MHD and multi-species studies of astrophysical outflows

在这个延续项目中，我们将在之前工作的基础上，追求三条研究路径。首先，我们将应用我们在CRONOS代码中实现的膨胀日冕湍流等离子体的自一致波驱动模型来改进日冕物质抛射（cme）及其与太阳风相互作用以及相互作用的模拟。其次，我们将通过初始波谱和光球磁结构之间的明确关系，将日冕基础之上的等离子体动力学模型扩展到太阳低层大气。将特别注意光球磁通管，这是一个非常有用的概念，可以用它来形成更复杂的磁结构。第三，我们将调整CRONOS代码，以便可以模拟宇宙射线驱动的磁化星系风的天体物理场景。通过这些研究活动，该项目与其他项目以及研究股的所有三个主要等离子体物理专题保持密切联系。

With this continuation project we will, based on our previous work, pursue three research paths. First, we will apply the self-consistent wave-driven model for the turbulent plasma of the expanding solar corona, that we have implemented in the CRONOS code, to an improved simulation of coronal mass ejections (CMEs) and their interaction with the solar wind as well as which each other. Second, we will extend the modelling of the plasma dynamics above the coronal base by coupling it, via an explicit relation between the initial wave spectrum and photospheric magnetic structures, to the lower solar atmosphere. Special attention will be given to photospheric magnetic flux tubes that constitute a very useful concept with which more complex magnetic structures can be formed. And, third, we will adapt the CRONOS code such that the astrophysical scenario of a cosmic ray-driven magnetized galactic wind can be simulated. With these research activities the project remains tightly connected to other projects as well as to all three main plasma physical topics of the Research Unit.