| PHYSICS OF GASES, PLASMAS, AND ELECTRIC DISCHARGES |
|
|
|
|
Emission Lines of Boron, Carbon, Oxygen and Iron in Tokamak Plasma |
| DI Long1, SHI Jian-Rong1, WANG Shou-Jun2, DONG Quan-Li2, ZHAO Jing2, LI Yu-Tong2, FU Jia3, WANG Fu-Di3, SHI Yue-Jiang3, WAN Bao-Nian3, ZHAO Gang1**, ZHANG Jie2,4
|
1Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012
2Laboratory of Optical Physics, Beijing National Laboratory for Condensed Matter Physics, Institute of Physics, Chinese Academy of Sciences, Beijing 100190
3Institute of Plasma Physics, Chinese Academy of Sciences, Hefei 230031
4Department of Physics, Shanghai Jiao Tong University, Shanghai 200240
|
|
| Cite this article: |
|
DI Long, SHI Jian-Rong, WANG Shou-Jun et al 2011 Chin. Phys. Lett. 28 075201 |
|
|
|
|
Abstract The emission lines of B, C, O and Fe in tokamak plasma are reported. The spectra are compared with those calculated by the CHIANTI code, which is based on the collisional-radiative models with a large amount of accurate atomic data. General agreement is obtained between the results of experiment and computation. Most of the lines in the spectra are identified, and the relative number density ratios of B, C, O and Fe are determined. It is found that the processes of line formation in our experiment are similar to those in the stellar coronae. The line-averaged electron density of the tokamak plasma is measured by the HCN laser, indicating a good agreement with the theoretical prediction by the density-dependent line ratio of Fe XXI.
|
| Keywords:
52.55.Fa
07.85.Nc
95.30.Ky
|
|
|
Received: 01 March 2011
Published: 29 June 2011
|
|
| PACS: |
52.55.Fa
|
(Tokamaks, spherical tokamaks)
|
| |
07.85.Nc
|
(X-ray and γ-ray spectrometers)
|
| |
95.30.Ky
|
(Atomic and molecular data, spectra, and spectralparameters (opacities, rotation constants, line identification, oscillator strengths, gf values, transition probabilities, etc.))
|
|
|
|
|
|
[1] Fournier K B et al 2001 the Astrophys. J. 561 1144
[2] Finkenthal M, Yu T L, Lippmann S, Huang L K, Moos H W, Stratton B C and Bhatia A K 1987 Astrophys. J. 313 920
[3] Wei H G, Shi J R, Zhao G et al 2008 Astrophys. J. 683 577
[4] Liang G Y, Zhao G, Zeng J L and Shi J R 2004 Mon. Not. R. Astron. Soc. 350 298
[5] Huang J, Wan B N, Gong X Z, Wu Z W, Lin H, Zhou Q, and The HT-7 Team 2006 Plasma Phys. Control. Fusion 48 1709
[6] Ding B J, Kuang G L, Shan J F, Xu G S, Wan B N, Li J G, and HT-7 team 2003 Nucl. Fusion 43 558
[7] Gu M F 2003 the Astrophys. J. 582 1241
[8] Landi E, Del Zanna G, Young P R, Dere K P, Mason H E and Landini M 2006 Astrophys. J. Suppl. 162 261
[9] Dere K P, Landi E, Mason H E, Monsignori-Fossi B C and Young P R 1997 Astron. Astrophys. Suppl. 125 149
[10] Young P R, Watanabe T, Hara H and Mariska J T 2008 Astron. Astrophys. (submitted) arXiv:0805.0958
[11] Mazzotta P, Mazzitelli G, Colafrancesco S and Vittorio N 1998 Astron. Astrophys. Suppl. 133 403
[12] Maggio A, Drake J J, Kashyap V, Harnden F R, Micela G et al 2004 Astrophys. J. 613 548
[13] Sanz-Forcada J and Micela G 2002 Astron. Astrophys. 394 653
[14] Brickhouse N S, Dupree A K, Edgar R J, Liedahl D A, Drake S A et al 2000 Astrophys. J. 530 387
[15] Ness J U, Gudel M, Schmitt J H M M, Audard M and Telleschi A 2004 Astron. Astrophys. 427 667
[16] Maggio A and Ness J U 2005 Astrophys. J. 622 L57
[17] Feldman U, Curdt W, Landi E and Wilhelm K 2000 Astrophys. J. 544 508
[18] Shirai T, Sugar J, Musgrove A and Wiese W L 2000 J. Phys. Chem. Ref. Data Monograph No 8
|
|
Viewed |
|
|
|
Full text
|
|
|
|
|
Abstract
|
|
|
|
|
