Travel grant for observing with SST, La Palma- Dynamic events in the chromosphere of coronal holes: RBE's and Swirls

现代等离子体天体物理学最令人感兴趣的问题之一是磁化太阳大气中温度的快速上升。现在很清楚，光球下颗粒运动的巨大机械能的一部分被引导到太阳大气中（例如，参见我们的Nature论文，Wedemeyer-Bhom等人，2012年关于这种能量传输如何在太阳龙卷风中占据空间），在那里它被耗散，导致环境等离子体的巨大加热到数百万K。这种能量传输的细节尚未完全了解。由于太阳大气层有各种各样的特征，从针状体、纤维、孔隙、太阳黑子、日冕环、日冕洞等，它们中的每一个的能量可能都是不同的。基本问题是：磁流体动力学（MHD）波是否起着关键作用，或者它是磁应力的积累和快速释放？磁场在塑造太阳大气层方面非常重要，因为：它（i）不仅概述了作为能量传播通道的MHD波导，而且（ii）确定了连接拓扑结构;（iii）存储了与等离子体加热相关的能量。这种能量通道的一个可行方案是，相干和随机（子）光球运动激发MHD波，这些波穿过磁化的太阳大气层，同时携带和阻尼与太阳大气层磁结构相关的必要非热能。是否存在MHD波已不再是一个问题。相反，现在的重点是如何对等离子体加热所需的必要的波通量存在于磁化等离子体结构和什么类型的MHD波是能量传输过程中的主要参与者（ES）。在这里，我们建议（i）观测和全面跟踪MHD波从光球到色球在局部高动态磁波导的重点是这些波的磁签名：（ii）下一步，我们将确定实际的身份和性质的检测MHD波（慢，快，阿尔芬;扭结，香肠;表面，身体等）; (iii)我们将研究这些波是如何出现在一系列结构中的（例如a）边缘的针状物; B）冕洞中的漩涡）（iv）我们将建立这些结构和其中存在的波的统计数据

One of the most intriguing problems of modern plasma-astrophysics is the rapid rise of temperature in the magnetised solar atmosphere. It is now clear that part of the vast mechanical energy of sub-photospheric granular motions is channelled into the solar atmosphere (see e.g. our Nature paper, Wedemeyer-Bhom et al. 2012 on how this energy transport takes space in solar tornadoes), where it is dissipated leading to the enormous heating of ambient plasma to millions of K. The details of this energy transport is not yet fully understood. Since the solar atmosphere has a large variety of features, from spicules, fibrils, pores, sunspot, coronal loops, coronal holes, etc. the energisation may be different in each of them. Cardinal questions are: do magnetohydrodynamic (MHD) waves play a key role, or is it the build-up and rapid release of magnetic stresses? Magnetic field is very central in shaping the solar atmosphere because: it (i) not only outlines the MHD waveguides that act as channels for the energy to propagate but, it also (ii) determines connectivity topology; and (iii) stores energy relevant to plasma heating. A viable scenario of this energy channelling is that the both coherent and random (sub)photospheric motions excite MHD waves that sail through the magnetised solar atmosphere, while carrying and damping the necessary of non-thermal energy relevant in the magnetic structures of the solar atmosphere. It is not anymore a question whether MHD waves are there. Instead, focus is now on how the necessary wave flux needed towards plasma heating is present in the magnetised plasma structures and what type of MHD waves are the major players in the energy transport process(es). Here we propose (i) observing and comprehensive tracking MHD waves from photosphere to chromosphere in localised highly dynamic magnetic waveguides with emphases on the magnetic signatures of these waves; (ii) Next, we will determine the actual identity and nature of the detected MHD waves (slow, fast, Alfven; kink, sausage; surface, body; etc.); (iii) We will investigate how these waves are present in a range of structures (e.g. a) spicules at limb; b) swirls in coronal holes)(iv) We will build up statistics of these structures and the waves present therein