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Travel grant for ROSA DST/Sacramento Peak Observations: Magnetic mapping of the chromosphere - Magneto-seismology of bright points

ROSA DST/萨克拉门托峰观测的旅费补助：色球层磁测图 - 亮点磁地震学

基本信息

批准号：
ST/I000844/1
负责人：
Robert Von Fay-Siebenburgen
金额：
$ 0.19万
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%2FI000844%2F1
关键词：
Travel grant ROSA DST Sacramento

项目摘要

The rapid rise of plasma temperature up to 1-2 MK from the solar photosphere towards the corona is still an unresolved problem in solar physics. It is clear that the mechanical energy of sub-photospheric motions is transported somehow into the upper solar atmosphere, where it may be dissipated leading to the heating of the ambient plasma. A key role in the energy transport is played by the magnetic field because: the magnetic field (i) outlines the shape of magnetohydrodynamic (MHD) waveguides; (ii) guides MHD waves; (iii) determines connectivity topology; and (iv) contributes to plasma heating. A viable scenario of this energy transport is that the convective motions and solar global oscillations may excite MHD waves in the (sub-)photosphere, which may then propagate through the chromosphere carrying relevant energy into the corona. If MHD waves play a role in the energy transport process(es), it is of great importance that these waves are tracked observationally from where they are generated in the lower solar atmosphere. It is also of fundamental importance to understand the nature of magnetic topology (e.g. force free or non-force free, helicity, etc.) in order to reveal the available free energy stored in magnetic structures. Here we propose (i) observing and tracking MHD waves from photosphere to chromosphere in magnetic bright points; (ii) Next, by means of magneto-seismology of bright points, we will determine not just the nature of these important features (potential or not) but will also construct for the first time their 3D magnetic map.

从太阳光球层到日冕的等离子体温度快速上升高达 1-2 MK，仍然是太阳物理学中尚未解决的问题。很明显，亚光球运动的机械能以某种方式传输到上层太阳大气中，在那里它可能被消散，导致周围等离子体的加热。磁场在能量传输中发挥着关键作用，因为：磁场 (i) 勾勒出磁流体动力学 (MHD) 波导的形状； (ii) 引导 MHD 波； (iii) 确定连接拓扑； (iv)有助于等离子体加热。这种能量传输的一个可行方案是，对流运动和太阳全球振荡可能会在（亚）光球层中激发 MHD 波，然后该波可能通过色球层传播，将相关能量带入日冕。如果 MHD 波在能量传输过程中发挥作用，那么从太阳低层大气中产生这些波的地方对这些波进行观测跟踪就非常重要。了解磁性拓扑的本质（例如无力或非无力、螺旋性等）对于揭示磁性结构中存储的可用自由能也至关重要。在这里，我们建议（i）观察和跟踪磁性亮点中从光球层到色球层的 MHD 波； (ii) 接下来，通过亮点磁地震学，我们不仅将确定这些重要特征的性质（潜在的或潜在的），还将首次构建它们的 3D 磁图。