Heizung des chromosphärischen Netzwerks

观测表明，在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，必须澄清波的性质和周期的起源以及加热。我们的目标是确定的物理过程中发生的色球层的磁网络，并有助于其动力学和加热。具体来说，我们要调查的横向（扭结）磁流体动力学波，通过足点运动在磁通管中激发。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。这种模态解耦在冲击附近特别有效。而扭折波可以传播通过过渡区，并最终加热日冕，部分能量转换为纵波耗散在色球层的冲击加热。我们的目标是将辐射的处理纳入我们以前的代码，波的传播模型，并检查这些波的观测签名。

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.