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The spectral data of a lightning discharge process are captured by a high-speed slit-less grating spectrograph. Based on the plasma spectrum theory, the lightning return stroke channel temperature is estimated according to the spectral information of the different bands. The results show that the average temperatures of the lightning return stroke channel estimated by the Boltzmann plot method are 43270, 17660 and 17730 K, respectively, when the spectral line group of the single ionized nitrogen atom (NII), neutral oxygen atom (OI) and neutral nitrogen atom (NI) are selected respectively. The average temperature of the lightning return stroke channel is 24770 K, which is estimated based on the Saha-Boltzmann plot method by using NII and NI spectral line groups. Based on the lightning channel corona sheath model and the spectral radiation theory, it can be inferred that the temperature obtained by using only NII spectral line group should be the temperature of the lightning return stroke channel core, and the temperature obtained by using only NI or OI spectral line group should be the temperature of the corona sheath around the lightning return stroke channel core. Using both NII and NI spectral line groups, the obtained temperature should be the average temperature of the entire channel section (including the channel core and corona sheath) in the exposure time.
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Keywords:
- spectral diagnosis /
- lightning return stroke channel temperature /
- Boltzmann plot method /
- Saha-Boltzmann plot method
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图 1 闪电原始光谱图
Figure 1. Original spectrum of lightning.
图 2 六个采样点的谱线图
Figure 2. Spectral diagram of six sampling points.
表 1 不同谱线组估算所得的六个采样点的温度(单位: K)
Table 1. Temperature of six sampling points estimated by different spectral line groups (unit: K).
谱线组 1 2 3 4 5 6 平均值 NII 43680 42850 43250 44410 42980 42440 43270 NI 18600 42850 17170 16710 17300 18990 17660 OI 17520 17130 18190 17690 17200 18220 17730 NII和NI 24800 25110 24780 24710 24530 24670 24770 
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[1] Prueitt M L 1963 J. Geophys. Res. 68 803
Google Scholar
[2] Orville R E 1968 J. Atmos. Sci. 25 839
Google Scholar
[3] Uman M A 1969 J. Geophys. Res. 74 4
[4] Walker T D, Christian H J 2019 J. Geophys. Res. 124 3930
Google Scholar
[5] 欧阳玉花, 袁萍, 贾向东 2006 西北师范大学学报(自然科学版) 42 49
Ouyang Y H, Yuan P, Jia X D 2006 J. Northwest Normal Univ. (Natural Science) 42 49
[6] Wan R, Yuan P, An T, Liu G, Wang X, Wang W, Huang X, Deng H 2021 J. Geophys. Res. 126 e2021JD035387
[7] Kunze H J 2009 Introduction to Plasma Spectroscopy (Berlin: Springer) pp187–192
[8] Aguilera J A, Aragón C 2004 Spectrochim. Acta, Part B 59 1861
Google Scholar
[9] Griem H R 1964 Plasma Spectroscopy (New York: McGraw-Hill) pp267–295
[10] Griem H R 1997 Principles of Plasma Spectroscopy (New York: Cambridge University Press) pp279–287
[11] Yalcin X, Crosley D R, Smith G P, Faris G W 1998 Appl. Phys. B 68 121
[12] Cen J Y, Yuan P, Xue S M 2014 Phys. Rev. Lett. 112 035001
Google Scholar
[13] Cen J Y, Yuan P, Xue S M, Wang X J 2015 Appl. Phys. Lett. 106 054104
Google Scholar
[14] 王雪娟, 袁萍, 岑建勇, 张廷龙, 薛思敏, 赵金翠, 许鹤 2013 62 109201
Google Scholar
Wang X J, Yuan P, Cen J Y, Zhang T L, Xue S M, Zhao J C, Xu H 2013 Acta Phys. Sin. 62 109201
Google Scholar
[15] 王雪娟 许伟群 王海通 杨静 袁萍 张其林 化乐彦 张袁瞰 2021 70 099202
Google Scholar
Wang X J, Xu W Q, Wang H T, Yang J, Yuan P, Zhang Q L, Hua L Y, Zhang Y K 2021 Acta Phys. Sin. 70 099202
Google Scholar
[16] Dong C X, Yuan P, Cen J Y, Wang X J, Mu Y L 2016 Atmos. Res. 178–179 1
[17] Maslowski G, Rakov V A 2006 J. Geophys. Res. 111 D14110
Google Scholar
[18] Cvetic J, Heidler F, Markovic S, Radosavljevic R, Osmokrovic P 2012 Atmos. Res. 117 122
Google Scholar
[19] Maslowski G, Rakov V A 2013 Atmos. Res. 129–130 117
[20] Ignjatovic M, Cvetic J, Heidler F, Markovic S, Djuric R 2014 Atmos. Res. 149 333
Google Scholar
[21] Wang X J, Yuan P, Cen J Y, Liu G R 2016 J. Geophys. Res. Atmos. 121 8615
Google Scholar
[22] Wang X J, Yuan P, Cen J Y, Liu G R 2017 J. Geophys. Res. Atmos. 122 4993
Google Scholar
[23] Liu G R, Yuan P, An T T, Cen J Y, Wang X J 2019 Appl. Phys. Lett. 115 064103
Google Scholar
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