Line identification of extreme ultraviolet spectra of Mo V to Mo XVIII in EAST tokamak

Zhang Wen-Min; Zhang Ling; Cheng Yun-Xin; Wang Zheng-Xiong; Hu Ai-Lan; Duan Yan-Min; Zhou Tian-Fu; Liu Hai-Qing

doi:10.7498/aps.71.20212383

Abstract

The presence of high-Z impurities in magnetically confined fusion devices has different influences on the confinement property of the plasma due to the high cooling rate of high-Z impurities. The first wall of EAST is equipped with molybdenum tiles, molybdenum particles sputtered from inevitable plasma-wall interaction enter into the plasma and become high-Z impurity. In this paper, four fast-time-response extreme ultraviolet (EUV) spectrometers, a system which is upgraded in the EAST 2021 campaign, are used to monitor the line emission from impurity ions in the 5–500 Å wavelength range simultaneously. The in-situ wavelength calibration is carried out accurately using several well-known emission lines of low- and medium-Z impurity ions. The observed spectral lines are carefully identified based on the National Institute of Standards Technology (NIST) database, previously published experimental data and the time evolution of the normalized line intensity of emission lines from impurity ions. At the lower electron temperature (T_e0 = 1.5 keV), the EUV spectra emitted from molybdenum ions in the range of 5–485 Å are systematically identified in EAST discharges accompanied with spontaneous sputtering events. As a result, two unresolved transition arrays of molybdenum spectra composed of Mo¹⁹⁺-Mo²⁴⁺ (Mo XX-Mo XXV) and Mo¹⁶⁺-Mo²⁹⁺ (Mo XVII-Mo XXX) are observed in the ranges of 15–30 Å and 65–95 Å. In addition, several spectral lines of lower molybdenum ions of Mo⁴⁺-Mo¹⁷⁺ (Mo V-Mo XVIII) in the ranges of 27–60 Å and 120–485 Å are observed and identified on EAST for the first time, including a few strong and isolated forbidden and resonant lines, e.g. Mo XII at 329.414 Å, 336.639 Å and 381.125 Å, Mo XIII at 340.909 Å and 352.994 Å, Mo XIV at 373.647 Å and 423.576 Å, Mo XV at 50.448 Å, 57.927 Å and 58.832 Å. Six spectral lines are newly observed in the range of 27–32 Å, i.e. (27.21 ± 0.01) Å, (27.37 ± 0.01) Å, (28.99 ± 0.01) Å, (30.81 ± 0.01) Å, (31.54 ± 0.01) Å and (31.83 ± 0.01) Å, which may be Mo XV-Mo XVIII spectral lines. As a result, twelve strong and isolated spectral lines are chosen in routine observation for impurity transport physical study. The identification of these spectral lines not only enriches the molybdenum atom database, but also provides a solid experimental data base for magnetically confined devices to study the behavior and transport in core and edge plasmas of high-Z impurity.

Keywords:

Authors and contacts

1.
School of Physics, Dalian University of Technology, Dalian 116024, China
2.
Institute of Plasma Physics, Chinese Academy of Sciences, Hefei 230031, China
3.
Science Island Branch of Granduate Suchool, University of Science and Technology of China, Hefei 230026, China

Corresponding author: Zhang Ling, zhangling@ipp.ac.cn ; Wang Zheng-Xiong, zxwang@dlut.edu.cn ;

Funds: Project supported by the National MCF Energy R&D Program, China (Grant No. 2022YFE03180400 ), the National Natural Science Foundation of China (Grant No. 11925501), and the National Key Research and Development Program of China (Grant Nos. 2018YFE0311100, 2019YFE030403)

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References

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Cited By

图 1 极紫外光谱仪的光路设计　(a) 短波段快速EUV谱仪; (b) 长波段快速EUV谱仪

Figure 1. Optical layout of fast-time-response EUV spectrometer: (a) EUV_Short; (b) EUV_Long_a, EUV_Long_b, EUV_Long_c.

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图 2 EAST极向截面、最外磁面(红色线)以及4套快速极紫外光谱仪观测弦

Figure 2. EAST poloidal cross section and the last closed magnetic surface (red line), and lines of sight of four fast-time-response EUV spectrometers on EAST.

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图 3 发生钼杂质溅射的典型波形图　(a) 等离子体电流I_p; (b) 低杂波、离子回旋和中性束加热功率(P_LHW, P_ICRF, P_NBI); (c) 芯部弦平均电子密度n_e; (d) 归一化的Mo V 258.069 Å和Mo XXIV 70.726 Å线辐射强度(I_{Mo V}, I_{Mo XXIV}); (e) 归一化的边界辐射和芯部辐射强度(Edge I_AXUV, Core I_AXUV)

Figure 3. Typical waveform of discharge with molybdenum impurity sputtering: (a) plasma current, I_p; (b) heating power of low hybrid wave, P_LHW, ion cyclotron range of frequency heating, P_ICRF, and neutral beam injection, P_NBI; (c) central line-averaged electron density, n_e; (d) normalized intensities of Mo V at 258.069 Å, I_{Mo V}, and Mo XXIV at 70.726 Å, I_{Mo XXIV}; (e) normalized radiation intensities observed by fast AXUV system along an edge and central chord, Edge I_AXUV, and Core I_AXUV, respectively.

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图 4 EAST #101700放电中钼杂质爆发前后辐射分布　(a) 9.1—9.9 s的时间演化; (b) t = 9.172 s, 9.480 s, 9.497 s 3个时刻

Figure 4. Radiation profiles before and after the molybdenum impurity burst in EAST #101700 discharge: (a) Time evolutions during 9.1–9.9 s; (b) at three timings of t = 9.172 s, 9.480 s and 9.497 s.

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图 5 EAST #101700放电钼杂质爆发前325 ms(灰色线, t = 9.172 s)和爆发期间(蓝色线, t = 9.497 s)观测5—485 Å波段范围的EUV光谱　(a) 5—45 Å; (b) 45—165 Å; (c) 165—285 Å; (d) 285—485 Å

Figure 5. EUV spectra observed 325 ms before (grey lines, t = 9.172 s) and during (blue lines, t = 9.497 s) the molybdenum burst at the wavelength ranges of 5–485 Å in EAST discharge #101700: (a) 5–45 Å; (b) 45–165 Å; (c) 165–285 Å; (d) 285–485 Å.

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图 6 EAST #101700放电中四条钼离子归一化谱线强度随时间的演化　(a) Mo VII 235.694 Å; (b) Mo XV 57.928 Å, 2^nd Mo XV 115.856 Å; (c) Mo XXIV 70.726 Å

Figure 6. Time evolutions of the four molybdenum ions normalized line emission intensities in EAST #101700 discharge: (a) Mo VII at 235.694 Å; (b) Mo XV at 57.928 Å and 2^nd Mo XV at 115.856 Å; (c) Mo XXIV at 70.726 Å.

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表 1 在EUV波段识别的钼谱线

Table 1. Identified molybdenum lines in EUV range.

谱线	离子	电离能/eV	波长/Å		跃迁能级
谱线	离子	电离能/eV	实验值	参考值	跃迁能级
Mo V	Mo⁴⁺	54.42	258.09 ± 0.03	258.069	4p⁵4d³ ₃ → 4p⁶4d² ¹D₂
			324.98 ± 0.02	324.979	4p⁶4d5f ³H°₄ → 4p⁶4d² ³F₄
			327.13 ± 0.01	327.167	4p⁵4d³ ₃ → 4p⁶4d² ³P₂
Mo VI	Mo⁵⁺	68.83	227.75 ± 0.04	227.801	4p⁵(²P°)4d(³F)5s ²F°_5/2→4p⁶4d ²D_5/2
Mo VI	Mo⁵⁺	68.83	229.20 ± 0.04	229.262	4p⁶6f ²F°_5/2 →4p⁶4d ²D_3/2
Mo VII	Mo⁶⁺	125.64	151.85 ± 0.04	151.747	4s²4p⁵(²P°_3/2)5d ²[1/2] °₁ → 4s²4p⁶ ¹S₀
Mo VII	Mo⁶⁺	125.64	235.66 ± 0.05	235.694	4s²4p⁵(²P°_3/2)5f ²[3/2]₁ → 4s²4p⁵(²P°_1/2)4d ²[3/2]°₂
Mo VIII	Mo⁷⁺	143.6	133.18 ± 0.03	133.168	4s²4p⁴(³P)5d ²P_3/2→4s²4p⁵ ²P°_3/2
			134.34 ± 0.03	134.362	4s²4p⁴(³P)5d ⁴F_5/2→4s²4p⁵ ²P°_3/2
			136.83 ± 0.03	136.782	4s²4p⁴(³P)5d ²D_3/2→4s²4p⁵ ²P°_3/2
Mo IX	Mo⁸⁺	164.12	132.03 ± 0.03	132.077	4s²4p³(²P°)5d ³P°₁→4s²4p⁴ ¹S₀
			158.53 ± 0.03	158.641	4s²4p³(²P°_1/2)5s (1/2, 1/2)°₁→4s²4p⁴ ³P₂
			176.67 ± 0.04	176.682	4s²4p³(²D°_3/2)5s (3/2, 1/2)°₂→4s²4p⁴ ¹D₂
			231.90 ± 0.05	231.991	4s²4p³(²D°)4d ¹F°₃→4s²4p^{4 1}D₂
			237.76 ± 0.05	237.843	4s²4p³(²D°)4d ¹D°₂→4s²4p^{4 1}D₂
Mo X	Mo⁹⁺	186.3	152.54 ± 0.04	152.683	4s²4p²(³P)5s ⁴P_3/2 →4s²4p³ ⁴S°_3/2
			157.65 ± 0.04	157.624	4s²4p²(³P)5s ²P_3/2 →4s²4p³ ²D°_5/2
			159.07 ± 0.04	159.049	4s²4p²(³P)5s ⁴P_5/2 →4s²4p³ ²D°_5/2
			159.42 ± 0.04	159.219	4s²4p²(³P)5s ⁴P_3/2 →4s²4p³ ²D°_3/2
			231.07 ± 0.04	231.110	4s²4p²(¹D)4d ²F_7/2 →4s²4p³ ²D°_5/2
			239.03 ± 0.06	239.017	4s²4p²(¹S)4d ²D_5/2 →4s²4p³ ²P°_3/2
			243.05 ± 0.06	243.071	4s²4p²(¹D)4d ²D_3/2→4s²4p³ ²D°_5/2
Mo XI	Mo¹⁰⁺	209.3	146.65 ± 0.04	146.641	4s²4p (²P°_1/2)5s (1/2, 1/2)°₁→4s²4p² ³P₂
Mo XI	Mo¹⁰⁺	209.3	322.12 ± 0.04	322.158	4s4p³ ¹P°₁ → 4s²4p² ¹D₂
Mo XII	Mo¹¹⁺	230.28	131.37 ± 0.03	131.394	4s²5s ²S_1/2→4s²4p ²P°_1/2
			250.09 ± 0.06	250.112	4s²4d ²D_5/2→4s²4p ²P°_3/2
			329.53 ± 0.01	329.414	4s4p² ²P_3/2→4s²4p ²P°_3/2
			336.51 ± 0.01	336.639	4s4p² ²P_1/2→4s²4p ²P°_3/2
			381.13 ± 0.06	381.125	4s4p² ²D_3/2→4s²4p ²P°_1/2
Mo XIII	Mo¹²⁺	279.1	53.56 ± 0.02	53.551	3d⁹4s²4p ³D°₁→3d¹⁰4s² ¹S₀
			54.12 ± 0.02	54.101	3d⁹4s²4p ¹P°₁→3d¹⁰4s² ¹S₀
			340.88 ± 0.01	340.909	3d¹⁰4s4p ¹P°₁→3d¹⁰4s² ¹S₀
			352.87 ± 0.03	352.994	3d¹⁰4p² ³P₁→3d¹⁰4s4p ³P°₀
Mo XIV	Mo¹³⁺	302.6	51.98 ± 0.02	52.000	3d⁹(²D)4p²(³P) ²P_1/2→3d¹⁰4p ²P°_3/2
			52.77 ± 0.02	52.753	3d⁹(²D)4s4p (³P°) ²P°_3/2→3d¹⁰4s ²S_1/2
			121.68 ± 0.02	121.647	3d¹⁰5s ²S_1/2→3d¹⁰4p ²P°_3/2
			241.78 ± 0.06	241.609	3d¹⁰4d ²D_3/2→3d¹⁰4p ²P°_1/2
			373.55 ± 0.05	373.647	3d¹⁰4p ²P°_3/2→3d¹⁰4s ²S_1/2
			423.57 ± 0.07	423.576	3d¹⁰4p ²P°_1/2→3d¹⁰4s ²S_1/2
Mo XV	Mo¹⁴⁺	544	29.48 ± 0.01	29.458	3d⁹5f ¹P°₁→3d^{10 1}S₀
			29.81 ± 0.01	29.774	3d⁹5f ³D°₁→3d^{10 1}S₀
			35.39 ± 0.01	35.368	3d⁹4f ¹P°₁→3d^{10 1}S₀
			50.43 ± 0.02	50.448	3d⁹(²D_5/2)4p (5/2, 3/2)°₁→3d¹⁰ ¹S₀
			58.04 ± 0.04	57.927	3d⁹(²D_3/2)4s (3/2, 1/2)₂→3d¹⁰ ¹S₀
			58.86 ± 0.04	58.832	3d⁹(²D_5/2)4s (5/2, 1/2)₂→3d¹⁰ ¹S₀
			347.47 ± 0.05	347.339	3d⁹(²D_5/2)4p (5/2, 3/2)°₃→3d⁹(²D_5/2)4s (5/2, 1/2)₃
			365.77 ± 0.04	365.924	3d⁹(²D_5/2)4p (5/2, 3/2)₄→3d⁹(²D_5/2)4s (5/2, 1/2)₃
Mo XVI	Mo¹⁵⁺	591	32.92 ± 0.05	32.916	3p⁶3d⁸(¹G₄)4f ²[1]°_3/2→3p⁶3d⁹ ²D_5/2
			34.03 ± 0.01	33.992	3p⁶3d⁸(³F₂)4f ²[1]°_3/2→3p⁶3d⁹ ²D_3/2
			54.46 ± 0.03	54.348	3p⁶3d⁸(³F₄)4s (4, 1/2) _9/2→3p⁶3d⁹ ²D_5/2
Mo XVIII	Mo¹⁷⁺	702	38.81 ± 0.01	38.700^a	3d⁶4p→3d⁷
^a 数据来源于文献[18], 其他数据来源于NIST数据库^[25], 粗体表示可用于杂质诊断的谱线.

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[1]	Wan B N, Gong X Z, Liang Y, et al. 2022 Nucl. Fusion 62 042010 Google Scholar
[2]	Gao X, Zeng L, Wu M Q, Zhang T, Yang Y, Ming T F, Zhu X, Wang Y M, Liu H Q, Zang Q, Li G Q, Huang J, Gong X Z, Li Y Y, Li J G, Wan Y X 2020 Nucl. Fusion 60 102001 Google Scholar
[3]	Zhang L, Morita S, Xu Z, et al. 2017 Nucl. Mater. Energy 12 774 Google Scholar
[4]	李加宏, 胡建生, 王小明, 余耀伟, 吴金华, 陈跃, 王厚银 2012 物理学报 61 205203 Google Scholar Li J H, Hu J S, Wang X M, Yu Y W, Wu J H, Chen Y, Wang H Y 2012 Acta Phys. Sin. 61 205203 Google Scholar
[5]	Gong X Z, Garofalo A M, Huang J, et al. 2019 Nucl. Fusion 59 086030 Google Scholar
[6]	张凌, 吴振伟, 高伟, 黄娟, 陈颖杰, 高伟, 胡立群 2013 原子与分子物理学报 30 779 Google Scholar Zhang L, Wu Z W, Gao W, Huang J, Chen Y J, Gao W, Hu L Q 2013 J. At. Mol. Phys. 30 779 Google Scholar
[7]	Asmussen K, Fournier K B, Laming J M, Neu R, Seely J F, Dux R, Engelhardt W, Fuchs J C 1998 Nucl. Fusion 38 967 Google Scholar
[8]	Chowdhuri M B, Morita S, Goto M, Nishimura H, Nagai K, Fujioka S 2007 Rev. Sci. Instrum. 78 023501 Google Scholar
[9]	Huang X L, Morita S, Oishi T, Goto M, Dong C F 2014 Rev. Sci. Instrum. 85 043511 Google Scholar
[10]	Beiersdorfer P, Magee E W, Träbert E, Chen H, Lepson J K, Gu M F, Schmidt M 2004 Rev. Sci. Instrum. 75 3723 Google Scholar
[11]	Lepson J K, Beiersdorfer P, Clementson J, Gu M F, Bitter M, Roquemore L, Kaita R, Cox P G, Safronova A S 2010 J. Phys. B:At. Mol. Opt. Phys. 43 144018 Google Scholar
[12]	Cui Z Y, Morita S, Zhou H Y, et al. 2013 Nucl. Fusion 53 093001 Google Scholar
[13]	Zhang L, Morita S, Xu Z, et al. 2015 Rev. Sci. Instrum. 86 123509 Google Scholar
[14]	Xu Z, Zhang L, Cheng Y X, et al. 2021 Nucl. Instrum. Methods Phys. Res. A 1010 165545 Google Scholar
[15]	Li L, Zhang L, Xu Z, et al. 2021 Plasma Sci. Technol. 23 075102 Google Scholar
[16]	Chowdhuri M B, Morita S, Goto M, Nishimura H, Nagai K, Fujioka S 2007 Plasma Fusion Res. 2 S1060 Google Scholar
[17]	Liu Y, Morita S, Oishi T, Goto M, Huang X L 2018 Plasma Fusion Res. 13 3402020 Google Scholar
[18]	Schwob J L, Klapisch M, Schweitzer N, Finkenthal M, Breton C, Michelis C D, Mattioli M 1977 Phys. Lett. A 62 85 Google Scholar
[19]	Jupén C, Denne-Hinnov B, Martinson I, Curtis L J 2003 Phys. Scr. 68 230 Google Scholar
[20]	杨友磊, 胡叶民, 项农 2017 物理学报 24 245202 Google Scholar Yang Y L, Hu Y M, Xiang N 2017 Acta Phys. Sin. 24 245202 Google Scholar
[21]	洪斌斌, 陈少永, 唐昌建, 张新军, 胡有俊 2012 物理学报 61 115207 Google Scholar Hong B B, Chen S Y, Tang C J, Zhang X J, Hu Y J 2012 Acta Phys. Sin. 61 115207 Google Scholar
[22]	Wan B N, Li J G, Guo H Y, Liang Y F, Xu G S, Wang L, Gong X Z 2015 Nucl. Fusion 55 104015 Google Scholar
[23]	姚黎明, 张凌, 许棕, 杨秀达, 吴承瑞, 张睿瑞, 杨飞, 吴振伟, 姚建铭, 龚先祖, 胡立群 2019 光谱学与光谱分析 39 2645 Google Scholar Yao L M, Zhang L, Xu Z, Yang X D, Wu C R, Zhang R R, Yang F, Wu Z W, Yao J M, Gong X Z, Hu L Q 2019 Spectrosc. Spect. Anal. 39 2645 Google Scholar
[24]	杨秀达, 张凌, 许棕, 张鹏飞, 陈颖杰, 黄娟, 吴振伟, 龚先祖, 胡立群 2018 光谱学与光谱分析 38 1262 Google Scholar Yang X D, Zhang L, Xu Z, Zhang P F, Chen Y J, Huang J, Wu Z W, Gong X Z, Hu L Q 2018 Spectrosc. Spect. Anal. 38 1262 Google Scholar
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