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Co-ordinated Research Program on “Atomic Data for Heavy Element Impurities in Fusion Reactors”, 4-6 March 2009, IAEA headquarters, Vienne Plasma Diagnostics by spectra from LHD and Atomic Data.

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  1. Co-ordinated Research Program on “Atomic Data for Heavy Element Impurities in Fusion Reactors”, 4-6 March 2009, IAEA headquarters, ViennePlasma Diagnostics by spectra from LHD and Atomic Data T. Kato, N. Yamamoto1, G. O’Sullivan2, I. Murakami, D. Kato and H. Funaba, K. Sato, M. Goto, B. Peterson, National Institute for Fusion Science, Toki, Gifu 509-5292, Japan • Institute of Laser Engineering, Osaka University, Suita, Osaka 565-0871, Japan • University College Dublin, Dublin, Ireland

  2. Outline • We have observed EUV spectra from the Large Helical Device (LHD) at the National Institute for Fusion Science (NIFS). • We analyzed the spectra of impurity ions; carbon, iron, xenon, tin and tungsten ions. • C and Fe spectra; we studied plasma diagnostics by intensity ratios of spectral lines. • For higher Z element, Xe, Sn and W; we studied mainly line identifications comparing with theoretical calculations. • Related atomic data for these spectra will be discussed. • Working group in NIFS updated the data for high Z elements for the NIFS database.

  3. 1. Carbon EUV Spectra from LHD • We try to make a quantitative study of radiation collapse using spectroscopic measurement of carbon ion lines of C III, C IV and C V from LHD plasmas. • The line intensity ratios for one ion depend on the electron density and electron temperature. • We studied the time dependent intensity ratios of spectral lines from C V and C III using the collisional radiative model of carbon ions. • We find that the intensity ratios of C V are affected by recombination at the end of plasma before radiation collapse. • Intensity ratios for non-radiation collapse are always ionizing spectra even during the plasma decays. • We will make a time dependent model for carbon ions.

  4. Shot Summary for #55644 (Radiation Collapse) Heating continues Plasma energy drops Ne rises Te drops Radiation increases Gas puff causes collapse

  5. C V 227.18A 1s2s 3S- 1s3p 3P C V 248.6 1s2p 3P- 1s3d 3D C IV 312.4A 2s - 3p C IV 289.22 2p - 4d C III 977.02 A 2s2 1S – 2s2p 1P CIII 1175.5 2s2p 3P – 2p23P HI 1024A (Lya) HI 1215.7A (Lyb) We measured EUV spectra from Carbon ions (SOXMOS)Spectra in two wavelength ranges before collapse at 0.9 sec 200 - 346A 953 - 1232A

  6. Spectra at 1.1 sec (during/after radiation collapse, low Te) 200 - 346A CIV(2s-3p), CIII (2s2 - 2s2p) line intensities increase more than CV lines 953 - 1232A

  7. Time history of line intensities #55644 Line intensities begin to increase at 0.94 s. Radiation power seen by bolometer increases about 7 times. Main part of the radiation might be CV or CIV because intensity time history looks like that of bolometric measurement.

  8. Electron temperature profilemeasured by K. Narihara Electron density profilemeasured by K. Tanaka Ne rises Te falls Row is the scaled radius (row = 1 is the last closed magnetic surface)

  9. Bolometer emissivity profilemeasured by B. Peterson The peak position of the radiation power is near the edge at row = 0.9 Row is the scaled radius (row = 1 is the last closed magnetic surface)

  10. Intensity ratios for CV and CIII lines Intensity ratios begins to increase at 0.94secEvidence for Recombination Big change CIII I(2s2p 3P - 2p23P)/I(2s2 1S - 2s2p1P) CV I(1s2p - 1s3d)/I(1s2s - 1s3p)

  11. 1s 1s3s 1s3d 1s3p 1s2s 1s2p 1s2 Temperature dependence of Intensities of CV linesfor different plasma conditionsCalculated by Collisional Radiative Model Excitation Data Suno &Kato(2006) Itikawa (1985)

  12. Density dependence of the intensity ratioIntensity ratios are constant for Ne = 1010 - 10 14 cm-3

  13. Temperature dependence of Intensity ratios of CV linesMeasured Intensity ratios are plotted. A recombination process is necessary to explain the observed intensity ratios.

  14. Calculated time dependent CV radiationpower Ionizing component is larger than recombining component even during recombination phase for total radiation power of CV

  15. Shot summary for Non radiation collapse (#55642 ) We measured the carbon ion spectra for a shot without radiation collapse to compare the spectra with radiation collapse. Plasma decays gradually after NBI heating ends.

  16. Te and Ne for #55642 Te decreases with time. Ne increases with time. Plasma shrinks.

  17. Comparison of spectra with non radiation collapse Time history of line intensities #55642

  18. Intensity ratio of CV and CIII lines Non radiation collapse case (#55642 )very different with those during radiation collapse NBI off Intensity ratio of C V decreases and indicates Ionizing even after NBI heating off Intensity ratio of C III increases

  19. Summary and Discussion for carbon lines • We measured time dependent spectra from carbon ions for a shot with radiation collapse • Main part of the radiation loss is probably CIV and CV line emission from the time history of line intensities • Intensity ratios of CV and CIII indicate an increase of the recombining component after 0.94 s. • We could explain the increase in time for CV radiation by recombination processes qualitatively • We found the intensity ratios of CV indicate ionizing plasma even after NBI ends for non radiation collapse case. This might indicate the C4+ ions move towards the center after NBI ends. We will study this phenomena using other lines of CV. • We will study the behavior of CIV and CIII lines. • Is it possible to explain the time dependence of bolometric measurement by carbon line emissions? • Why does the electron temperature decrease because of radiation after 1.0s?

  20. Problem of atomic data for C4+ ions • Observed Intensity Ratios I (1s2p 3P - 1s3s 3D)/ I(1s2s 3S - 1s3p 3P) are smaller than theoretical values Excitation rate coefficients and radiative transition probabilities are important We need more accurate data even for C4+ (He-like) ions 2 1S - 2 3P, 2 3S - 2 1P, 2 3P - 3 3S 1 1S - 3 1S, 3 3S

  21. 2. Fe EUV Spectra from LHDN. Yamamoto, T. Watanabe, T. Kato • Fe is an intrinsic impurity in Laboratory Plasmas • Important also in Astrophysics and the Sun • We studied EUV Fe spectra from LHD and EIS (EUV Imaging Spectrometer) on board the Hinode satellite for plasma diagnostics • We evaluate Atomic Data for Fe ions: Ionization, Excitation, Wavelength, Transition probabilities.

  22. Slot Observation / EISHinode satellite Slit observation (full CCD) active region FeXV FeXIV SiVII 4-5 November 2006

  23. Solar EUV Spectra by EIS Spectral lines of EIS/HINODE were identified by using NIST / CHIANTI wavelength database.

  24. Spectra of LHD with TESPELFe Pellet was injected into plasma FeIX FeX FeXI FeXII FeVIII FeXIII

  25. (5) (1) Ip=361eV (4) (3) (7) (6) (2) 3P 3F 1P 1F 3S 3D 1S 5S 1D 3s23p3d (2,3) (6) (1) 3s3p3 (4,7) (5) 3s23p2 Energy levels for Fe XIII lines #66810-4.3s@LHD 3p-3d transition (3s23p2-3s23p3d) （1） 196.525A: 1D2-1F3 (with FeXII) （2） 200.021A: 3P1-3D2 （3） 201.121A: 3P1-3D1 (with FeXII) （4） 202.044A: 3P0-3P1 （5） 203.793A+203.826A: 3P2-3D2,3D3 （6） 208.679A: 1S0-1P1 （7） 209.617A: 3P1-3P2

  26. Density Diagnostics Collisional excitation between ground states (E = 0 eV) and excited states (E < 10 eV) with same configurations is important. For example, Fe XIII (Si-like) Low density, Ne < 108 cm-3 High density, Ne > 1012 cm-3 3s23p3d 3D3 3s23p3d 3P1 Density increase I2, Strong intensity Radiative Transition I1, Strong intensity I2, Weak intensity Collisional excitation I1 , Strong intensity 3s23p23P2 3s23p23P2 3s23p23P0 3s23p23P0 I1 >> I2 I1 ~ I2

  27. FeXIII Line Spectra are calculated with three different Atomic Data by our CRM (N. Yamamoto) DARC(AK2005) CHIANTI Difference of A-values also makes large difference AK: Aggarwal and Keenen(2005) CHIANTI: Gupta and Tayal(2000) Hullac: DW

  28. Density Dependent line ratios, Fe XIII ___ Aggarwal & Keenen (2005) Data …...… CHIANTI Gupta & Tayal (1998) Data

  29. LHD and Quiet region/EIS@HINODE Spectral structures of LHD (blue) and Q-EIS (red) are quite different. The electron density in quiet regions is lower than in LHD plasmas. Density effect on the lines of 202.0A and 203.8A is clearly seen.

  30. Wavelengths of NIST data（N) and CHIANTI（C) data are different for Line identification α N FeXI C α β γ N FeXII C γ β δ N FeXIII C δ

  31. Wavelengths forFe XIII Line Intensity Ratios • In order to obtain the correct observed line intensity it is necessary to know the intensities of the blended lines. • 203.8A/202.0A: Often used for density diagnostics • Many lines from FeXI-XIII are observed around 203A. The wavelengths from NIST and CHIANTI database are different. NISTCHIANTI α: FeXIII, 202.4A → 203.2A (3s23p2 3P1-3s23p3d 3P0) β: FeXII, 203.3A → 203.7A (3s23p3 2D5/2-3s23p(1S)3d 2D5/2) γ: FeXII, 202.1A → 201.7A (3s23p3 2P1/2-3s23p2(1D)3d 2P1/2) δ: FeXI, 201.7A → 203.3A (3s23p4 1D2-3s23p3(2D)3d 1P1)

  32. Observed FeXIII Line Intensity Ratios 活動領域 静穏領域 LHD&EBIT are close to calculations by AK and CHIANTI Active@Sun Ne=2-10x109cm-3、Quiet@SunNe=3-30x108cm-3。

  33. Summary for Fe spectral diagnostics Proton excitation between the fine structure levels is important as well electron excitation Wavelength and Transition probability are also important for line intensities Eg. For 204.26 A, A- values by AK(1.540x109) and CHIANTI (2.015x1010) makes the intensity quite different. Watanabe et al(2009)

  34. We are working on Data evaluation for Fe ions Comparison of effective collision strengths Fe XI 3s23p43P2 – 3s23p3(2D)3d 1F3 and 1D2 • Proton impact excitation FeX - XV(NIFS-DATA), FeXVII - FeXXIII(NIFS-DATA) • Electron impact excitation FeX - Fe XIII (Skobelev, NIFS-DATA-104,2009) M-sell, L-shell data will be evaluated (I. Murakami) • Ionization and recombination (I. Murakami and D. Kato) solid lines: Aggarwal and Keenan (2003)  : Gupta and Tayal (1999)

  35. 3. Spectra from High Z elements G. O’Sullivan, C. Suzuki, H. Tanuma, T. Kato • We have measured W, Sn, Xe spectra from LHD plasmas • Xe and Sn ion spectra are measured by Charge exchange with He and Xe atoms in Metropolitan University (H. Tanuma). Spectra from specific ion can be measured Snq+ + He --> Sn (q-1)+ + He+

  36. W spectra near 5nm from LHD (NIFS) Lower Te Higher Te Te(0) = 3 keV

  37. Cowan Code Calculations 4p64dn- 4p64dn-14f + 4p54dn+1transitions G. O’Sullivan 4d10 4d5 Fk, Gk and Rk parameters reduced to 80%. Spin Orbit parameter unchanged 4d9 4d4 4d8 4d3 4d2 4d6 4d

  38. UTA statistics for W XXIX – W XXXVIII Putterich et al Plasma Phys. Control. Fusion 50 085016 2008 Mean of UTA matches ADAS data very well Widths = standard deviation Mean of UTA matches ADAS data very well Widths = standard deviation

  39. Cowan Code CalculationsFor W XVI – W XXVIII transitions based on the open 4f subshell 4d104fn -4d104fn-15d 4d104fn -4d94fn+1 n = 2 n = 1 n = 3 n = 4 n = 6 n = 7 n = 5

  40. Comparisons Sugar, Kaufman (1980)

  41. Radke (2001) 4p-4d gives two groups of lines near 4.7 and 6.5 nm

  42. Tentative Conclusions for W spectra WXXXIX-WXLV 4p1/2-4d3/2 WXXII - WXXVII 4f-5d WXXXIX-WXLV 4p3/2-4d5/2 WXXIX- WXXXVIII 4p64dn-4p54dn+1 + 4dn-14f WXXII-WXXVII 4d-4f

  43. Going Forward Repeat Cowan code calculations with different % scaling of Slater Condon parameters to optimise agreement with experiment. Give lines an instrumental width to get ‘spectrum’ for each stage. Add stages to reproduce UTA shape. Perform calculations for 4p excitation. Expect contributions near 4.5 and 6 nm Calculate 4f -5d transitions in W21+ - W26+

  44. W ion spectra in JT-60U plasma Yanagibayashi • Lines with 3p-3d transitions of Wq+ (q >= 47) around 2.8 nm appeared with increasing Te up to 8 keV. These lines are believed to be useful for W accumulation diagnosis in ITER high temperature plasmas (Te > 10 keV). 3p-3d transitions 4s-4p, 4p-4d transitions

  45. EUV Spectra of Sn recorded at NIFS A. Sasaki et al Review of Laser Engineering Suppl. 1132 (2008) NIFS LHD Spectrum of Sn dominated by an unresolved transition array (UTA) near 13.5 nm (C. Suzuki et al. 2008, J. Phys. Conf. Ser.)

  46. Analysis of the UTA Churilov and Ryabtsev Phys. Scr. 73 614-619, 2006   Spectra due to 4p64dn-4p64dn-14f + 4p54dn+1 transitions Configuration Interaction very important

  47. Charge Exchange Spectra of SnXV - SnXVIII

  48. Resonance 4p-4d Transitions in Sn XVIII – Sn XX Cowan Code Calculations Fk, Gk and Rk parameters reduced to 85%. Spin Orbit parameter unchanged Resonance transitions cannot explain observed spectrum.

  49. Origin of CXS spectral features Cannot be due to resonance transitions to ground state. Cannot arise from lower stages Can only arise from 4-4 transitions Must be due to transitions between excited states fed by cascades.

  50. Configuration Interaction effects in Sn XVII (example) Strong final state CI for transitions of the type: 4s24p34d – 4s24p34f + 4s24p24d2 + 4s4p44d (between excited states)

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