太阳活动区内振荡现象的统计研究及理论探索

With the help of the large number of the high-resolution data observed by NVST in the spectral lines Ha, G-band and TiO,and the multi-band data observed by Solar-B and SDO, this project will undertake some basic research about the oscillations and running waves within the solar active region. The real period and propagation velocity of these running waves will be measured accurately by using the statistical methods and periodic analysis methods. The nature of the solar oscillations and their role in the eruption of the solar flares and CME are also investigated in this project. In the work, the propagation velocity of these running waves will be measured by fitting their traveling tracks, and the periods of these physical quantities, such light intensity I and velocity V related to the running waves be exactly measured by using these methods of wavelet analysis and Fourier transform. Furthermore, the statistical method will be used to analyze the distributions of the extreme values on the observed light intensity profiles and velocity profiles. On the basis of these profiles, the relationship between the real period of the waves and the periods of the observable quantities will be determined. And then, the real period of the waves will be obtained on the basis of the measured periods of these observable quantities and the relationship between period of waves and periods of the observable quantities. The measured result of the real period of the waves will help us to prove that the umbral oscillations and the running penumbral waves may be a pair of different phenomena relating to a same running waves with a period of about 300s. The affect of the quantities, such as vector magnetic field, plasma density and temperature, to the running waves will also be investigated in this project. Some exploratory work that the effect of the solar oscillations to the eruption of the high-energy activity are also carried out in this project.

本项目着重利用NVST在Ha、G-band、TiO等谱线观测的大量高分辨率数据，结合Solar-B、SDO等观测的多波段数据，应用统计方法和周期分析方法准确测定太阳振荡和行波的真实周期、传播速度等，深入研究太阳振荡的物理本质，探索振荡和行波等客体在太阳耀斑、CME等高能活动中的作用和影响。工作中，除了通过拟合行波传播轨迹测量行波传播速度、利用小波分析及傅里叶变换等工具精确测量与本影振荡和半影行波紧密联系的光强I、速度v等的变化周期外，还对I--t曲线、v--t曲线的极值特征进行统计研究，确定光强、速度等可观测量的极值分布，从而得到可观测量周期与行波周期之间的函数，进而确定行波周期。结果可能证实本影振荡和半影行波是由周期约300秒的行波所产生的不同观测现象。活动区的矢量磁场结构、等离子体密度和温度等对行波的影响，太阳振荡在太阳高能活动爆发中的作用和影响也将做一些探索性工作。

望远镜SDO、NVST等在多波段观测的高分辨率数据为我们研究太阳振荡和行波、暗条爆发、耀斑爆发等活动现象提供了便利条件，我们应用这些数据的比较系统地研究了这些活动现象的物理参数，并且探讨了它们的可能演化过程及活动规律。本项目依托这些高质量数据就太阳振荡、暗条爆发、矢量磁场计算电流结构等做了一些基础性的工作，获得了一些具有积极意义的研究成果。在项目执行期间，共计发表学术论文7篇（其中5篇已正式发表，2篇已正式接收排版中），其中SCI收录论文3篇，国内核心期刊2篇，申请并被授权专利2项，硕士毕业4人，成功举办一次全国性的天文学术研讨会“第一届西南天文观测与技术研讨会”。取得了如下主要创新成果：1）利用SDO、NVST等望远镜观测的数据详细研究了位于太阳高层中的太阳振荡和波动现象，获得了该行波的传播速度、传播方向角等波的及特务特性，发现该波动的可能扰动源为耀斑等；（2）利用SDO、NVST两个望远镜观测的数据研究了另一种太阳振荡的扰动源太阳暗条的演化特征，发现一种有趣的活动现象，即两个临近的暗条会相互挤压碰撞，并最终形成活动区增亮以及暗条爆发现象。（3）研究了太阳高能活动与活动区内的电流结构的相互关系，论证了太阳活动区电流计算的最优化方法是安培定律的积分形式，计算出的电流结构与耀斑的爆发位置和形态具有较强的相关性。（4）研究了耀斑对应的活动区内电流结构随时间的演化过程，结果发现在耀斑爆发时，电流强度会出现快速的显著增强现象。（5）为了引导学生理解磁场与原子核之间的相互作用过程以及引导学生学会望远镜的工作原理和使用方法，在研究和教学过程中教会学生拆卸和安装仪器，学生申请并被授权了两项专利。