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

ROSA DST/萨克拉门托峰观测旅行补助金：寻找 MHD 波 - 孔隙磁地震学和 MBP

基本信息

批准号：
ST/I00341X/1
负责人：
Robert Von Fay-Siebenburgen
金额：
$ 0.25万
依托单位：
University of Sheffield
依托单位国家：
英国
项目类别：
Research Grant
财政年份：
2010
资助国家：
英国
起止时间：
2010 至无数据
项目状态：
已结题

来源：
https://gtr.ukri.org/projects?ref=ST%2FI00341X%2F1
关键词：
Travel grant ROSA DST Sacramento

项目摘要

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.

现代天体物理学最吸引人的问题之一是太阳大气层温度的迅速上升。现在很清楚，亚光球运动的机械能被传输到太阳大气中，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尚未完全了解：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？磁场是塑造太阳大气的核心，因为：它（i）勾勒出MHD波导;（ii）确定连接拓扑结构;（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的方案是，相干和随机（子）光球运动激发MHD波，通过太阳大气传播，同时携带和阻尼能量相关的能量在大气中。这不再是一个问题，是否有MHD波，但如何相关的波通量是对等离子体加热和什么类型的MHD波是主要的球员在能量传输过程（ES）。在这里，我们提出：（1）在局部磁波导中观测和全面跟踪从光球到色球的MHD波，重点是这些波的磁特征;（2）接下来，我们将确定所探测到的MHD波的实际身份和性质（慢，快，阿尔芬;扭结，香肠;表面，身体等）; (iii)通过新的磁震学（Verth等人（2010 a，B）; Erdelyi等人（2010）），我们不仅将确定这些局部MHD波导的形态（潜在的或不潜在的），而且还将构建其精确的3D磁图，并试图通过空间磁震学确定其加热贡献。