AAS  >> Vol. 2 No. 4 (October 2014)

    太阳日冕软X射线Fe XVII光谱线诊断的理论研究
    Theoretical Study of Diagnostic for Fe XVII Spectral Line in Solar Coronal Soft X-Ray

  • 全文下载: PDF(541KB) HTML   XML   PP.27-32   DOI: 10.12677/AAS.2014.24004  
  • 下载量: 1,442  浏览量: 5,182   国家自然科学基金支持

作者:  

廖腊梅,曹 虹,时永鹏:洛阳师范学院物理与电子信息学院,河南 洛阳;
贺 健:河南科技大学物理工程学院,河南 洛阳

关键词:
太阳日冕不透明度等离子体温度电子数密度Solar Coronal Opacity Plasma Temperature Electron Density

摘要:

本文以太阳日冕软X射线Fe XVII光谱线中1.501 nm谱线为例,分析了不透明度对1.501 nm谱线的影响,再讨论了太阳日冕等离子体温度和电子数密度的诊断原理。结果表明,太阳日冕等离子体温度的数量级为106K ,电子数密度的数量级为1010cm-3,这些都和实际观测数量级完全相同。通过分析,得到了一些重要结论。本研究对太阳日冕等离子体诊断具有重要的参考意义和价值。

In this paper, taking the 1.501 nm spectral line in Fe XVII spectral lines in solar coronal soft X-ray as an example, we analyze the effect of opacity on the 1.501 nm spectral line, then we discuss the diagnostic principle of plasma temperature and electron density. Results show that, the plasma temperature in solar coronal has the 106K order of magnitude, and the electron density has the 1010cm-3 order of magnitude, which has the same order of magnitude in actual observation. Through analysis, we obtain some important conclusions. This study will have reference significance and value in solar coronal plasma diagnostic.

文章引用:
廖腊梅, 曹虹, 时永鹏, 贺健. 太阳日冕软X射线Fe XVII光谱线诊断的理论研究[J]. 天文与天体物理, 2014, 2(4): 27-32. http://dx.doi.org/10.12677/AAS.2014.24004

参考文献

[1] Brichhouse, N.S. and Schmelz, J.T. (2006) The transparency of solar coronal active regions. Astrophysical Journal Letters, 636, L53-L56.
[2] Schmelz, J.T., Saba, J.L.R. and Strong, K.T. (1992) Resonance scattering of Fe XVII—A density diagnostic. Astrophysical Journal, 398, L115-L118.
[3] He, J. and Zhang, Q.G. (2013) Calculation of the effect of opacity in the solar spectral lines of carbon ions. Advances in Space Research, 51, 2002-2009.
[4] He, J. and Liao, L.M. (2012) The opacity of the solar spectral lines of CII 133.5 nm. Spectroscopy Letters, 45, 452-457.
[5] Saba, J.L.R., Schmelz, J.T., Bhatia, A.K. and Strong, K.T. (1999) Fe XVII soft x-ray lines: Theory and data comparisons. Astrophysical Journal, 510, 1064-1077.
[6] Kastner, S.O. and Bhatia, A.K. (1997) Half-widths, escape probabilities and intensity factors of opacity-broadened Doppler- and Voigt-profile lines. Journal of Quantitative Spectroscopy and Radiative Transfer, 58, 217-231.