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中温度的迅速升高。现在很明显，亚光层运动的机械能被运输到太阳大气中，在那里它被消散，导致环境血浆的加热。这种能量传输的细节尚未完全理解：磁性水力学（MHD）波是否起关键作用，还是磁应力的积累和快速释放？磁场在塑造太阳大气中是中心的，因为它（i）概述了MHD波导；（ii）确定连通性拓扑；（iii）存储与血浆加热相关的能量。这种能量传输的可行场景是，相干和随机（亚）光电运动激发了MHD波，这些波浪在太阳大气中传播，同时携带和抑制大气中的能量相关的能量。是否存在MHD波是否存在，而是一个问题，而是波通量与等离子体加热的相关程度以及能量传输过程中哪种类型的MHD波是哪种类型的MHD波（ES）。在这里，我们提出（i）在局部磁性波导中观察和全面跟踪MHD波，从光球到色球，重点是这些波的磁特征；（ii）接下来，我们将确定检测到的MHD波的实际身份和性质（慢速，快速，Alfven；扭结，香肠；表面，身体；等）；（iii）通过新颖的磁性学科（Verth等人（2010a，b）； Erdelyi等（2010）），我们将不仅确定这些局部MHD波导的形态（是否潜在），而且还将构建其准确的3D磁性图，并尝试通过Spatio-Magneto-Magneto-Magneto-Magneto-sesismology来构建其准确的3D磁性图。