Heizung des chromosphärischen Netzwerks

观测结果表明，磁网络中存在长周期振荡。为了解释它们和推断磁管大气的性质，必须弄清楚波的性质和周期的起源以及加热。我们的目标是确定发生在色球磁场网络中的物理过程，这些过程对色球的动力学和加热有贡献。具体地说，我们想要研究通过足点运动在通量管中激发的横向(扭结)MHD波。当这些波向上传播时，它们通过非线性效应(模式耦合)部分转换为纵波。这种模式脱钩在受到冲击时尤其有效。虽然扭结波可以通过过渡区传播并最终加热日冕，但转化为纵波的部分能量通过激波加热在色球中消散。我们的目标是将辐射处理纳入我们以前的代码，对波的传播进行建模，并检查这些波的观测特征。

Observations show the existence of long-period oscillations in the magnetic net-work. In order to interpret them and deduce the properties of the magnetic tube atmosphere, the nature of the waves and the origin of the periods as well as the heating must be clarified. We aim to identify the physical processes which occur in the magnetic network of the chromosphere and which contribute to its dynamics and heating. Specifically, we want to investigate transverse (kink) MHD waves which are excited in flux tubes through footpoint motions. When theses waves travel upwards, they get partially converted to longitudinal waves through nonlinear effects (mode-coupling). This modecoupling is particularly efficient near shocks. Whereas kink waves can propagate through the transition region and eventually heat the corona, the fraction of energy converted to longitudinal waves dissipates in the chromosphere by shock heating. Our aim is to incorporate the treatment of radiation into our previous codes, model the wave propagation and examine the observational signature of these waves.