical models  are needed. Their observable consequences have to be derived using numerically solved plasma simulation approaches. Both RHMD and plasma simulation approaches and their results are presented dealing with the key questions of coronal plasma heating, eruptions and  and solar wind acceleration.