spectroscopic research projects on heavy elements at nist
DESCRIPTION
Spectroscopic Research Projects on Heavy Elements at NIST. Wolfgang L. Wiese National Institute of Standards and Technology (NIST), USA. Participants. Experimental Research: J. Reader, G. Nave, J. Gillaspy, M. Bridges,* W. Wiese* - PowerPoint PPT PresentationTRANSCRIPT
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Spectroscopic Research Projects on Heavy Elements at
NIST
Wolfgang L. Wiese
National Institute of Standards and Technology (NIST), USA
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ParticipantsExperimental Research: J. Reader, G. Nave,
J. Gillaspy, M. Bridges,* W. Wiese*Theoretical Approaches: Ch. Froese-Fischer,*
Y. Ralchenko,*Y.-K. Kim , P. Stone*
Data Assessment and J. Reader, E. Saloman,* Compilations: J. Fuhr,* D. Kelleher,*
L. Podobedova,* A. Kramida,* W. Wiese*
Database Development: Y. Ralchenko,* A. Kramida*R. Ibacache
*indicates Contractors or Guest Researchers
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Three On-going Spectroscopic Research Projects on Heavy Elements at NIST
1. An updated and expanded critical compilation of spectroscopic reference data for Fe I and Fe II, focusing on better transition probabilities.
2. Calculations of ionization and excitation cross-sections of neutral and singly ionized Mo and W with the Binary-Encounter-Bethe (BEB) model.
3. Experimental observations of the spectra of highly charged tungsten ions, in the range from W+35 to W+63, with an Electron Beam Ion Trap (EBIT) and their analysis.
.
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Fe I
O’Brian 180 lifetimes and branching fractions
Blackwell absorption (based on one lifetime)
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Fe I
Kock several lifetimes and branching fractions
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Fe II
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Fe II
Raassen = semi-empirical calculation
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1988
2006
Fe I
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19882006
Fe II
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Electron-Impact Cross Section Database(http://physics.nist.gov/ionxsec)
M. A. Ali, K. K. Irikura, Y.-K. Kim, P. M. Stone
Already in the database:
1. Total ionization cross sections of neutral atoms and molecules, singly charged molecular ions (about 100)
2. Differential ionization cross sections of H, He, H2
3. Excitation cross sections of light atoms
New results to be added by summer, 2007:
4. Total ionization cross sections (direct + excitation-autoionization) of Mo, Mo+, W, W+ (joint work with KAERI, see graphs)—BEB model plus BE/E scaling of Born cross sections [Mo/Mo+ in Kwon, Rhee & Kim, Int. J. Mass Spectrometry, 245, 26 (2005)]
5. Excitation cross sections of H2 (see graphs)—BE scaling of Born cross sections
6. Ionization cross sections of Si, Ge, Sn, Pb, Cl, Br, I, Cl2, Br2, I2
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A Major Spectroscopic Research Project on Heavy Elements at NIST
• Experimental observations of the spectra of highly charged tungsten ions, in the range from W+35 to W+63, with an Electron Beam Ion Trap (EBIT) and their theoretical analysis.
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SPECTRUM OF W IN ORMAK
INTERPRETATION AS W XXX - W XXXV
ISLER, NEIDIGH, AND COWAN (1977)
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Cu and Zn sequences to W
READER & LUTHER (1980)
1S0-1P1
1/2-3/2
1/2-1/2
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The EBIT not only creates a highly charged ions, but can hold their center
of mass at rest.
EBIT size ~ 1 m
This overcomes the primary limitation of large HCI facilities for precision
spectroscopy.
To first order, the relative Doppler shift is
/ =v/c
The NIST Electron Beam Ion Trap (EBIT)
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Ion production, trapping, and excitation
http://physics.nist.gov/ebit
EBIT on a table top
EBIT Internal View
107 K plasma
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A simplified EBIT:
Intense Electron Beam (4,000 A/cm2)
Strong magnetic field (3 tesla)
Highly Charged Ions (up to Bi72+at NIST).
Creates (by electron impact ionization) Traps (by electric and magnetic fields) Excites (electron impact)
Ion cloud width ~ 150 m
2 cmUltrahigh vacuum (~10-10 torr)
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J.D. Gillaspy, Phys. Scr. T71, 99 (1997).
NIST EBIT 0.1-33 keV e-beam energy
Q up to 72+ produced
Ne-like U82+ threshold: 10 keV (10 remaining electrons)
He-like U90+ threshold: 33 keV (2 remaining electrons)
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• operates at 65 mK
• absorber: a foil of superconducting tin
• thermistor: neutron transmutation-doped
(NTD) germanium
Quantum Microcalorimeter
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“Crystal-quality” resolution, wide bandwidth and 100% efficiency.
L-shell
K-shell
Ar
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EUV SPECTROMETER AT NIST EBIT
BLAGOJEVIC, LE BIGOT, ET AL. (2005)
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IONIZATION ENERGIES FOR W IN ALL STAGES
KRAMIDA & READER (2006)
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Ion Seq.IE
103 cm–1
Unc.103 cm–1
IE eV
Unc. eV
Unc., %
Ref.
W0+ W 63.4277 0.0008 7.86403 0.00010 0.0013 CM96
W+ Ta 132.0 1.2 16.37 0.15 0.9 K04
W2+ Hf 209.9 3.6 26.0 0.4 1.7 TW
W3+ Lu 308.2 2.9 38.2 0.4 0.9 TW
W4+ Yb 416.1 2.7 51.6 0.3 0.6 TW
W5+ Tm 522.37 0.30 64.77 0.04 0.06 S79
W6+ Er 984.1 0.5 122.01 0.06 0.05 S75
W7+ Ho 1139 10 141.2 1.2 0.9 TW
W8+ Dy 1292 10 160.2 1.2 0.8 TW
W9+ Tb 1444 10 179.0 1.2 0.7 TW
W10+ Gd 1685 10 208.9 1.2 0.6 TW
W11+ Eu 1868 10 231.6 1.2 0.5 TW
W12+ Sm 2083 10 258.2 1.2 0.5 TW
W13+ Pm 2345 10 290.7 1.2 0.4 TW
W14+ Nd 2624 12 325.3 1.5 0.5 TW
W15+ Pr 2919 12 361.9 1.5 0.4 TW
W16+ Ce 3129 10 387.9 1.2 0.3 TW
W17+ La 3393 11 420.7 1.4 0.3 TW
W18+ Ba 3727 11 462.1 1.4 0.3 TW
W19+ Cs 4054 11 502.6 1.4 0.3 TW
W20+ Xe 4383 11 543.4 1.4 0.3 TW
W21+ I 4795 12 594.5 1.5 0.3 TW
W22+ Te 5167 12 640.7 1.5 0.2 TW
= THIS WORK
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IONIZATION ENERGIES OF W IONS
ION SEQUENCE GROUND CONFIG
ENERGY(eV)
W40+ Se 4s24p4 1941
W41+ As 4s24p3 1995
W42+ Ge 4s24p2 2149
W43+ Ga 4s24p 2210
W44+ Zn 3d104s2 2354
W45+ Cu 3d104s 2414
W46+ Ni 3d10 4057
W47+ Co 3d9 4180
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COMPILATIONS of W SPECTRA AND ENERGY LEVELS
KRAMIDA & SHIRAI (2006 & 2007)
W I & II (260 pages)
W III - LXXIV (~250 pages)
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IE (eV)
Cowan
(1977)
IE (eV) - Exp
Kramida
(2006)
Transition WL(Å) Cowan
(1977)
WL(Å) -Obs Obs. Source
Zn-like 44+ 2354 2354.5(1.5) 4s2 1S0 - 4s4p 1P1 60.2 60.931(2) Livermore
4s2 1S0 - 4s4p 3P1 135.0 132.88(3) ASDEX/NIST
4s4p 3P1 - 4s4p 3P2 127.47 134.80(3) NIST
Cu-like 45+ 2415 2414.1(4) 4s 2S1/2 - 4p 2P3/2 61.2 62.336(2) Livermore
4s 2S1/2 - 4p 2P1/2 127.5 126.998 Seely - ISO
Ni-like 46+ 4055 4057(3) 3d10 1S0 - 3d94f 3D1 5.68 5.6900(3) Livermore
3d10 1S0 - 3d94f 1P1 5.87 5.8665(3) Livermore
3d10 1S0 - 3d94f 3P1 5.95
3d10 1S0 - 3d94p 3D1 6.75 6.779(3) Israel
3d10 1S0 - 3d94p 1P1 7.01 7.028(3) Israel
3d10 1S0 - 3d94p3P1 7.17 7.1733(3) Livermore
COWAN (1977) vs. OBSERVED
IE’s SEMI-EMPIRICAL - KRAMIDA & READER (2006)
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CuCu
O
O
CuCu
Zn
GaGe
Zn Zn
Ge
Ge
Ga
BrBr
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CR MODELING OF PLASMA OF W IN NIST EBIT -
RALCHENKO ET AL. (2007)
EXPERIMENT THEORY
CO
UN
TS
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SPECTRUM OF W IN NIST EBIT AT 4228 eV RALCHENKO ET AL. (2007)
Cu
Ni UTA
Ni
Cu
CoNiZn
* = 2 or 3 rd order
+ = O or NCu
Ni UTA
Cu
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4p
4f
5f6f
4s
X-RAY SPECTRUM OF W WITH MICROCALORIMETER ON NIST EBIT
3d10-3d9nl
RALCHENKO ET AL. (2006)
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E2 LINES OF W IN NIST EBIT - RALCHENKO ET AL. (2006)
0
2
1
2
3d10
3d94s
3
7.610 Å
7.930 Å
M
E2
E2
L
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4p
4f
5f6f
4s
X-RAY SPECTRUM OF W WITH MICROCALORIMETER ON NIST EBIT
3d10-3d9nl
RALCHENKO ET AL. (2006)
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E2 AND M3 LINES OF W IN NIST EBIT
RALCHENKO ET AL. (2006)
0
2
1
2
3d10
3d94s
3
7.610 Å
7.930 Å0.009 Å
M
L
E2
E2M3
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CALCULATED E2:M3 RATIOS
RALCHENKO J. Phys. B: At. Mol. Opt. Phys. 40 (2007) F175
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