| 其他摘要 | The sun is the most concerned about human star in the universe, and directly impacts our production and life. The observation of sun has always been the hot spot in the astronomy, the sun is a natural laboratory when we study the physical processes under extreme conditions. A large number of observations show that the physical state of solar upper atmosphere can seriously affect the Earth's space environment. Therefore, to research the dynamic properties and the material cycle progresses in the region, it also has practical significance for human survival and development. Solar spectrum is a major tool to study the physical properties of the solar atmosphere. A total solar eclipse is the best time to observe the solar upper atmosphere, in general, it has a complex morphology and frequent activities in this region. In this paper, using the spectra observed by Fiber Arrayed Solar OpticTelescope (FASOT) to study the spectral profiles and their physical nature, at the same time, the motion characteristics of the solar atmosphere are also discussed.When the total solar eclipse occurs, the strong emission lines, namely flash spectrum, can be observed at the solar edges. The lines can provide the important information to study the physical properties of the plasma. Complex material recycling process leads to the spectral profile appears asymmetries, both coronal heating mechanism and the formation of the solar wind provides a possible theoretical models, but also for spectral analysis to provide the necessary technical means; In addition, the characteristics in different lines of the solar atmosphere show the complex movement. November 3, 2013, using FASOT to observe the spectral band range from 516 nm to 531 nm during total solar eclipse in the territory of the Republic of Gabon, through different research methods, we analyzed the spectrum lines wing emission enhancement phenomena. Combined with the existing theoretical models, we explored the Solar Dynamics features.By applying the observed data, we do a statistical research to the characteristics of different emission lines. After executing a single Gaussian fit, we can obtain the parameters of spectral profiles. The results show that there is a clear relationship between these parameters and the wavelengths, the spectral width and the Doppler velocity is a function of wavelength. Specific studies have shown that polynomial fit can accord with observations well. This is a new approach to learn more about the movement of solar material. Based on the findings, we suggest that it should examine the observed features of whole spectrum, and not just studying the nature of the solar atmosphere by one of the spectral. Of course, the more accurate and detailed research, need further modeling and computing. |
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