太阳光球和色球磁亮点的多波段观测模式与数值分析方法探讨

项目名称： 太阳光球和色球磁亮点的多波段观测模式与数值分析方法探讨

项目编号： No.U1531140

项目类型： 联合基金项目

立项/批准年度： 2016

项目学科： 天文学、地球科学

项目作者： 邓林华

作者单位： 中国科学院云南天文台

项目金额： 43万元

中文摘要： 日冕加热机制是太阳物理领域十分重要的研究课题之一。光球和色球磁亮点是扎根于米粒暗径里的超精细磁流管结构，其足点的快速横向本征运动通过激发磁波或磁重联的方式将磁能向上传输到高层大气并加热日冕。本项目立足于NVST的高分辨多波段观测资料，结合SDO和Hinode的高层大气和磁场数据，运用多种图像处理技术和数值分析手段开展对磁亮点的高分辨观测特征研究。本项目拟在（1）NVST光球和色球的多波段观测模式和策略的选取与优化；（2）磁亮点在光球和色球多个波段、宁静区和活动区及冕洞区的物理异同性；（3）光球和色球磁亮点的湍流扩散、波动和振荡行为等方面取得定性和定量的分析结果。在此基础之上，深刻理解光球和色球磁亮点在揭示日冕加热机制和局部湍流发电机理论中的作用，探索磁亮点与色球针状体、微耀斑和纳耀斑等小尺度宁静和爆发现象的物理联系，进而评估NVST在解决太阳物理前沿热点问题中的科学地位并提供观测指导建议。

中文关键词： 磁亮点；日冕加热；局部发电机；观测模式；数值分析

英文摘要： The heating of the solar corona to high temperatures is one of the most important problems in solar physics. Solutions have been hampered by an incomplete understanding of the magnetically controlled structures in the lower solar atmosphere. Magnetic bright points (MBPs) in the photosphere and chromosphere of the Sun, located in the dark inter-granular lanes, are ultrafine magnetic structures that are extensively used as reliable tracers for magnetic flux tubes. The rapidly transverse motions of the footpoints of photospheric MBPs are thought to be an ultimate source of the energy needed to heat the solar corona, either via waves or via magnetic reconnection of intertwined flux tubes. Based on the ultra-high-resolution ( about 0.1″-0.2″) and multi-wavelength observations with the New Vacuum Solar Telescope (NVST) and the data of both upper solar atmosphere and magnetogram provided by SDO and Hinode, we will study the high-resolution observational characteristics and physical mechanism of MBPs with the help of several image processing techniques and numerical analysis approaches. We will work on (1) selection and optimization of multi-wavelength observational modes for NVST; (2) physical similarities and distinctions of MBPs located in photosphere and chromosphere, and in the quite-Sun area, the active region, and the coronal hole; (3) turbulent diffusion, magnetic wave modes, and oscillatory behavior of photospheric and chromospheric MBPs, and obtain the qualitative and quantitative results. We aim our studies at getting better understanding about their crucial roles in the coronal heating mechanism and local turbulent dynamo, and the physical relationship between MBPs and small-scale quiet and explosive phenomena, such as spicules, microflare and nanoflare. Finally, we will evaluate the scientific status of NVST that solving the frontier and hot topics in solar physics, and will provide some observational suggestions or comments for NVST.

英文关键词： Magnetic Bright Points;Coronal Heating;Local Dynamo;Observational Modes ;Numerical Analyses