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.