Travel grant for ROSA DST/Sacramento Peak Observations: Hunt for MHD waves - Magneto-seismology of pores and MBPs

现代天体物理学最吸引人的问题之一是太阳大气温度的快速上升。现在很清楚，亚光球运动的机械能被输送到太阳大气中，在那里它被耗散，导致周围等离子体的加热。这种能量传输的细节目前还不完全清楚：磁流体动力(MHD)波起关键作用，还是它是磁应力的积累和快速释放？磁场是塑造太阳大气的核心，因为：它(I)勾勒出MHD波导的轮廓；(Ii)确定连接拓扑；(Iii)存储与等离子体加热相关的能量。这种能量传输的一个可行方案是，相干和随机(次)光球层运动都会激发通过太阳大气传播的MHD波，同时在大气中携带和衰减与能量相关的能量。现在的问题不再是MHD波是否存在，而是波通量与等离子体加热的相关性如何，以及在能量传输过程(ES)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磁波导中从光球层到色球的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、Alfven；扭结、香肠；表面、身体等)的实际身份和性质；(Iii)通过新的磁震学手段(Verth等人)。(2010a，b)；Erdelyi等人。(2010))，我们将不仅确定这些局域MHD波导的形态(可能与否)，而且还将构建它们准确的3D磁图，并试图通过空间-磁震-地震学确定它们的加热贡献。

One of the most appealing problems of modern astrophysics is the rapid rise of temperature in the solar atmosphere. It is now clear that mechanical energy of sub-photospheric motions is transported into the solar atmosphere, where it is dissipated leading to the heating of ambient plasma. The details of this energy transport is not yet fully understood: do magnetohydrodynamic (MHD) waves play a key role, or is it the build-up and rapid release of magnetic stresses? Magnetic field is central in shaping the solar atmosphere because: it (i) outlines the MHD waveguides; (ii) determines connectivity topology; and (iii) stores energy relevant to plasma heating. A viable scenario of this energy transport is that the both coherent and random (sub)photospheric motions excite MHD waves that propagate through the solar atmosphere, while carrying and damping energy relevant energy in the atmosphere. It is not anymore a question whether MHD waves are there, but how relevant the wave flux is towards plasma heating 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 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) By means of novel magneto-seismology (Verth et al. (2010a,b); Erdelyi et al. (2010)), we will determine not just the morphology of these localised MHD waveguides (potential or not) but will also construct their accurate 3D magnetic map and attempt to determine their heating contribution through spatio-magneto-seismology.