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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. - PowerPoint PPT PresentationTRANSCRIPT
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
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 (1) Institute of Laser Engineering, Osaka University, Suita,
Osaka 565-0871, Japan(2) University College Dublin, Dublin, Ireland
Outline• We have observed EUV spectra from the Large Helical Dev
ice (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 elemen
ts for the NIFS database.
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.
Shot Summary for #55644 (Radiation Collapse)
Heating continues
Plasma energy drops
Ne rises
Te drops
Radiation increases
Gas puff causes collapse
We measured EUV spectra from Carbon ions (SOXMOS)
Spectra in two wavelength ranges before collapse at 0.9 sec
C V 227.18A1s2s 3S- 1s3p 3PC V 248.6 1s2p 3P- 1s3d 3DC 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 – 2p2 3PHI 1024A (Ly)HI 1215.7A (Ly)
1000
800
600
400
200
0
Intensity (a.u.)
10008006004002000
Channel Number
45 (0.9sec)
CV 227.18CV 248.6
CIV 289.22
CIV 312.4
2000
1500
1000
500
0
Intensity (a.u.)
20001800160014001200
Channel Number
45
CIII 977
HI 1024
OVI 1037.6, CII 1036, 1037
CIII 1175.5HI 1215.7
OVI 1031.9
200 - 346A
953 - 1232A
Spectra at 1.1 sec (during/after radiation collapse, low Te)
CIV(2s-3p), CIII (2s2 - 2s2p) line intensities increase more than CV lines
4000
3000
2000
1000
0
Intensity (a.u.)
10008006004002000
Channel Number
55 (1.1 sec)
CV CV CIV
CIV
40x103
30
20
10
0
Intensity (a.u.)
20001800160014001200
Channel Number
55 (1.1 sec)
CIII
CIII
200 - 346A
953 - 1232A
Time history of line intensities #55644
101
102
103
104
Line Intensity (a.u.)
1.41.21.00.80.60.40.2
Time (s)
0.01
0.1
1
10
Ne (10^19m-3)
1
10
100
1000
Prad (KW)
CV 227.2A(2s 3S- 3p 3P) CV 248.6A (2p 3P - 3d 3D) CIV 312.4A (2s - 3p) CIII 977.0A (2s2 1S - 2s2p 1P) Ne Prad Lya
CIII
Ne
CIV
CV
#55644
Prad
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.
Electron temperature profilemeasured by K. Narihara
3000
2500
2000
1500
1000
500
0
Electron Temperature (eV)
-1.0 -0.5 0.0 0.5 1.0
row
#55644 900ms 940ms 960ms 1000ms 1060ms 1100ms 1140ms
Te falls
14
12
10
8
6
4
2
0
Electron density (10^19 m-3)
1.21.00.80.60.40.20.0
rou (r/a)
600ms 800ms 940ms 960ms 980ms 1000ms 1020ms 1040ms
Ne rises
Electron density profilemeasured by K. Tanaka
Row is the scaled radius (row = 1 is the last closed magnetic surface)
Bolometer emissivity profilemeasured by B. Peterson
10
2
3
4
5
6
78
100
2
3
4
5
6
78
1000
Bolometric emissivity (KW/M3)
1.00.80.60.40.20.0
row
0.50 sec 0.9 0.940.98 1.00 1.051.081.09 1.10 1.13 1.14 1.15 1.18 1.30
#55644Bolometer
0.5s
0.9s0.94s
1.0s
1.05s
1.08s
1.09s
1.13s
1.10s
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)
Intensity ratios for CV and CIII lines Intensity ratios begins to increase at 0.94sec
Evidence for Recombination
101
2
4
6810
2
2
4
6
8103
2
4
6810
4
Intensity
1.41.21.00.80.60.40.20.0
Time (s)
2.0
1.5
1.0
0.5
0.0
Intensity ratio
227 (2s-3p) 248 (2p - 3d) Ratio248_227
CV
#55644
100
101
102
103
104
Intensity (a.u.)
1.41.21.00.80.60.40.2
Time (s)
0.4
0.3
0.2
0.1
0.0
Intensity ratio
977(CIII)' '1175(CIII)' Ratio1175_977b
(x1.4 sensitivity correction Å@x1.4 line width correction )
CV I(1s2p - 1s3d)/I(1s2s - 1s3p)
CIII I(2s2p 3P - 2p2 3P)/I(2s2 1S - 2s2p1P)
Big change
Temperature dependence of Intensities of CV linesfor different plasma conditions
Calculated by Collisional Radiative Model
10-15
10-14
10-13
10-12
10-11
10-10
Intensity (cm3 s-1)
102 3 4 5 6 7 8 9
1002 3 4 5 6 7 8 9
Te (eV)
Ne = 10^13 cm-3 I(2p -3d) I(2s -3p) R(2p -3d) R(2s -3p) E(2p -3d) E (2s -3p)
with recommended data
ionizing
equilibrium
recombining
1s2
1s2s 1s2p
1s3s 1s3p 1s3d
1s
Excitation DataSuno &Kato(2006)Itikawa (1985)
Density dependence of the intensity ratioIntensity ratios are constant for Ne = 1010 - 10 14 cm-3
2
3
4
5
6
7
8
9
1
2
3
4
5
6
Intensity ratio (3d /3p)
107
108
109
1010
1011
1012
1013
1014
1015
1016
1017
1018
Electron density (cm-3)
Ionizing Te = 10eV Te = 100eV Te = 1000 eV
Recombining Te = 10eV Te = 100eV Te = 1000 eV
Intensity Ratio I(2p - 3d)/I(2s-3p)
Temperature dependence of Intensity ratios of CV linesMeasured Intensity ratios are plotted. A recombination process is necessary to explain the observed intensity ratios.
3.0
2.5
2.0
1.5
1.0
0.5
0.0
Intensity Ratio
102 3 4 5 6 7 8 9
1002 3 4 5
Te (eV)
Measured Equilibrium Ne = 10^13 cm-3 Ionizing Recombining CVI/CV = 4
with recommended atomic data
Intensity Ratio I(2p - 3d)/I(2s-3p)
IonizingEquilibrium
Recombining
0.94 s
1.0
1.04
1.06
1.08s
Calculated time dependent CV radiation power
10-30
10-29
10-28
10-27
10-26
10-25
Rad. Loss (W/el/ion)
102 3 4 5 6 7 8 9
1002 3 4 5 6 7 8 9
10002 3 4
Te (eV)
CV Radiation loss (ne = 10^13 cm-3)
Ionizing recombining
3
4
5
67
10-30
2
3
4
5
67
10-29
2
3
Radiation of CV (W/el/ion)
1.051.000.950.90
Time (s)
Radiation of CV /el/ion Ionizing component Recombining component
Ionizing component is larger than recombining component even during recombination phase for total radiation power of CV
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.
Te and Ne for #55642
1400
1200
1000
800
600
400
200
0
Te (eV)
4500400035003000
Radius (mm)
TS_Te_2000 TS_Te_3220 TS_Te_3480 TS_Te_3603 TS_Te_3669
1400
1200
1000
800
600
400
200
0
Ne (a.u.)
4500400035003000
Radius (mm)
TS_Ne_2000 TS_Ne_3200 TS_Ne_3480 TS_Ne_3603 TS_Ne_3669
Te decreases with time.
Ne increases with time.Plasma shrinks.
Comparison of spectra with non radiation collapse Time history of line intensities #55642
100
101
102
103
104
Intensity (a.u.)
4.03.53.02.52.0
Time (s)
1
10
100
1000
Bolometer
0.01
0.1
1
10
100
Ne
CV227 CV248 CIV312 CIII977 H Lya1215 Prad_KW 'Ne-av'(m-3) H Lyb1024
CIII
CIV
CV HLya
Ne
HLyb
Intensity ratio of CV and CIII lines Non radiation collapse case (#55642 )very different with those during radiation collapse
0.20
0.15
0.10
0.05
0.00
Intensity ratio (CIII 1175/977)
3.63.43.23.02.82.62.42.22.0
time (s)
10-1
100
101
102
103
104
Ratio_CIII CIII 977 CIII 1175
#55642
Intensity ratio of C V decreases and indicates Ionizing even after NBI
heating off
Intensity ratio of C III increases
2.0
1.5
1.0
0.5
0.0
Intensity ratio (CV 248 2p - 3d /227 2s - 3p)
3.63.43.23.02.82.62.42.22.0
Time (s)
10
2
3
4
5
6
789100
2
3
4
5
6
7891000
Intensity (a.u.)
CV Intensity ratio (248/227) 227 (2s - 3p) 248 (2p - 3d)
NBI off
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?
Problem of atomic data for C4+ ions
• Observed Intensity Ratios I (1s2p 3P - 1s3s 3D)/ I(1s2s 3S - 1s3p 3P) are smaller than theoretical valuesExcitation rate coefficients and radiative transition pr
obabilities are importantWe need more accurate data even for C4+ (He-like) io
ns 2 1S - 2 3P, 2 3S - 2 1P, 2 3P - 3 3S 1 1S - 3 1S, 3 3S
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 p
robabilities.
Slot Observation / EISHinode satellite
FeXV
FeXIVSiVII 4-5 November 2006
Slit observation (full CCD) active region
Solar EUV Spectra by EISSpectral lines of EIS/HINODE were identified by using NIST / CHIANTI wavelength database.
Spectra of LHD with TESPELFe Pellet was injected into plasma
FeVIII
FeIX FeX FeXIFeXII
FeXIII
Energy levels for Fe XIII lines
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
(1)
(2)(3)(4)
(6)
(5)
(7)
#66810-4.3s@LHD1S 1P 1D 1F 3S 3P 3D 3F 5S
(1)
(2,3
)
(4,7
)
(5)
(6)
3s23p2
3s3p3
3s23p3d
Ip=361eV
Density Diagnostics
For example, Fe XIII (Si-like)
Low density, Ne < 108 cm-3
High density, Ne > 1012 cm-3
3s23p2 3P0
3s23p2 3P2
Density increase
3s23p3d 3P1
3s23p3d 3D3
I 2, W
eak
inte
nsit
y
I 2, St
rong
inte
nsit
y
Rad
iati
ve T
rans
itio
nI 1,
Stro
ng in
tens
ity
Col
lisio
nal e
xcita
tion
Collisional excitation between ground states (E = 0 eV) and excited states (E < 10 eV) with same configurations is important.
I 1 , S
tron
g in
tens
ity
I1 >> I2 I1 ~ I2 3s23p2 3P0
3s23p2 3P2
FeXIII Line Spectra are calculated with three different Atomic Data by our CRM (N. Yamamoto)
DARC(AK2005)
CHIANTI
AK: Aggarwal and Keenen(2005)CHIANTI: Gupta and Tayal(2000)Hullac: DW
Difference of A-values also makes large difference
Density Dependent line ratios, Fe XIII
___ Aggarwal & Keenen (2005) Data …...… CHIANTIGupta & Tayal (1998) Data
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.
Wavelengths of NIST data( N) and CHIANTI( C) data are different for Line
identification
C
N
C
N
C
N
FeXI
FeXII
FeXIII
α
αβ
β
γ
γδ
δ
Wavelengths for Fe 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.
NIST CHIANTI
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)
Observed FeXIII Line Intensity Ratios
• LHD&EBIT are close to calculations by AK and CHIANTI• Active@Sun Ne=2-10x109cm-3 、 Quiet@SunNe=3-30x108cm-3 。
活動領域
静穏領域
Summary for Fe spectral diagnosticsProton excitation between the fine structure levels is important as well electron excitationWavelength 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)
We are working on Data evaluation for Fe ions
• Proton impact excitation FeX - XV(NIFS-DATA), Fe
XVII - 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)
0.00
0.02
0.04
0.06
0.08
0.10
0 100 200 300 400
Electron temperature (eV)
Effective collision strength
Comparison of effective collision strengths
Fe XI 3s23p4 3P2 – 3s23p3(2D)3d 1F3 and 1D2
solid lines: Aggarwal and Keenan (2003) : Gupta and Tayal (1999)
3. Spectra from High Z elements
• 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+
G. O’Sullivan, C. Suzuki, H. Tanuma, T. Kato
W spectra near 5nm from LHD (NIFS)
QuickTime˛ Ç∆TIFF (LZW) êLí£ÉvÉçÉOÉâÉÄ
ǙDZÇÃÉsÉNÉ`ÉÉÇ å©ÇÈÇΩÇflÇ…ÇÕïKóvÇ≈Ç∑ÅB
Lower Te Higher TeTe(0) = 3 keV
Cowan Code CalculationsCowan Code Calculations
Fk, Gk and Rk parameters reduced to 80%. Spin Orbit parameter unchanged
0
5
10W XXIX
0
5
10W XXX
0
5
10W XXXI
0
5
10
gf
W XXXII
4 5 6 70
5
10
Wavelength (nm)
W XXXIII
0
5
10W XXXIV
0
5
10W XXXV
0
5
10
gf
W XXXVI
0
5
10W XXXVII
4 5 6 70
5
10
Wavelength (nm)
W XXXVIII
G. O’Sullivan4p64dn- 4p64dn-14f + 4p54dn+1 transitions
4d10
4d9
4d8
4d6
4d5
4d4
4d3
4d2
4d
UTA statistics for W XXIX – W XXXVIII
0
5
10W XXIX
0
5
10W XXX
0
5
10W XXXI
0
5
10
gf
W XXXII
4 5 6 70
5
10
Wavelength (nm)
W XXXIII
0
5
10W XXXIV
0
5
10W XXXV
0
5
10
gf
W XXXVI
0
5
10W XXXVII
4 5 6 70
5
10
Wavelength (nm)
W XXXVIII
0
500
1000 W XXIXμ1 = 4.91σ = 0.12
0
5001000 W XXX
μ1 = 4.95σ = 0.22
0
5001000 W XXXI
μ1 = 4.99σ = 0.29
0
5001000
gf
W XXXIIμ1 = 5.03σ = 0.36
4 5 6 70
5001000
Wavelength (nm)
W XXXIIIμ1 = 5.08σ = 0.42
0
5001000 W XXXIV
μ1 = 5.12σ = 0.48
0
5001000 W XXXV
μ1 = 5.16σ = 0.54
0
5001000
gf
W XXXVIμ1 = 5.19σ = 0.60
0
5001000 W XXXVII
μ1 = 5.23σ = 0.66
4 5 6 70
5001000
Wavelength (nm)
W XXXVIIIμ1 = 5.25σ = 0.72
28 29 30 31 32 33 34 35 36 37 38 394.8
4.9
5
5.1
5.2
5.3
5.4
Ion stage (charge +1)
UTA mean
λ (nm)
Mean of UTA matches ADAS data very wellWidths = standard deviation
Mean of UTA matches ADAS data very wellWidths = standard deviation
Putterich et al Plasma Phys. Control. Fusion 50 085016 2008
Cowan Code CalculationsCowan Code Calculations For W XVI – W XXVIII transitions based on the open 4f subsh
ell
4d104fn -4d104fn-15d4d104fn -4d94fn+1
n = 1
n = 4n = 3
n = 2
n = 5 n = 6 n = 7
ComparisonsComparisons
Sugar, Kaufman (1980)
4p-4d gives two groups of lines near 4.7 and 6.5 nm
Radke (2001)
Tentative Conclusions for W spectraTentative Conclusions for W spectra
WXXXIX-WXLV4p1/2-4d3/2
WXXXIX-WXLV4p3/2-4d5/2
WXXIX- WXXXVIII 4p64dn-4p54dn+1 + 4dn-14f
WXXII-WXXVII4d-4f
WXXII -WXXVII4f-5d
Going ForwardGoing 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+
W ion spectra in JT-60U plasma
• 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 (T
e > 10 keV).
4s-4p, 4p-4dtransitions
3p-3dtransitions
Yanagibayashi
EUV Spectra of Sn recorded at EUV Spectra of Sn recorded at NIFS NIFS
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.)
A. Sasaki et al Review of Laser Engineering Suppl. 1132 (2008)
Analysis of the UTAAnalysis of the UTA
• Spectra due to 4p64dn-4p64dn-14f + 4p54dn+1 transitions
• Configuration Interaction very important
Churilov and Ryabtsev Phys. Scr. 73 614-619, 2006
Charge Exchange Spectra of SnXV - Charge Exchange Spectra of SnXV - SnXVIIISnXVIII
Resonance 4p-4d Transitions in Sn XVIII – Sn XXResonance 4p-4d Transitions in Sn XVIII – Sn XXCowan Code CalculationsFk, Gk and Rk parameters reduced to 85%.Spin Orbit parameter unchanged
Resonance transitions cannot explain observed spectrum.
Origin of CXS spectral featuresOrigin 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.
Configuration Interaction effects in Sn Configuration Interaction effects in Sn XVII (example)XVII (example)
Strong final state CI for transitions of the type: 4s24p34d – 4s24p34f + 4s24p24d2 + 4s4p44d (between
excited states)
Comparison of theory with experiment, Comparison of theory with experiment, Sn XV and SnXVISn XV and SnXVI
Comparison between theoretical spectra for Sn XV and Sn XVI convolved with a Gaussian instrumental function and the observed experimental spectra of Sn XV and Sn XVI The theoretical data are also presented in the form of stick plots of height equal to the gf -value
Comparison of theory with experiment, Sn Comparison of theory with experiment, Sn XVII and SnXVIIIXVII and SnXVIII
Comparison between theoretical spectra of Sn XVII and Sn XVIII convolved with a Gaussian instrumental function and the observed experimental spectra of Sn XVII and Sn XVII. The theoretical data are also presented in the form of stick plots of height equal to the gf -value
Summary for high Z spectraSummary for high Z spectra
•Lines arising from 4d - 4f, 4p - 4d and 4f - 5d transitions in W XXII - XLV identified.•Calculations by Cowan’s code were made for 4d - 4f transitions in W XXIX - XXXVIII and 4f - 5d and 4d - 4f transitions in W XXIV - XXVIII.
•Strongest lines arising from 4d-5p, 4d-4f and 4p-4d transitions in Sn XV – Sn XVIII identified. •Necessary to allow for 4pm-14f + 4pm-24d2 + 4s4pm4d CI. Such interactions appear to be a universal feature associated with δn = 0, 4 – 4 excitation.
Data Compilation for Electron and Atomic Collisions with High Z elements; Ar, Fe, Ni, Kr, Mo, Xe and W
Working group for updating atomic and molecular collision data in the NIFS database AMDIS (electron scattering) and CHART (ion scattering) has been organized. This group has searched and reviewed literatures for collecting relevant atomic data which are to be included into NIFS database.
D. Kato, I. Murakami, M. Kato et al
Compiled data to be published in NIFS-DATA (2009)
Electron collisions• Kr, Xe Total, Elastic, Ionization cross sections, recombination, photo
emission, effective collision strength, W, Ne Ionizaiton, excitation, Fe Ionization, recombination, excitationAtom collisions Charge transfer cross sections with Ne Ion - ion and ion - atom collisions Ar State selective charge transfer cross sections --> added in
to CHART Kr Charge transfer, ionization, electron loss
ExampleElectron-impact cross sections for Fe ; Notation: charge number (E: experimental data. T: Theoretical calculation) Ionization: 4, +0(E), +21(T), +24(T), +25(E) Recombination: 12, +16(2T), +17(3T), +18(5T), +19(3T), +20(3T), +21(3T), +22(3T), +23(3T), +24(2T), +25(T) Excitation: 36, +1(T), +2(T), +3(T), +4(T), +8(T), +9(2T), +10(T), +11(T), +12(2T), +14(3T), +16(3T,E), +17(T), +18(3T), +19(3T), +20(5T), +21(5T), +22(5T), +23(6T), +24(2T), +25(T)
52 papers published in 2001-2006with help of Drs. J.-S. Yoon (NFRI, Daejon, Korea) and J. Yan (IAPCM, Beijing, P.R.China). Throughout the present compilation, majority of recent theoretical and experimental works seem intended for investigation of K-shell ionization, ionization of highly charged ions, and double-ionization.