AAS  >> Vol. 3 No. 1 (January 2015)

    利用电子碰撞模型诊断星际介质H II空间温度的理论模拟
    Theoretical Simulation of Temperature Diagnostic for the H II Interstellar Medium Space Using the Electron Impact Model

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贺 健,张庆国:河南科技大学物理工程学院,河南 洛阳

星际介质碰撞平衡温度诊断S III离子河南科技大学物理工程学院河南 洛阳


本文利用离子和自由电子碰撞产生的激发和退激发模型,理论分析了星际介质等离子体的碰撞平衡条件,并且分析了在碰撞平衡条件下三能级等离子体的温度诊断的原理。以星际介质H II空间的S III离子为例,分析了碰撞平衡条件下根据谱线强度比诊断等离子体温度的原理和方法,并和常用的局域热平衡条件下的温度诊断进行了比较,得到了一些重要结论。本研究对空间等离子体温度诊断具有重要参考意义和价值。

In this paper, using the excitation and de-excitation by impact of ion and free electron, we analyze the impact equilibrium condition of interstellar medium plasma, and discuss the diagnostic prin-ciple for temperature diagnostic for the plasma with three levers. Taking the S III ion in H II in-terstellar medium space as an example, we discuss the temperature diagnostic principle and me-thod by intensity ratio under the condition of impact equilibrium, and compare the result with under the condition of local thermal equilibrium, and we obtain some important conclusions. This study will be significant in space plasma diagnostic.

贺健, 张庆国. 利用电子碰撞模型诊断星际介质H II空间温度的理论模拟[J]. 天文与天体物理, 2015, 3(1): 1-6. http://dx.doi.org/10.12677/AAS.2015.31001


[1] Tayal, S.S. (1997) Effective collision strengths for electron impact excitation of inelastic transitions in S III. Astrphysical Journal, 481, 550-556.
[2] Herter, T., Briotta Jr., D.A., Gull, G.E., Shure, M.A. and Houck, J.R. (1982) Observations of the infrared fine-structure lines of S III at 18.71 and 33.47 microns in four H II regions. Astrphysical Journal, 262, 164-170.
[3] Herter, T., Houck, J.R., Shure, M.A., Gull, G.E. and Graf, P. (1984) The electron density in the galactic center as derived from the S III 18.71/33.47 micron line ratio. Astrphysical Journal, 287, L15-L18.
[4] He, J., Zhang, Q.G. and Zhang, H.Q. (2012) Effect of opacity on the solar spectral line of C I 165.7 nm by escape factor treatment. Spectroscopy Letters, 45, 563-568.
[5] 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.
[6] He, J. and Liao, L.M. (2012) The opacity of the solar spectral lines of CII 133.5 nm. Spectroscopy Letters, 45, 452-457.
[7] Ya’akobi, B. and Avivi, P. (1969) A diagnostic method for a plasma in local thermodynamic equilibrium. Journal of Physics B: Atomic, Molecular and Optical Physics, 2, 706-712.
[8] Fincke, J.R. (1996) Advanced diagnostic techniques for thermal plasmas. Pure and Applied Chemistry, 68, 1001-1006.
[9] Ramsbottom, C.A., Belli, K.L. and Keenan, F.P. (1997) Effective collision strengths for fine-structure forbidden transitions among the 3s23p3 levels of Ar IV. Monthly Notices of the Royal Astronomical Society, 284, 754-760.
[10] Tayal, S.S. and Gupta, G.P. (1999) Collision strengths for electron collision excitation of fine-structure levels in S III. Astrphysical Journal, 526, 544-548.