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耐人寻味的问题之一是磁化的太阳大气中温度的快速上升。现在很明显，亚光球颗粒运动的巨大机械能的一部分被输送到太阳大气中(例如，参见我们的《自然》论文，韦德迈耶-博姆等人)。关于这种能量传输如何在太阳龙卷风中占据空间)，它在哪里消散，导致环境等离子体被巨大加热到数百万K。这种能量传输的细节尚未完全了解。由于太阳大气有各种各样的特征，从针状物、纤维、气孔、太阳黑子、日冕环、日冕洞等等，它们的能量可能是不同的。主要的问题是：磁流体动力(MHD)波起关键作用吗，还是它是磁应力的积累和快速释放？磁场在塑造太阳大气方面非常重要，因为：(I)它不仅勾勒出充当能量传播通道的MHD波导，而且(Ii)确定连接拓扑；(Iii)存储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(次)光球层运动都会激发MHD波，这些MHD波穿过磁化的太阳大气，同时携带和抑制与太阳大气的磁结构相关的非热能。MHD波是否存在已不再是一个问题。相反，现在的焦点是如何在磁化等离子体结构中存在必要的等离子体加热所需的波通量，以及在能量传输过程中哪种类型的MHD波是主要参与者。在这里，我们建议(I)观测和全面跟踪局域高动态磁波波导中从光球到色球的MHD波，重点是这些波的磁特征；(Ii)接下来，我们将确定检测到的MHD波(慢、快、阿尔芬；扭结、香肠；表面、身体等)的实际身份和性质；(Iii)我们将调查这些波如何存在于一系列结构中(例如，a)肢体针状物；b)日冕洞中的漩涡)(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