太阳低层大气磁亮点在不同波段中的特征与相互关系研究

Magnetic bright points (MBPs) in solar lower atomosphere are the tracers of the slender flux tubes. They are taken for the solar minimum-scale magnetic structures which are distinguishable by the present observational technologies. The rapidly transverse motions of MBPs are thought to be an ultimate source of the energy needed to heat the solar corona, either via waves or via magnetic reconnection. The proposal focuses on the quantitative descriptions of the features and the relationships of the solar lower atomospheric MBPs in high-resolution multi-wavelength observations. It will be good for knowing the mechanisms of the heating of coronal, the characteristic of the solar minimum-scale magnetic structures, and the different origins of solar magnetic field. A mass of observational data are adopted, which are obtained from multi-wavelength observations with NVST, NST, SOT and SuFI telescopes. The multi-wavelength data consist of Tio-band、G-band、Ha, Ca II H line, and magnetogram data. We will study the features of solar lower atomospheric MBPs in multi-wavelength observations, the relationships among MBPs in multi-wavelength observations, and the relationships between MBPs in multi-wavelength observations and magnetic field. It aims at the quantitative descriptions of slender flux tubes, including their evolutionary processes on the time dimension, their fine structures and motion transmissions on the three-dimensional space, their interactions, their difference due to the different magnetic strengths, the influence of surrounding magnetic environment, and so on. There are two predominant features. One is extending the study of MBPs to four-dimension which consists of three-dimensional space and time dimension. Another is introducing the advanced information technologies in the field of MBPs, such as genetic algorithm and deep learning.

太阳低层大气中的磁亮点是目前观测技术能够分辨的太阳最小尺度磁场结构——细磁流管的示踪物。其快速的横向运动被认为激发了波或磁重联，将能量传输到高层大气从而加热日冕。本项目通过定量描述多波段高分辨观测中磁亮点的特征与关系，促进理解磁亮点在日冕加热中的作用、太阳最小磁结构的特性和太阳磁场的不同起源等科学问题。项目采用NVST的G、Tio、Ca II H和Ha等多个波段的数据，辅以NST、SOT和SuFI的数据和磁场数据。主要研究太阳低层大气不同波段磁亮点的特征提取、不同波段磁亮点的关系、不同波段磁亮点和磁场的关系等内容，为细磁流管的时间维度的演化、三维空间维度的精细结构和运动传递、细磁流管之间的相互作用、不同磁场强度的细磁流管的区别、周围磁场环境对细磁流管的影响等方面提供观测上的定量描述。主要特色为：将磁亮点的研究扩展到三维空间加时间的四维模式；结合深度学习和遗传算法等先进信息技术。

太阳低层大气中的磁亮点是目前观测技术能够分辨的太阳最小尺度磁场结构——细磁流管的示踪物。其快速的横向运动被认为激发了波或磁重联，将能量传输到高层大气从而加热日冕。目前对多波段亮点的特征提取及其之间的关系方面的研究还比较缺乏。本项目采用NVST的Tio、NST的TiO和Ha多个偏带、SOT的G和Ca II H数据和磁场数据，研究了太阳低层大气不同波段观测数据的预处理,主要包括降噪、对齐和配准等问题，提出了基于贝叶斯的降噪方法，提出了用深度学习的思路进行对齐和配准的一些可行方法；研究了太阳低层大气不同波段磁亮点的检测、识别、分类和跟踪方法，以及不同波段磁亮点的匹配问题，提出了基于拉普拉斯、区域生长、阈值法等技术的磁亮点检测方法、基于三维分割的磁亮点跟踪方法、基于深度学习的磁亮点形态分类方法、基于深度学习的多波段磁亮点匹配方法等一系列方法；研究了太阳低层大气不同波段磁亮点的特征提取、不同波段磁亮点之间的关系、不同波段磁亮点和磁场的关系等问题，提供了不同波段磁亮点的主要特征的定量描述，分析了细磁流管的时间维度的演化、三维空间维度的精细结构和运动传递、细磁流管之间的相互作用、不同磁场强度的细磁流管的区别、周围磁场环境对细磁流管的影响等问题。本项目填补了多波段磁亮点研究领域中的多项空白，通过定量描述多波段高分辨观测中磁亮点的特征与关系，对促进理解磁亮点在日冕加热研究领域中具有非常重要的意义。