4th International Colloquium on Atomic

Spectra and Oscillator Strengths for

Astrophysical and Laboratory Plasmas

POSTER PAPERS

Jack Sugar and David Leckrone, Editors
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A75r Special Publication 850

4th International Colloquium on Atomic

Spectra and Oscillator Strengths for

Astrophysical and Laboratory Plasmas

POSTER PAPERS

at the National Institute of Standards and Technology

y

Gaithersburg, Maryland

September 14-17, 1992

Jack Sugar and David Leckrone,* Editors

Atomic Physics Division

Physics Laboratory

National Institute of Standards and Technology

Gaithersburg, MD 20899

*NASA/Goddard Space Flight Center

Greenbelt, MD

April 1993

U.S. Department of Commerce

Ronald H. Brown, Secretary

National Institute of Standards and Technology

Raymond G. Kammer, Acting Director
National Institute of Standards U.S. Government Printing Office

and Technology Washington: 1993

Special Publication 850

Natl. Inst. Stand. Technol.

Spec. Publ. 850

199 pages (Apr. 1993)

CODEN: NSPUE2

For sale by the Superintendent

of Documents

U.S. Government Printing Office

Washington, DC 20402
Sponsors

National Institute of Standards and Technology

National Aeronautics and Space Administration

Naval Research Laboratory

U.S. Department of Energy, Office of Fusion Energy

National Science Foundation

Computer Sciences Corporation

IBM

Program Committee

D. Leckrone (Chairman), NASA, Goddard Space Flight Center, Greenbelt, MD

S. Adelman, CITADEL, Charleston, SC

R. C. Elton, Naval Research Laboratory, Washington, D.C.

J. E. Hansen, Zeeman Laboratory, University of Amsterdam

S. Johansson, University of Lund, Sweden

R. McKnight, U.S. Department of Energy, Germantown, MD

D. Morton, Herzberg Institute of Astrophysics, NRC, Ottawa, Canada

J. Sugar, NIST, Gaithersburg, MD

Organizing Committee

J. Sugar (Chairman), NIST, Gaithersburg, MD

R. Bell, University of Maryland, College Park, MD

L. Curtis, University of Toledo, Toledo, OH

G. Doschek, Naval Research Laboratory, Washington, D.C.

D. Leckrone, NASA, Goddard Space Flight Center, Greenbelt, MD

W. Wiese, NIST, Gaithersburg, MD

It

iii
Colloquium This was the fourth in a series of colloquia begun at the

Description University of Lund, Sweden in 1983 and subsequently held in

Toledo, Ohio and Amsterdam, The Netherlands. The purpose of

these meetings is to provide an international forum for

communication between major users of atomic spectroscopic

data and the providers of these data. This affords an

opportunity for the users to review their present and future

needs and the providers to review their laboratory capabilities,

new developments in data measurement, and improved

theoretical capabilities. These data include atomic wavelengths,

line shapes, energy levels, lifetimes, and oscillator strengths.

Speakers were selected from a wide variety of disciplines

including astrophysics, laboratory plasma research,

spectrochemistry, and theoretical and experimental atomic

physics.

Contact between data users and providers has grown even more

critical today with the prolific acquisition of data from spacebased astrophysical observatories, with high temperature

laboratory experiments in fusion energy and x-ray lasers, and

with the demands for higher accuracy and large quantities of

data from neutral to highly ionized atoms. The means of

delivery of these data with new light sources such as the

tokamak, the electron beam ion trap (EBIT), laser-generated

plasmas, inductively-coupled plasmas (ICP), and with new

techniques such as laser-induced fluorescence and fourier

transform spectroscopy, has advanced considerably.

These colloquia assist in matching these resources with the

current and anticipated demands for atomic data.

Format The progi'am consisted of presentations by invited speakers and

poster sessions. One session was devoted to an informal

workshop at which users of data briefly described their most

immediate needs and providers of data give brief summaries of

work currently in progress. The invited papers will be

published in a topical issue of Physica Scripta.

iv
Table of Contents

Lifetimes-theory

Transition Rates in the 3d^ Configuration of the Calcium Isoelectronic

Sequence 3

E. Biemont, J. E. Hansen, P. Qiiinet, and C. J. Zeippen

Oscillator Strengths of Astrophysical Interest for Ol-sequence 4

K. S. Baliyan and A. K. Bhatia

Radiative Data for Si-like Ions: Si°, S-^, A^^, Ca^+ 7

Sultana N. Nahar and Anil K. Pradhan

Large Scale Radiative and Collisional Calculations for Fe II 10

Sultana N. Nahar and Anil K. Pradhan

Calculation of Oscillator Strengths in Hg III 13

P. H. M. Uylings, A. J. J. Raassen, A. A. Joueizadeh,

J. O. Ekberg Se. Johansson, and J.-F. Wyart

Transitions in Neutral Chromium 16

D. J. R. Robinson and A. Hibbert

RCI Calculation of Energy Levels and Oscillator Strengths in Highly

Ionized Atoms 19

Takashi Kagawa, Yoshie Honda, and Shiiji Kiyokawa

A Density-Matrix Description for the Broadening of Spectral Lines

by Autoionization, Radiative Transitions, and Collisions 22

V. L. Jacobs

Developments in Computation of Form Factors 23

C. T. Chantler

Accurate Oscillator Strengths for Neutral Carbon and Astrophysical

Implications 26

E. Biemont, A. Hibbert, M. R. Godefroid, and N. Vaeck

Relativistic Study of Lifetimes for the ns^np^(n + l)s Levels in Heavy

Systems 29

Jacek R. Bieroh and Jacek Migdalek

Oscillator Strengths for the Transitions in Singly Ionized Kr II 31

P. Anantha Lakshmi and K. S. Baliyan

V
Lifetimes — measurements

Transition Probabilities and Line Shapes: Usage and Needs at the

University of Illinois 37

Alexander Scheeline, Cheryl A. Bye, Herman Krier,

Jyotirmoy Mazumder, Xiangli Chen, Tom Duffey,

Siidhir Tewari, David Zerkle, and Mark J. Kushner

New Measurements in the Spectrum of Neutral Lithium (Li I) by Fourier

Transform Spectroscopy 40

Leon J. Radziemski, Rolf Engleman, and James Brault

The Atomic Branching Ratio Project at NIST 41

/. Z. Klose and W. L. Wiese

Precision Measurement of the Mean Life of the Ar II 4p' Level 44

Jian Jin and D. A. Church

Accurate Oscillator Strengths for Interstellar Ultraviolet Lines of CI I 47

R. M. Schectman, S. R. Federman, D. J. Beideck,

and D. G. Ellis

Relative Intensities of Resonance Transitions in B-like Ions 50

/. Doerfert, E. Trabert, P. H. Heckmann, G. Mdller,

J. Granzow, and C. Wagner

Accelerator-based Spectroscopy Projects at Bochum 53

E. Trabert

Work in Progress at the Lund VUV-FTS 56

Ulf Litzen and Sveneric Johansson

Radiative Decay Rates for the 3s3p^(*P) Metastable Levels of Si II 59

Anthony G. Calamai, Peter L. Smith, V. H. S. Kwong

and William H. Parkinson

Atomic Oxygen Transition Probabilities and Recombination Rates of

Astrophysical and Geophysical Interest 62

V. Escalante, G A. Victor, and A. Gongora

Transition Probabilities and Lifetimes of Ar I 65

K Helbig D. E. Kelleher, and W. L. Wiese

Calculated Ar XVII Line Intensities and Comparison with Spectra

from the Alcator C Tokamak 68

K. J H. Phillips, F. P. Keenan, L. K. Harra, S. M. McCann,

E. Rachlew-Kdllne, J. E. Rice, and M. Wilson

Comprehensive Measurements of Fe I Oscillator Strengths 71

T R. O'Brian, M. E. Wicklijfe, J E. Lawler, W. Whaling

and J. W. Brault

Measurement of Lifetimes of Excited States of Selected VUV Lines

of N I, N II, Al II, and Al III 74

Santosh K. Srivastava

Oscillator Strength Measurements of Neutral Nitrogen Lines in the

900 - 1200 A Range 77

C. Goldbach, T. Liidtke, M. Martin, and G Nollez

vi
Sun and Stars

Observed Redshift of O V Lines in Solar UV Spectra 83

P. Brekke

Ruthenium Stellar Abundance Determined from FTS Branching Ratios,

LIF Lifetimes and HST Observations 86

S. Johansson, A. Joueizadeh, U. Litzen, J. Larsson,

A. Persson, S. Svanberg D. S. Leckrone, and G. M. Wahlgren

Investigating the Pt III Spectrum in Chemically Peculiar Stars 88

Glenn M. Wahlgren, David S. Leckrone, and Sveneric Johansson

Burst Models for Line Emission in the Solar Atmosphere 91

/. M Laming and U. Feldman

Photoionization Resonances of Si II in the Spectrum of Ap Si Stars 93

T. Lanz, M.-C. Artru, M. Le Dourneuf, and I. Hiibeny

Photospheric Heavy Elements in Hot, Hydrogen-rich White Dwarfs

(DA WD) 96

Stephane Vennes and Stuart Bowyer

Atomic Data Needs for Optical Region Studies of Early A Type Stars 99

Saul J. Adelman and Austin F. Gulliver

Experimental Isotope Shifts in Ni II and Fe II 102

Maria Rosberg Ulf Litzen, and Sveneric Johansson

Accurate Wavelengths and Isotope Shifts for Lines of Doubly-ionized

Mercury (Hg III) of Astrophysical Interest 105

Craig J. Sansonetti and Joseph Reader

Line Blanketing in Nova Atmospheres 108

P. H. Hauschildt and S. Starrfield

Density Sensitive Lines of Boron-like Ions of C, N and O Ill

Philip Judge, Rong Lu, Paal Brekke, and Anil Pradhan

The Need for Electron/Neutral-atom Collision Cross Sections

at Thermal Energies 114

Philip Judge and Mats Carlsson

Laboratory Sources

Interpretation of the VUV Spectra of Some Iron Group Element Ions 119

W.-U. L. Tchang-Brillet, J.-F. Wyart, V. Azarov,

L. L Podobedova, and A. N. Ryabtsev

VUV-lines of Low-Z Ions and Their Identification 122

H. H. Bukow, A. Bastert, G. Rieger, and M. Krenzer

Analysis of the (5s5p--l-5s-5d) - [5p^-l-5s5p5d+5s5p6s] Transitions

of IV 125

A. Tauheed and Y. N. Joshi

New High Excitation Fe I Levels Determined by Fourier Transform

Spectrometry 128

Gillian Nave and Sveneric Johansson

vii
A Progress Report on the Analysis of VUV-FTS Spectra of Ru I and Ru II . . . . 131

Ali Joueizadeh and Sveneric Johansson

Diagnostics of Electron Temperature and Density in High Density Plasmas

Using L-shell Xenon Emission Spectroscopy 134

C /. Keane, B. A. Hammel, A. L. Osterheld, D. R. Kania

120-keV Kr^* - Li Collisions Studied by Near UV and Visible

Photon Spectroscopy 136

E. Jacquet, P. Boduch, M. Chantepie, M. Druetta, D. Hennecart,

X. Husson, D. Lecler, N. Stolterfoht, and M. Wilson

Photon and Auger Spectroscopy of Single and Double Electron

Capture Following 90-keV C^^ -Li Collisions 139

F. Fremont, E. Jacquet, P. Boduch, M. Chantepie, G. Cremer,

D. Hennecart, S. Hicham, X. Husson, D. heeler, N. Stolterfoht,

M. Druetta, and M. Wilson

Measurements of Electron Emission from Collisions of MeV Energy

N, C, and He Ions with He Gas 142

N. A. Guardala, J. L. Price, D. J. Land, M. F. Stumborg,

D. G. Simons, and G. A. Glass

Update on the NIST EBIT 145

/. D. Gillaspy, J. R. Roberts, C. M. Brown and U. Feldman

Performance and Resolving Power of Concave Multilayer-coated

Gratings Operating Near Normal Incidence in the 136-300 A Region 148

/. F. Seely, M. P. Kowalski, W. R. Hunter, J. C. Rife,

T. W. Barbee, Jr., G. E. Holland, C. N. Boyer and C. M. Brown

New Line Identifications in Xe VIII and Xe VII 151

M. Druetta, D. Hitz, and P. Ludwig

Transition Element Spectra by High Resolution Fourier Transform

Spectrometry 154

Jon. E. Murray, J. Pickering, G. Nave, R. C. M. Learner,

and A. P. Thome

Atomic Structure-theory

Atomic Structure in Ultrastrong Magnetic Fields 159

E. P. Lief and J. C. Weisheit

Fine Structure Splittings in the Ground State of B-like Ions:

Rb^^^--Xe^^^ 162

M. A. Ali and Y.-K. Kim

Complex Quantum Defect and Screening Parameters for Autoionizing

States of Two- and Three-electron Atoms from Lowest-order

Perturbation Theory 165

Lonnie W. Manning and Frank C. Sanders

Pair Function Calculations for Screened Coulomb Potentials 168

Zhengming Wang Yong Yan, Hongbin Zhan, and Peter Winkler

Atomic Properties from Large-Scale Relativistic Calculations 171

F. A. Parpia and C. F. Fischer

viii
Convergence Studies of Atomic Properties from Variational Methods:

Total Energy, Ionization Energy, Specific Mass Shift, and Hyperfine

Parameters for Li and Be 174

Ming Tong Per Jonsson, and Charlotte Froese Fischer

Prospects for Relativistic Multiconfiguration Dirac-Fock-Breit

Calculation Using Gaussian Basis Set Method 177

Farid A. Parpia and Ajaya K. Mohanty

Databases

Critically Evaluated Data on Atomic Spectra-energy Levels,

Wavelengths, and Transition Probabilities 183

W. C. Martin, A. Miisgrove, J. Reader, J. Sugar,

W. L. Wiese, J. R. Fiihr, G. R. Dalton, and T. Shirai

Need for Complete Spectroscopic Tables 186

Vivek Bakshi, Tom D. Boone, Jr., and William C. Nunnally

Spectral Atlas of the Inductively Coupled Plasma 189

R. K. Winge, D. E. Eckels, S. J. Weeks,

J. C. Travis, and M. L. Salit

Atomic Data Center for Astrophysical and Laboratory Plasmas 192

K. T Lii, Dennis Baba, and Aria Kohshkhoii

ix
I

I
Lifetimes-theory

Transition Rates in the 3d Configuration

of the Calcium Isoelectronic Sequence

E. Biemont^'*, J.E. Hansen^, P. Quinet^'^

4 and C.J. Zeippen

1 Institut d 'Astrophysique et Institut de Physique Nucleaire

Experimentale, Universite de Liege, B-4000 Liege, Belgium.

2 Van der Waals-Zeeman Laboratorium, Universiteit van Amsterdam,

NL-1018 XE Amsterdam, The Netherlands.

3 Faculte des Sciences, Universite de Mons-Hainaut , B-7000 Mons, Belgium.

4 lli'K 261 du CNRS et DAMp, Observatoire de Pans, F-92195 Meudon, France.

Abstract

Transitions emitted from the 3d" configurations are important

in hot plasmas of low electron density (i.e. in astrophysical

objects or in Tokamak devices) where magnetic dipole (Ml)

or electric quadrupole (E2) transitions become observable

due to low collisional rates for the deexcitation from metastable levels. In this work, we concentrate on the study of

2 the forbidden (Ml and E2) transitions appearing in the 3d

ground configuration of the Ti III to Ag XXVIII Ca-like ions.

Three different theoretical methods (MCDF, HFR and SST) taking

configuration interaction into account are compared with

respect to their ability to predict energy levels and radiative transition rates for the forbidden lines considered.

2 The probabilities for the 3d -3d4s transitions, which might

significantly contribute to the depopulation processes of

the 3d4s levels are also predicted. It is shown that the

methods considered 'in our work are basically equivalent,

in their respective range of applicability, for the prediction

of accurate oscillator strengths.

* Senior Research Associate of the Belgian FNRS.

$ Hnlrl^r nf sr. TRSIA Fellowshin.

3
Oscillator strengths of astrophysical interest for Ol-sequence

K S Baliyan* and A K Bliatia

Laboratory for Astronomy and Solar Physics, NASA/Goddard Space Flight Center

Greenbelt, Maryland 20771 USA

X-ray and UV emission lines due to the transitions in the ions of oxygen iso-electronic sequence

are frequently observed in the spectra of astrophysical objects, such as solar flares, active Sun,

supernova remnants and other stellar objects. Many of these lines are Usted by Acton et al. [1] and Doschek and Cowan [2] for the 10- 200 A range and recently by Feldman and Doschek [3] for 910- 1200A range. Most of the lines in this spectral region are from the transitions in the

highly ionized atoms. This spectral information may be used to determine the gas temperature

and the density of the emitting plasma through diagnostic emission line ratios. To evaluate these

quantities accurate oscillator strengths and electron- excitation rates are required.

Here we report oscillator strengths for several transitions among the ground and excited

states of the oxygen-like Ca XIII ion. We will also discuss intercombination transition OI('^P^ —

2s'^2p^^s ^5°). Extensive configuration interaction wavefunctions have been used for the states involved in the transitions. The calculations are performed in both, the LS and the intermediate

coupling schemes. In a configuration interaction calculation, the atomic wavefunctions have a form of a configuration state function superposition,

m

^J{LS) = Y.Ct^M<^^LS) (1)

1 = 1

in the LS coupling or m

*.(J) = E«u<^^(«^LiSiJ) (2)

i =l

in the Breit-Pauli approximation. For a given set of {(f>i}, the variationally optimal values of the

mixing coefficients aij are the components of the eigenvectors of the Hamiltoinian matrix. The

configuration state functions {(f)i} are built using the one electron orbitals:

Unlm.mAr) = - PrrMY'r' {0 , <P)x'^ ' {s) (3) r and radial functions are expressed in analytic form as:

k Pni{r) = 5]QrP^exp(-Czr). (4)

1=1 Several choices of the orbital basis set were considered. The final CI calculation has been performed using an orthogonal basis set,

{Is, 2s, 2p, 3s, 3p, 3c?, 4s, ip, id, bs, bp}.

The Is, 2s and 2p orbitals were taken from tables of Clementi and Roetti [4] given for the

*NAS-NRC Research Associate

4
K. S. Baliyan and A. K. Bhatia 5

ground state 2s^2p^ ^P^ . The radial functions for the rest of the orbitals are obtained by using

CIVS [5] program. The 3s radial functions were obtained by minimizing 3s state energy.

Since 3s function in 3s is different from the one in 3s ^5°, we used 4s orbital to optimize on

Table 1

Transition Oscillator st rength

L(CIl) V(CIl) L(CI2) V(CI2)

2s22/ ^P- 2p^3s 4 1697( -2) 4.0866(-2) 4.169( -2) 4.166( -2)

2s22/ 3p. 2p^3d 1 7528( -1) 1.5496(-1) 1.7657( -1) 1.5019( -1)

2p^35 ^5"- 2p^3p ^P' 2 5036( -1) 2.4638(-l) 2.8110( -1) 3.4670( -1)

6 3385( -2) 6.1239(-2) 6.0918( -2) 5.9899( -2)

2s22p4 2p^3d 2 8840( -1) 2.7423(-l) 2.9629( -1) 2.7486( -1)

2s^2p^ 3P- 2p3(2D°)3(^ 5 17291 -1) 4.8677(-l) 0.25961 -1) 4.86581 -1)

2s22/ 2s2p^ 1 0997( -1) 9.8608(-2) 1.1008( -1) 9.5607( -1)

2s 2p^ P- 2p'*35 ^P° 3 6415( -2) 3.7456(-2) 3.5578( -2) 3.744( -2)

2p^3s ^P°- 2p337) ^S' 2 7871( -2) 2.9125(-2) 2.6894( -2) 2.8229( -2)

2s2p' ^P°- 2s2p'*35 1 5507( -2) 1.6761(-2) 1.5236( -2) 1.7036( -2)

2s22p'* ^i^^- 2^2?^ 1 4075( -1) 1.0441(-1) 1.3985( -1) 1.0278( -1)

2s22p^ ^D'- 2p^3s ^P° 3 0290( -2) 3.2023(-2) 2.9394( -2) 3.2165( -2)

2s'^2p^ ^D'- 2p^33 1 0115( -1) 9.8737(-2) 9.6989( -2) 9.5700( -2)

2p^35 '5°- 2p33p ^P' 2 9207( -1) 2.8546(-l) 2.9628( -1) 2.8180( -1)

2p^3p ^P"- 2s2p^3p ^5° 1 8533( -2) 1.2398(-2) 1.8638( -2) 1.3560( -2)

the energy of 3s ^5° state. The 5s orbital parameters were obtained on the average energy of

4s ^5° and 4s states. The 3p orbital was obtained minimizing ground state energy and 4p was subsequently optimized on the 3p ^P^ state. The average energy of 4p ^P^ and 4p ^P^ was

used to obtain parameters for the 5p orbital. The 3d and 4d orbitals were obtained minimizing

3d and 4d states respectively. In all 1221 configurations were formed for 21 even and

odd parity symmetries using these orbitals in CIl calculation while a limited set of configurations

(a^j > 0.005) was retained in CI2 calculation ( see table 1).

In general, there is a good agreement between the calculated energies of the states and the

values given by Sugar and CorUss [6]. These CI wavefunctions are used to calculate oscillator

strengths in the dipole length and velocity formulation. Most of the length and velocity f- values

agree within 10%. But for some of the transitions they differ by as much as 50%. This is mainly

due to the use of common basis orbital set. These transitions need be considered separately. The

intermediate coupling f- values are obtained by including the spin-orbit (S-0), spin spin (SS),

spin-other orbit(S-O-O), mass correction and Darwin terms of the Breit-Pauli operator in the

non-relativistic Hamiltonian. These calculations were performed using the configurations of the

CII2 model. The f- values for some transitions calculated in the LS and intermediate coupling are given in tables 1 and 2, respectively. It was observed that S-0-0 term plays very important role

in the case of intercombination transitions. The inclusion of this term reduces the f-value for

these transitions by a factor of half while it has Uttle effect on the spin allowed transitions.
6

The ground state intersystem transitions of 01 at 1355.6 and 1358. 5A are important probe of

the oxygen abundance in interstellar medium and are potentially observable in the high resolution

spectra of stars (Leckrone and Adelman [7]). We used an extensive CI basis and obtained

4.28 xlO"*^ as gf- value for - 2p'^35 transition in 01. The detailed results wiU be presented

at the conference.

Table 2

Transition

^-f

Oscillator strength

L V

2s2 2/ 2s2p^35 ^Sl 4.4074( -2) 4.5300( -2)

28^2^^ 2s2p^35 ^5° 3.4895( -2) 3.4984( -2)

25^2^'' ^Po- 2s2p^35 4.0848( -2) 4.0149( -2)

'P2- 2s2p^35 5.7436( -4) 5.7590( -4)

2s22/ 'Pl- 2s2p^35 'S°2 1.3444( -4) 1.3510( -4)

'P2- 2s2p335 ^Dl 4.8491( -2) 4.9174( -2)

2s'2p^ 'P2- 2s2p335 2.0743( -2) 2.1229( -2)

2s'2p' 'P2- 2s2p335 ^Dl 8.5226( -4) 8.6304( -4)

2s'2p^ 'Pl- 2s2p335 ^D" 2.6739( -2) 2.6185( -2)

2s2 2p^ 'Pl- 2s2p335 ^Dl 2.3912( -2) 2.3767( -2)

2s2 2p'» 'Po- 2s2p335 ^D^ 3.6865( -2) 3.5418( -2)

2s^2p^ 'Pl- 2s2p=^35 ^P° 2.7642( -2) 2.8159( -2)

2s^2p^ 'P2- 2s2p=^35 ^P° 4.4341( -3) 4.5546( -3)

2s^2p' 'Pl- 2s2p3 35 ^P° 7.1692( -3) 7.4349( -3)

2s22p4 2s2p3 35 ^P^ 1.2015( -2) 1.2366( -2)

2s2p^ 3 no 2s2p33p 2.7593( -4) 2.9368( -4)

2s22p^ ^D2- 252/ ^P^ 2.6433( -3) 2.6984( -3)

2s2p^35 'SI- 2s2p^3p 'P2 9.9538( -2) 9.3898( -2)

2s2p^35 5 Co'-'2' 2s2p^3p 'Pi 5.9212( -2) 5.6578( -2)

2s2p^35 5 Co ^2" 2s2p33p 1.7761( -3) 1.6263( -3)

We wish to thank Dr D S Leckrone for helpful discussions. This work was funded by NASARTOP-188-38-53-14 grant. One of us (KSB) is thankful to NRC for research associateship.

1. Acton LW, Bruner ME and Brown WA 1985 Ap .J 291 865.

2. Doschek GA and Cowan RD 1984 Ap J (suppl) 56 67.

3. Feldman U and Doschek GA 1991 Ap J(suppl) 75 925.

4. Clementi E and Roetti C 1974 At. Data Nucl. Data Tables 14 177.

5. Hibbert A 1975 Comput.Phys.Conimun.9 141.

6. Sugar J and Corliss C 1985 J. Phys. Chem. Ref. Data 14 (suppl.2).

7. Leckrone DS and Adelman SJ 1986 in 'New Insights in Astrophys.' ed EJ Rolfe, p 65.
Radiative data for Si-Uke ions: Si", S^"^, A^"^, Ca"""

Sultana N. Nahar and Anil K. Pradhan

Dept of Astronomy, The Ohio State University, Columbus, OH 43210

Radiative data such as photoionization cross sections, oscillator strengths, energy levels for Si - like ions,

SiO, S2+, a4+ and Ca6+ are obtained as a part of the Opacity Project (OP) [1]. Calculations are carried out in the close coupling (CC) ^proximalion using the R-matrix method [2]. Partial photoionization cross sections of

the -^P ground state of each ion into various excited states of the residual ion are obtained.

Large number of bound states with n<10, l<5are considered, amounting to a few hundred excited states for each atom and ion. Table I shows number of bound SL;i's and the corresponding number of excited bound

states for each ion. All calculated energies for Sfi, S2+, a4+ and Ca^ agree in less than 5% with the observed

values except for a few excited states of Si^. Table I fH-esents observed and calculated ionization energies (IP.) of

the ^P ground state of each ion. Detailed photoionization cross sections, including autoionizing resonances, of all the excited bound states, ^bnd' obtained. Photoionization cross sections of the •'P ground state of Si-like ions are presented in the lowest panels of Figs. 1(a) - (d). Presence of a wide resonance near the threshold for Si^ can be

observed in Fig. 1(a). The upper panels of Figs. 1(a) - (d) exhibit partial photoionization cross sections of the ground state in to various exctied thresholds of the residiual ion. Partial cross sections are important in the determination of level populations under non-LTE conditions. The excited state photoionization cross sections usually show nonhydrogenic behavior. Excited states that are coupled to the ground state of the residual ion

show wide PEC (photoexcitation-of-core) resonances in the cross section profile. PEC's are due to excitation of

the core to dipole allowed stales while the outer electron remain as a spectator. The PEC resonances can enhance

the background cross sections significantly. Example of PEC features will be illustrated in poster presentation.

Except for a number of states of Si^, the photoionization cross sections detailed with autoionizing resonances and for a large number of states of S2+, A"^ and Ca^ are obtained fcM* the first time as known to the authors. Dipole oscillator strengths for transitions among all bound states with n < 10 are obtained in LS

multiplets. Table I shows the number of oscillator strengths obtained for each ion. A short comparison is made

with the available theoretical and experimental values in Table II. Oscillator strengths of Si^ show good

agreement with the values mesasured recently using laser induced flourescence, so are the oscillator strengths of

5^+ with a number of measured values obtained using beam-foil technique. Good comparison of oscillator strengths of a4+ and Ca^ is also found with the very little available data.

References

1. "Atomic Data for Opacity Calculations" XVI, Sultana N. Nahar and Anil K. Pradhan, JPhys. B (submtted).

2. M. J. seaton, J. Phys. B 20, 6363 (1987); K.A. Berrington, P.G. Burke, K. BuUer, M.J. Seaton, P.J. Storey, K.T. Taylor, and Yu Yan, J. Phys. B 20, 6379 (1987).

3. TP. O'Brian and J£. Lawler, Phys. Rev. A 44, 7134 (1991).

4. U. Becker, H. kerhoff, M. Kwiatkowski, M. Schmidt, U. Teppner and P. Zimmermann, Phys. Rev. Lett. 76A, 125 (1980).

5. Berry H G, Schectman R M, Martinsen I, Bickel W S, and Bashkin S J, J. Opt. Soc. Am. 60, 335 (1970).

6. Livingston A E, Dumont P D, Baudinet-Robinet Y, Gamir H P, Biemont E, and Grevesse N, in "Beam-Foil

Spectroscopy", eds. I.A. Sellin and DJ. Pegg, (PlCTum, New York), p. 339, 1976.

7. Ryan L J, Raybum L A. and Cunningham A J, J. Quant Spectrosc. Radiat. Transfer 42, 295 (1989).

8. Irwin D J G, Livingston A E and Kemahan J A, Nucl. Inst. Meth. 110, 111 (1973).

9. Biemont E, J. Opt. Soc. Am. B 3, 163 (1986).

* This work has been carried out on the Cray Y-MP at the Ohio Supercomputer Center and is supported

partially by a grant from NSF (PHY- 9115057).

7
8

Table I: Ionization potential, LP., of the ions; ^SLn number of bound symmetries and N^n^j is the

corresponding number of bound states with n < 10 and I < 5 for each ion; Nf is the number of oscillator strengths obtained far each ion.

Ion l.P.(Ry) NsLtc Nbnd Nf Ion NsLti Nbnd Nf

obs cal obs cal

SiO 0.598 0.601 27 218 3149 5.515 5.499 36 342 7863

S2+ 2.573 2.574 31 236 3973 9.389 9.364 40 497 16961

Table II: Oscillator strengths of Si^, $2+, and Ca^.

SiO S2+

Transition f Transition f OP expt OP expt

3p2 - 3p4s 3p. 3j>o 0.236 0.211^ 3p2- 3s3p3 3p. 3d° 0.024 0.022±.0025,.0226

Ipo 0.195 0. 163^,0. 170"^ 3p. 3po 0.043 0.036^

is- Ipo 0.101 0.09133,0.0984 iD- l£)0 1.02 0.9910.10^

3p2 -3p3d 3p. 3po 0.053 0.05 13^ 3p2- 3p3d 3p- 3 DO 1.670 0.96±0.19'' iD- Ipo 0.0056 0.0029^,0.00364 iD- l^o 0.021 0.016710.0005^

iD- l£)0 0.041 0.040^ 3p4p -3p4d 3D- 3po 0.947 0.685±0.055

Ipo 0.358 0.3 18^ 3p2- 3p4s Ipo 0.094 0.07±0.047

is- Ipo 0.409 0.331^,0.3554 is- Ipo 0.066 0.0810.05'^

3p2 - 3s3p3 3p. 3do 0.051 0.0563

a4+ Ca^

OP expt OP Ref. 9

3p2- 3s3p3 3p- 3po 0.061 0.057±0.0028 3p2 -3s3p3 3p- 350 0.268 0.249

3p- 350 0.306 iD- Ipo 0.250 0.236

3p- 3 DO 0.042 iD- iDO 0.088 0.096

3p2- 3p3d 3p- 3po 0.581 is- Ipo 0.175 0.191

3p- 3 DO 1.411 3p2 -3p3d 3p- 3 DO 1.133 1.082

iD- Ipo 1.212 3p- 3po 0.460 0.399

is- Ipo 2.270 iD- Ido 0.678 0.504

3p2 - 3p4s 3p- 3po 0.147 Ipo 0.974 0.896
Sultana N. Nahar and Anil K. Pradhan 9

0.0

-1.0

-2.0 -U

-3JJ

-5.0 i -7.0

ao - 3.0 -U

-*.0

-OJ

-4.0

OJ

-1.0

u>

-1.0

^

(a) Si(=^)

i.

^ ^

,11

I ""--^^^^^ ^

f : , .

taul

o.is 0.32 a.*9 o.a* Photoeiectron Energy (Ry)

Fig. 1(a)

-U3

-2.0 -

-3.0

-2JJ C. -3J

3- -2.0 z^ -U)

aM -2.0 3

-S.0 -u

-iO

-1.0

-2.0

0.0

-2.0

3«39'{'S)

3»3p'(»

.0 t^l^L-f^v

0 OJ* 1-Q8

^ Photoeiectron Energy (Ry) Fig. 1(c)

Fig.l Partial photoionization cross

ions into various excited states of

-1.0

-2.0

-3.0 -2J

-3J

-3.0

-S.Q

aM -2.0 O

-3.0

-8.0

-Li

-3.0 -OJ

-2.0

0.0

-2.0

QJ

-1.0

1 (b)

" 3pm

" 3*'f('z)

3*^(^)

' siap't*?) .... ,;' , :

; aiap'Cs)

!

1 '

'

i

; 383p'('D) —'

' ' i

'

1

' 1— 1

1 ;1 1 1

I

'

.

1

' ' 1

'

\ Imap'fPJ 1^*^A^^^"' — —

1 , ,

.

toui

0.4 3.8 1.2 1.S Photoeiectron Energy (Ry) Fig. Kb)

-1.0

-2.0

-3.0

-2J3

-XO

-2.0

aM -2.0 3 -U

-3.0

-IJ

-2.0

-OJ

-2.0

-OJ

-2J

(d) Ca'* (^P)

3»3p3<lf r*.*p*1. sp'Cp*)

-I3p'('0*.*n

3»*3<1(*0)

3«3p'('S.»P)

3j3p'('D)

3»3p'rp)

: I 3.'3p('p')

tot»l.

0 0.84 1.88 2J2 3.38 < Photoeiectron Energy (Ry) Fig. 1(d)

sections of the ground state of Si-like

the residual ions.
Large scale radiative and coUisional calculations for Fe n

Sultana N. Nahar and Anil K. Pradhan

Dept of Astronomy, The Ohio State University, Columbus, Ohio 43210

Large scale computations are in progress to obtain radiative data for energy levels, oscillator strengths and

photoionization cross sections, and for collision strengths of Fe II. Calculations are carried out in the close coupling (CQ approximation using the R-matrix method.

We define the atomic or ionic system as (N+1) electron system, and the residual ion or the target as the N-electron system. In CC approximation, the wave function of the (N+1) electron system is expanded in terms

of target states as

^'"^"(E) =A^ X.iT% -H ^C.O., (1)

i=l j=l

where %i(r'l)'s are the target states, and 0i(r)'s are the free electron wave functions, <I>j's are square-integrable

correlation type function for the bound states of the (N+1) electron system, and Cj's are variational parameters.

COLLISIONAL CALCULATIONS: Two sets of CC calculations, (1) a 38-term expansion in LS coupling and

(2) a 41 -level fine structure calculations in the Breit-Pauli ^proximation have been carried out for detailed

collision strengths, Q, including resonance structures. The first set includes the quartet and sextet terms and Q's

for 703 transitions in LS coupling are obtained. The second set includes a number of important fine structure levels from the quartet and sextet multiplets and ii's for 820 transitions are obtained. The autoionizing

structures enhance the background significantly. Computations are under progress now to carry out collision strengdi calculations using the 38-state LS exapnsion split into 142 J values for fine sructure transitions by

algebraic transformations. This will result in collision strengths and rates for about 10,000 fine structure

transitions of Fe II. RADIATIVE CALCULATIONS: The complication in computation of Fe II radiative data arises because of large

number of closely spaced energy levels of the "target" or residual ion Fe in requiring large CC expansions for Fe

II system. Studies of effect of correlations were made using several sets of CC expansions. In the present

calculations, a total of 83 Fe III states have been included to carry out CC calculations of Fe II. Table I shows

number of target states, N^^, that are included in CC expansion for each type of symmetry. Nsljt. the number

of SLjt, that form bound states and total number of corresponding bound states for each type of symmetry of Fe

II are also given in the Table. Photoionization cross secitons are obtained for all bound states. Cross sections for photoionization of 3d^4s ground state of Fe II are presented in Fig. 1. Present calculations are carried out in LS coupling. Table II shows number of oscillator strengths

obtained for allowed bound-bound transitions for each kind of symmetry. The f-values or the oscillator strengths

obtained in LS multiplet are now being converted to fine structure transitions using relative line strength

scheme. The accuracy of fine structure f-values are improved by use of observed energies in JJ. Present results are compared with the observed values^ as well as those of Kurucz^ in Table II.

References:

1. J.R. Fuhr, G.A. Martin and W.L. Wiese, J. Phys. Chem. Ref. Dt. 17 (AIP, 1988).

2. R.L. Kurucz, "Semiempirical calculation of gf values: Fe 11", Smithsonian Astrophysical Observatory

Special Report 390 (Cambridge, 1981).

Table I: N^c is the number of target states in the CC expansion, f^^Ln ^ number of bound symmtries and

N^j^jj is the corresponding number of bound states (n < 10, 1 < 7). Nf is the number of oscillator strengths in LS multiplet. * implies partial data from ongoing work.

Symmetry Ncc NsLtc Nbnd Nf Symmetry Ncc NsL;. Nbnd Nf

Octets 2 4 6 8 Quartets 58 19 305 9755

Sextets 21 19 200 4127 Doublets 62 12* 196* 4860*

10
Sultana N, Nahar and Anil K. Pradhan 11

Table H: Fine structure f-values for allowed transtions of Fe II.

Transition 2Jj+l 2Jffl fjf Present (OP) Expt^ (NIST) Kurucz^ (1981)

6d - 6po 0.12633

6j) . 6po

in oo

n 1 0fiA U. 1Z04 nil U.l 1 n 144

oo

QO n ndAO n nsi n n^74

(ioQo n nnoo n n4ni

oo O n nsM n noi n noni o o nW.U0771 III n in n in'^s A O U.Uj / / o

n nil nU.WJ ndn/ A n nfifi7 U.Uoo / n nfl7 nil 17 U. 1 1 J / 2 4 0.1263 0.13 0.194

u.zyJO nu.zo of^ in in n u.zoz in Qo nU.UJ'ro ns48 n n^s n n7'^^ 8o in n nA7^ n m'^ nU.Lr+ n4^fi JO

oooo U. 1 J 1

J

nil n 1 '^^ Co o 0 117 o

Qo nyj, 1948 izHo 0 084 0 088

D o n n4s 0U.UJZ 0'^7 D n 1 1 7^ n 1

1

0 1 '^1 U. 1 J J *A O nU. 1748 1 / to n 17 0 1

'^'^ U. 1 J J

A n nn'?9 n nn'^7 n nn4

n 1 144 n in 0U. 11 1Q17

A

*r 0 18 0V/. 11 87o / ^ n nso 0 0S9

0.3976

10 12 0.3425 0.37

10 10 0.0527 0.028 0.038

10 8 0.0043

8 10 0.2888 0.27 0.349

8 8 0.0968 0.089 0.100

8 6 0.0122

6 8 0.2431 0.20 0.287

6 6 0.1313 0.12 0.142

6 4 0.0227 0.019 0.019

4 6 0.2031 0.19 0.249

4 4 0.1610 0.14 0.181

4 2 0.0314 0.031 0.0316

2 4 0.1747 0.19 0.216

2 2 0.2199 0.21 0.254

* This woik is being carried out on the Cray Y-MP at the Ohio Supercomputer Center and is supported partially

by a grant from NSF (PHY- 91 15057).
12
Calculation of Oscillator strengths in Hg III

P. H.M. Uylings^^^ A . J . J . Raassen^^ \ A. A. Joueizadeh^^^

J.O. Ekberg^^\ Se. Johansson^^^ and J.-F. Wyart^^^

Van der Waals-Zeemanlaboratorium, Universiteit van Amsterdam,

Valckenierstraat 65-67, 1018XE Amsterdam, The Netherlands

Atomic Spectroscopy, Department of Physics, University of

Lund, Solvegatan 14, 223 62 Lund, Sweden

'•^^ Laboratoire Aime Cotton, CNRS II, Bat 505, Centre

Universitaire, 91405 Orsay, France

Abstract

Log(gf) values for the 5d^°+5d'6s + 5d®6s^ - 5d'6p+5d^6s6p transition

array of Hg III have been calculated by means of several methods.

Eigenvectors of the even and odd systems are obtained from

diagonaliz ing a model-Hamiltonian . The radial factors in the

Hamiltonian are either taken from ab initio calculations

(HXR,HFR) or treated as parameters (fitting the eigenvalues

towards the experimental energies) . The angular factors of the

Hamiltonian are either conventional (Slater-Condon) operators

extended with effective operators using Cowan's programs, or

orthogonal operators the associated parameters of which have a minimum correlation. The results of the various approaches are

compared to each other.

Introduction

The development of Space laboratories, like lUE and HST, has on

the one hand side enlarged the accessibility of the wavelength

region in the vacuum ultra violet while on the other hand the

resolving power of astrophysical observations has increased

tremendously. This calls for more and accurate data in the VUV

region for all elements of stellar interest. Traditionally, the

emphasis lies on the lighter elements but recent observations by

the Hubble Space Telescope have indicated very clearly the

presence of heavy elements, as Pt and Hg (belonging to the 5dsequence) , in stellar objects, e.g. x Lupi [1]. These new

developments imply the need of accurate data of the heavier

elements, which up to now were hardly considered to be of

astrophysical interest. It concerns here especially the lower

ionization stages: the I-, II- and Ill-spectra, with a nuclear

charge of about 80. Recently the spectrum of Pt III was analyzed

by Ryabtsev etal [2], while the analysis of the spectrum of Hg

III was extended to higher configurations [3]. For the latter

log(gf) values have been calculated and are presented in this

poster

.

13
14

Methods of calculation

The log(gf) values have been calculated in four ways. All four

are based on the principle of parametric fitting to experimental

level values. Two of them (marked 'HXR' and 'HFR') are obtained

from coefficient files produced by Cowan's programs [4]. Both the

transition integrals and the interaction integrals ( 5d5d , 6s6s)

and R^ ( 5d5d, 5d6s) [the latter scaled down to 80% of their

original value], have been calculated by means of Cowan's program

in the Hartree-plus-statist ical-exchange (HXR) as well as in the

Hartree-Fock (HFR) mode including relativistic corrections to the

wavefunctions . The values of the interaction integrals were

subsequently fixed in the fitting procedure. The other parameters

were free to vary. Therefore the difference between the two fits

is a result of the different values for the interaction

integrals. The eigenvector compositions obtained from the fits

were used to calculate the log(gf) values, with HXR or HFR radial

transition integrals, respectively. For both calculations the

interaction of the even configurations (5d^°, Sd'es and 5d®6s^) was

included while for the odd parity a single configuration approach

(i.e. only 5d'6p) was applied.

The two other fits were carried out with an orthogonal operator

set [5], including the configuration interaction of the three

even configurations. Unless enlarged with additional operators

for higher order magnetic or correlation effects, this set gives

in principle a description equivalent to the Cowan set or the

Slater Condon set. However, the orthogonal set is more stable in

the fitting procedure and therefore more suited to extend with

operators that describe smaller effects. In the even system (i.e.

Sd'ss) , our orthogonal operator set was extended with the

Electrostatic Spin-orbit parameter Amso. Next to the usual spin

orbit coupling constant this parameter describes the strength

of the operator s^^.l^^. In the odd system the parameter set is

enlarged with the pendants of the Amso, Z3 and Z^, which give the

strengths of the operators s^^.l^p and s^p.l^^. Using the orthogonal

operator set two calculations were made; one without and one with

the interaction with the 5d®6s6p configuration.

For the sake of completeness the results of an ab-initio

calculation, using Cowan's program in the relativistic mode is

given

[1] D.S. Leckrone, G.M. Wahlgren and Se. Johansson, Astrophys.

J. Letters 373, L33 (1991)

[2] A.N. Ryabtsev, J.-F. Wyart, Y.N. Joshi, A.J.J. Raassen and

P.H.M. Uylings, Phys. Scripta (submitted)

[3] J.-F. Wyart, A.J.J. Raassen, Y.N. Joshi and P.H.M. Uylings,

Journ. de Physique 2, 895 (1992)

[4] R.D. Cowan, The Theory of Atomic Structure and Spectra,

University of California Press 1981

[5] J.E. Hansen, P.H.M. Uylings and A.J.J. Raassen, Phys. Scripta

37, 664 (1988)

J.E. Hansen, A.J.J. Raassen, P.H.M. Uylings and G.M.S.

Lister, Nucl. Instr. Meth. Phys. Res. B35, 134 (1988)
p. H. M. Uylings et al. 15

Xv.c(A) lO; HXR HFR

3090.93

2725.23

2481.39

2354.95 -1.926 -1.903

2245.07 -1.884 -1.863

2215.15 -2.931 -2.908

1740.27 -0.560 -0.581

1738.53 -0.802 -0.778

1738.47 -0.573 -0.536

1677.90 0.176 0.200

1671.06 -0.247 -0.224

1662.73 -0.341 -0.318

1661.09

1652.45 -1.511 -1.490

1647.47 0.222 0.245

1599.44 -0.206 -0.183

1592.93 0.023 0.046

1527.40 -0.115 -0.147

1467.34 -0.644 -0.620

1383.19 -0.360 -0.336

1378.96 0.109 0.132

1377.83 -0.013 0.010

1360.50 0.479 0.503

1352.94 -0.676 -0.653

1335.14 -0.162 -0.137

1330.77 0.607 0.631

1326.38 0.101 0.124

1323.23 0.088 0.111

1321.04 -0.946 -0.923

1305.60 0.048 0.071

1280.85 -0.009 0.014

1280.78 -0.970 -0.945

1269.81 0.296 0.319

1241.82 -0.480 -0.455

1129.20

1123.98

1105.59

1090.06

1068.05

843.12 -1.322 -1.383

790.16

740.75

(gO

OFIS OFII ab-in

-3.624 -2.939 -3.289

-2.174 -2.125

-4.923 -3.498 -3.464

-1.856 -1.753 -1.668

-1.717 -1.597 -1.436

-2.895 -2.872 -2.733

-0.901 -0.994 -2.456

-0.907 -0.881 -1.220

-0.589 -0.552 -0.732

0.183 0.228 0.248

-0.173 -0.100 -0.071

-0.429 -0.447 -0.805

-3.008 -3.406 -2.039

-1.282 -1.213 -1.110

0.235 0.288 0.309

-0.144 -0.089 0.046

0.030 0.056 0.023

-0.140 -0.096 -0.054

-0.615 -0.581 -0.498

-0.351 -0.292 -0.288

0.183 0.257 0.359

0.007 0.065 0.109

0.486 0.531 0.526

-0.672 -0.636 -0.594

-0.278 -0.258 -0.755

0.620 0.658 0.661

0.107 0.170 0.198

0.089 0.124 0.080

-0.972 -0.869 -1.045

0.058 0.111 0.087

0.010 0.051 0.013

-1.115 -1.094 -1.616

0.311 0.368 0.390

-0.517 -0.497 -0.832

-0.962 -0.949 -0.701

-1.216 -1.258 -1.027

-1.318 -1.265 -1.192

-2.045 -1.921 -1.798

-1.919 -1.969 -1.729

-1.393 -1.327 -1.052

0.030 0.030 -0.018

-0.576 -0.587 -0.473

Even Lev Odd Lev

0 158909 1 126556

4 97893 3 134588

0 158909 1 118607

2 61085 2 103549

2 61085 3 105627

1 58405 2 103549

2 61085 2 118548

2 46029 2 103549

2 61085 1 118607

2 46029 3 105627

2 61085 2 120927

1 58405 2 118548

1 58405 1 118607

2 61085 3 121602

3 42850 2 103549

1 58405 2 120927

3 42850 3 105627

2 61085 1 126556

1 58405 1 126556

1 58405 0 130702

2 46029 2 118548

2 46029 1 118607

2 61085 3 134588

2 61085 1 134998

2 46029 2 120927

3 42850 4 117994

2 61085 2 136479

2 46029 3 121602

3 42850 2 118548

1 58405 1 134998

1 58405 2 136479

3 42850 2 120927

3 42850 3 121602

2 46029 1 126556

2 46029 3 134588

2 46029 1 134998

2 46029 2 136479

3 42850 3 134588

3 42850 2 136479

0 0 1 118607

0 0 1 126556

0 0 1 134998

OFIS: Orthogonal fit, even system with configuration interaction, odd system without

configuration interaction

OFII: Orthogonal fit, configuration interaction included in the even as well as the odd system
Transitions in neutral chromium

D.J.R. Robinson and A. Hibbert

Department of Applied Mathematics and Theoretical Physics, Queen's University,

Belfast, BT7 INN, N. Ireland.

Introduction

Knowledge of the oscillator strengths in neutral chromium is required for impurity

diagnostics in the JET plasma, in particular for the transitions

^ 3dUs-ip y'^^P''

A CI calculation of the septet transitions was undertaken b)' Hibbert ei al [l]. Quite

good agreement with experiment was obtained for the oscillator strength of the a — z transition, and between the length (//) and velocity (/^. ) forms. But for the a — y

transition, /; and differed by 30% (though the geometric mean of the two agreed

well with experiment).

Present work

One of the major difhcidties in obtaining accurate oscillator strengths for the septet

transitions is that the radial functions of the 3r/ and 4/) orbitals vary considerably from

state to state. A more accurate representation of these transitions would be

3J^46 a'-^S — 2dUp2 ='-''P''

where different subscripts denote different but not orthogonal orbitals. For singly

occupied orbitals such as 4p, it is in principle quite a simple matter to write 4p3 as a

linear combination of 4;>2 fincl another y>function (which below we label 5p) orthogonal

to 4p2. Hence the difference between the Ap functions for different states can be treated

by conventional orthogonal CI. Howe\er. in the case of multiply occupied orbitals

such as the 3d orbital in these transitions, linear combinations of different J-orbitals

would require very extensive CI (because of the many angular momentum couplings

of the open f/-subshells). Moreover, some electron correlation would also be effectively

introduced, though not in a systematic way. Thus, in calculation D of [l], with the

3d function determined as 3^/3, the configuration 3f/'4f/4p was included to act as a

first-order correction to 3d^Ap, i.e. to 3d2 being different from 3c/3. This configuration

also partially incorporates 4^ — 4d correlation in the y ' P° state. Prior to embarking on a non-orthogonal orbital approach to this problem, we have

undertaken a series of calculations with the code CIV3 [2] in which the orthogonal

orbitals arising in the configurations are optimised in different ways on the energies of

different states, and again in which various choices of configurations are employed.

We show in Table I two such calculations. Calculation 1 coincides with Calculation D of [1]. The orbitals are represented as sums of normalised Slater-type orbitals

(STOs). Those which differ in the two calculations were chosen as follows. In CcJculation 1, 3d was first fixed as the Hartree-Fock orbital of 3f/^45^ ^D, after which the

id and 5p were optimised of a' S and y' P° respectively. The 3d was then reoptimised

16
D. J. R. Robinson and A. Hibbert 17

on y' P°. Finally, the coefficients of the STOs of 4d were recomputed to ensure or- thogonality of 3d and Ad. In Calculation 2, the same configurations were used as in

Calculation 1, but 3d, 4d, 5p were optimised on ij' P°, a' 5, i/' P° in thai order. The

CI expansion coefficients do not differ greatly in the two calculations: typically by less than 5%.

In order to compare the contributions to the oscillator strength from individual

configurations, it is convenient to define for the length form

^'^ = [1—) a,b,mv\x,)\

(with an equivalent expression for the velocity form) in terms of the CI wave functions

of the two states in the transition:

> J Then, in either form, the oscillator strength is

Table I. F,j and /-values for septet transitions

a a - y

Calc. 1 Calc. 2 Calc. 1 Calc. 2

i // A. // /. // f. // /.

3d^4s 3d^Ap 0.758 0.718 0.748 0.729 0.555 0.440 0.594 0.483

3(i-'454p -0.098 -0.319 -0.104 -0.350 0.163 0.447 0.160 0.450

3f/-'455;) -0.034 -0.158 -0.038 -0.216 0.038 0.150 0.039 0.186

3f/'*454/ -0.013 -0.154 -0.013 -0.151 -0.017 -0.162 -0.018 -0.178

3d'^idAs 3^i'*454p -0.120 0.116 -0.098 0.095 0.201 -0.163 0.150 -0.122

3f/-'455p -0.003 0.070 -0.006 0.078 0.004 -0.070 0.007 -0.067

3dUd4p 0.112 0.106 0.087 0.085 0.075 0.059 0.064 0.052

3dUlAf 3(fMp -0.015 0.178 -0.015 0.178 -0.011 0.109 -0.012 0.118

Others -0.028 0.009 -0.019 0.005 -0.025 0.009 -0.022 0.011

Total F.j 0.559 0.566 0.542 0.453 0.983 0.819 0.962 0.933

/-value 0.313 0.321 0.294 0.205 0.967 0.671 0.926 0.870

Expt. 0.255 [4]; 0.254 [5] 0.884 [4; ; 0.856 [5]

The main F,j are shown in Table I. For the a — : transition, the total in length

form is little different in the two calculations, l)ut in the velocity form the total Fij

changes by 20%. resulting in a 35% change in f^. This is partly due to changes in Ad,

but more to changes in bp, brought about by the way in which the 3d was optimised.

Thus the length and velocity agreement achieved for a — z in Calculation 1 is lost in

Calculation 2. For the a-y transition, the situation is reversed: the poor agreement in Calculation

1 is much improved in Calculation 2, and the resulting // and /„ lie close to the

experimental values.
18

We have made extensive sets of calculations of these transitions, by varying the

way these orbitals are optimised and by increasing the number of configurations. In

ail this work, we find that in any one calculation, we can achieve good agreement with

experiment and between // and for either a — z or a — y, but not for both transitions

simultaneously.

Non-orthogonal approach

Accordingly, we have embarked on a calculation of these transitions using nonorthogonal orbitals. We have incorporated into CIVS the non-orthogonal angular

momentum package of [3] and have made the necessary (and extensive) changes to the

radial part of the code. Calculations of these oscillator strengths in this formalism

have begun and will be reported later.

Quintet transitions

Some calculations have also been made for the quintet transitions, using the same

configurations as, but more angular momentum couplings than, the septet transitions.

This work reveals much less CI cancellation than in the septet transitions. All our

calculations yield results similar to those of Table II. The calculated energies agree

well with experiment, as does the oscillator strength of the a — z transition. Length

and velocity forms agree quite well. However, our oscillator strength for a — y differs

markedly from experiment. The lack of an}- cancellation in a — y suggests that the

experimental value may be too low. A further experimented determination would be

helpful.

Table II. /-vahies for quintet transitions

d - = (L- y

AEla.u.) fi /, A£(a.u.) /, /,

Our work 0.0824 O.GIO 0.5SG 0.0971 0.094 0.105

Expt. 0.0875 0.64 [4] O.IOOG 0.034 [6]

References

1. Hibbert, A., Tait..T.H., Summers, H. P. and Burke. P.G..Nucl. Inst. Meth. B31,

276 (1988).

2. Hibbert, A., Comput. Phys. Commun. 9, 141 (1975).

3. Hibbert, A., Froese Fischer, C. and Godefroid, M.R.. Comput. Phys. Commun.

51,285 (1988).

4. Huber, M.C.E. and Sanderman, R.J.. Proc. Roy. Soc. A357, 355 (1977).

5. Blackwell, D.E., Menon, S.L.R. and Petford. A.D., Mon. Not. R.A.S. 207, 535

(1984).

6. Penkin, N.P., J. Quant. SPect. Rad. Transf. 4, 41 (1964).
RCI calculation of energy levels and oscillator

strengths in highly ionized atoms

Takashi Kagawa, Yoshie Honda and Shuji Kiyokawa

- Department of Physics, Nara Women's University

Nara 630, Japan

Structures for highly ionized atoms have attracted interest not only in rel- ativistic atomic physics but also other related fields such as astrophysics and

plasma physics. X-ray spectra emitted from highly ionized atoms immersed

in various plasmas such as solar, stellar and laboratory ones have been used

for diagnosing and modelling them. However, these spectra observed usually

are very complex because they consist of a large number of lines due to multiplet terms in the energy levels for ions in various charge states. So in the

analysis of such complex spectra, it is desired to calculate transition energies

and oscillator strengths for ions systematically.

Recently we have developed the relativistic configuration interaction (RCI)

theory for atomic systems with analytical relativistic Hartree-Fock-Roothaan

(RHFR) basis functions [1]. The basis set for constructing configuration

state functions (CSF's) consists of all real and virtual RHFR one-electron

functions expanded in terms of Slater-type orbitals. The Breit interaction

operator is treated by the first-order perturbation theory. The lowest-order

quantum electrodynamics (QED) corrections for the self-energy and vacuum

polarization terms are taken into account in the RCI calculation as a first- order perturbation energy by use of Mohr's numerical results for hydrogenic

systems [2,3]. Present RCI method has a merit that one can save much computation time when obtaining a large number of multiplet states in atomic

systems because of an analytical form of the basis set. The numerical application of the method to neonlike systems is carried

out to see the effectiveness of the theory. Here we show the calculated results

on the Z dependence of the transition frequencies and oscillator strengths

for the E\ transition from the ground state to singly excited ones in neon

isoelectronic sequence. In Fig. 1, the variation of the order of the excited

levels for odd-parity states with J = 1 in the isoelectronic sequence is shown.

19
20

It is seen from the figure that many level crossings apprear when Z increases.

In Fig. 2 and 3, variation of the oscillator strengths for the n = 2 —+ 3 and

n = 2 —> 4 E\ transitions in the isoelectronic sequence are shown. One

sees anormaly in the Z dependent behavior of the oscillator strengths in

which they suddenly increase or decrease in a position of a specific atomic

system with Z. If one compares Fig. 2 and 3 with Fig. 1, the anormaly

can clearly be explained as the CI effects in the oscillator strengths, since one can find in Fig. 1 that the level crossing for excited levels related to the

transitions under consideration occurs at a position close to a specific ion

in the isoelectronic sequence so that the wavefunctions between these states

in the system mix largely. The atomic data containing such Z dependent

behavior for the transition frequencies and optical oscillator strengths will

be very useful in the identification of the spectra observed.

References

[1] T. Kagawa, Y. Honda and S. Kiyokawa, Phys. Rev. A44, 7092 (1991).

[2] P. J. Mohr, AT. Data and Nucl. Data Tables 29, 453 (1983).

[3] P. J. Mohr and Y.-K. Kim, Phys. Rev. A45, 2727 (1991).

20

liJ >

Ul

15 Q

liJ H

O

X

UJ

u.O

cc

liJ Q

DCO

10

10 20 30 40 50 60 z

70 80 90

2s-»5ps«

2s-»5pi/»

2pi/2-»5dj/i

2pi/a-»5s

23-*'1pi/i

2s->4pi/a

2pt/j-»4di/t

2pi/2-»4s

2pi/a-»5dwj

2p3y«-»5dj/i

2pi/»-*53

2pj/a-»4d«;»

2pj/i-»4dj/»

2s-*3p3/i

2pi;r-43

2pt/»-»3d3/a

2s-»3pi/t

2pi/a—3S

2pi«-*3d5/i

2pa/a—3dj/i

2pj/a-*3s

100

Fig. 1 Order of odd parity states with J=1 in Ne-like systems.
Takashi Kagawa et al. 2

Z

Fig. 2. Oscillator strengths for n=2-3 transitions in Ne-like systems.

Fig. 3. Oscillator strengths for n=2-4 transitions in Ne-like systems.
A DENSITY-MATRIX DESRIPTION FOR THE

BROADENING OF SPECTRAL LINES BY AUTOIONIZATION,

RADIATIVE TRANSITIONS, AND COLLISIONS*

V. L. Jacobs

Complex Systems Theory Branch, Code 4694

Condensed Matter And Radiation Sciences Division

Naval Research Laboratory

Washington, D. C. 20375-5000

ABSTRACT

A density-matrix description has been developed to investigate the

broadening of atomic spectral lines by autoionization processes, radiative

transitions, and electron-ion collisions in a high-temperature plasma. Using

Liouville-space projection-operator techniques, collisional and radiative

relaxation processes are incorporated on an equal footing with

autoionization and radiative stabilization. Particular interest is directed at

the precise determination of the spectral line shapes for dielectronic

recombination satellite transitions.

* SUPPORTED BY THE DEPARTMENT OF ENERGY

22
Developments in computation of form factors

C. T. Chantler

Quantum Metrology Division, National Institute for Standards and Technology,

Gaithersburg, MD 20899, U.S.A.

Abstract

Imaginary parts of atomic form factors axe scaled total photoionisation and photoexcitation cross-sections. This relates directly to summed oscillator strengths for the excitation to continua or bound states for levels involved. Hence calculations of form factors,

oscillator strengths and absorption edge energies are intrinsically related. Form fax:tors are the fundamental unit in calculations of diffraction effects and shifts, involved in most

X-ray spectral analysis, which is a further incentive for investigation.

Tables for form factors and anomalous dispersion are of wide generaJ use in the UV,

X-ray and 7-ray communities, and have existed for several decades. They have, perhaps,

been dominated by the theoretical work of Cromer, Mzinn and Liberman (1968, 1970a,

1970b, 1981) and the experimental syntheses of Henke and co-workers (1982), with recent

developments of Doolen and Liberman (1987) and Henke et al. (1988). The generality

of these works has entsiiled numerous simplifications compared to detailed relativistic Smatrix calculations (Kane, 1986). However, the latter calculations do not appeair to give

convenient tabular application for the range of Z and energy of general interest, whereas

the former tables have large regions of limited validity throughout the range of Z and

energies, and in particular have limitations with regard to extrapolation to energies outside

tabulated ranges.

Several a priori assumptions limit the applicability of theoretical form factor computations. Chief of these is the independent particle approximation, treating adjacent atoms as independent and effectively restricting consideration to 10 eV - 100 eV and higher energies.

However, intermediate theoretical and procedural a.ssumptions further limit the precision

and applicability of available tabulations and procedures. This poster identifies regions of

Z and energy where these secondary assumptions fail and the improvement which can be

achieved by their avoidance, both in tabulated ranges and by extrapolation.

Particular concern involves the application of the dispersion relation to derive Re(/)

from photoelectric absorption cross-sections. Revised formulae can lead to significant qualitative and quantitative improvement, peirticularly above 30-60 keV energies (Fig. 1), near absorption edges (Fig. 2), or at 30 eV to 6 keV energies (Fig. 3). Current experimental

syntheses are not superceded by this approach, but examples Eire given where predictions underlying revised theoretical tables are in qualitative agreement with experiment

23
24

as opposed to results in available syntheses. Recent theoretical discussion involving small

corrections to earlier form factors are confused if the relatively large corrections discussed

herein axe not included.

References:

Brennan S. (1991) private communication.

Cromer D. T. and Liberman D. (1970a) J. Chem. Phys. 53, 1891-1898.

Cromer D. T. and Liberman D. (1970b) Los Alamos internal report LA-4403 UC-34,

163 pages.

Cromer D. T. and Liberman D. A. (1981) Acta Cryst. AST, 267-268.

Cromer D. T. and Mann J. B. (1968) Acta Cryst. A24, 321-324.

Doolen G. and Liberman D. A. (1987) Physica Scripta 36, 77-79.

Henke B. L., Lee P., TanaJca T. J., Shimabukuro R. L., Fujikawa B. K. (1982) At.

Dai. Nucl. Dat. Tab. 27, 1-144.

Henke E. L., Davis J. C, Gulhkson E. C, Perera R. C. C. (1988) Lawrence Berkeley

Laboratory report LBL-26259 UC-411, 376 pages.

Kane P. P., Kissel L., Pratt R. H., Roy S. C. (1986) Phys. Rep. 140, 75-159.

Perera R. C. C. and Gulliksen E. (1991) private communication.

110.0

105.0

100.0

95.0

o

• 90.0

85.0

80.0

75.0

70.0

*

, 1 . T^T-

'

! : ' 1 «

* }

* } '

1 a

• ' •

i' •

t ' *

r U L edges U K edge

i' " II ,1 t>

1

t * •'J

; ^

;

I, •

s

'.

s

\

'

\

1

\

\ "

\ ;

1 :

1

1

1

i

10* 10»

E (eV)

Figure 1: Form factor f\ for uranium near K and L-edges indicating aboveedge errors from standard formulae (Cromer et al., 1970a, 1970b, 1981; Brennan, 1991). (Solid line indicates revised formulation.)
C. T. Chantler 25

Figure 2: Form factor /i for carbon near K-edge indicating asymmetry

and discontinuity produced by standard formulae (*o% Cromer (1981)), and

inadequacy of synthesised data (dash, Henke (1982); triangles, Perera (1991)),

versus the revised formulation (*+').

Uranlump Zs92, effect of integration precision

83.0

69.0

Cromer (1981)

Henke (1988)

revlMd 5-polnt

- - - revised 10>polnt

revised 16«polnt

4200 4400 4600 4800 5000 5200 5400 5600

E (eV)

Figure 3: Form factor /i for uranium M/ - M/// edges showing importance

of higher precision integration and the use of revised formulae versus earlier

methods (Cromer, 1981) and synthesised data (Henke, 1988; Perera, 1991).
Accurate oscillator strengths for neutral carbon

and astrophysical implications

E. BieInont^ A. Hibbert^, M.R. Godefroid^ and N. Vaeck''

1 Institut d'Astrophysique, University of Liege, B-4000 Liege, Belgium.

2 Department of Applied Mathematics, Queen's University, Belfast, N. Ireland.

3 Laboratoire de Chimie Physique Moleculaire, CP 160/09,

Universite Libre de Bruxelles, B-1050 Bruxelles, Belgium

4 van der Waals-Zeeman Laboratory, University of Amsterdam,

NL-1018 XE Amsterdam, The Netherlands

The calculation

Recently we embarked on a major study of transitions in neutral carbon, nitrogen

and oxygen in order to provide a new determination of the solar content of these el- ements. Our transition probabilities in N I and 0 I [l] were used [2] to obtain solar

abundances which were in excellent agreement with those obtained from an investigation of molecules in the Sun [3]. We have very recently completed a similar calculation of transition probabilities in

C I [4]. The determination of the solar abundance of carbon is in progress [5]. CI is observed in the visible part of the solar spectrum but appears predominantly in the

infrared region. Consequently it is necessary to consider all states of the form 2s^2p^,

2^2p3, 2s^2p?>l (/=0,1.2). 2s^2iA} (/=0, 1,2.3), 2s^2pbs.

The calculation of transition probabilities was undertaken using the configuration

interaction (CI) code CIV3 [6] with an extensive set of orbitals whose radial functions,

chosen to represent both spectroscopic and correlation orbitals, were optimised variationally on the energies of various different LS states. The details are given in ref. [4]. The 57 even and 76 odd parity configurations gave rise to a total of over 4000 LSJ

couplings. This calculation is then much more extensive than the earlier structure

calculation of Nussbaumer and Storey (NS) [7]. Oscillator strengths of C I have also been obtained from close coupling (CC) cal- culations by Nussbaumer and Storey [7] and more recently by Luo and Pradhan (LP)

[8] using the R-matrix method.

Discussion of the accuracy of LS oscillator strengths

It is appropriate to compare our results with the above-cited calculations in order

to assess their accuracy. We give in Table I those of our Z5-coupled results for which

comparison is possible for the principal transitions contributing to the carbon abundance calculation. Oscillator strengths are calculated in length (//) and velocity (/i,)

forms. LP also give both forms, whereas NS give only the length form.

It is clear that our length values agree very closely with the SUPERSTRUCTURE

(SS) length values of NS. Hence, with two quite independent atomic structure codes,

very good agreement is achieved. The coUisional calculations yield length values which

are generally in good agreement with the structure calculations, but there are some

exceptions.

26
E. Biemont et al. 27

Table I. Multiplet oscillator stren^rtllS This work LP- NS(CC)t NS(SS)t

// // /. // fi 3^ — 3p 3po_3£) 0.536 0.507 0.497 0.548 0.507 0.526

3 po 3 p U.O ( O U.OOD 0.360 0.371 0.356 0.375

3po_3 5 0.113 0.081 0.10 1 0.109 0.10 < A 1 1 A 0.110

lpo_l£) 0.656 0.709 0.637 0.672 0.624 0.657

1 po_\

p

0.277 0.201 0.252 0.271 0.267 0.278

ipo_i5 0.125 0.105 0.121 0.120 0.117 0.122

3p - 3d 3 n 3 no n 7Q7 nu.ouy )5nQ 0.813 0.677 0.783 0.787

2p)_3p)0 0.142 0.131 U.149 O.lOb 0.143 A "1 ^ 1 0.141

3p_3po 0.301 0.276 0.301 0.232 0.265 0.304

1 p_\ po 0.336 0.297 0.316 0.0243 0.301 0.332

0.348 0.321 0.501 0.314 0.591 0.380

3p — 4s 3p)_3po 0.154 0.138 0.162 0.128 0.161 0.159

l/)_lpo 0.232 0.220 0.227 0.195 0.250 0.226

lp_lpo 0.0066 0.0069 0.0233 0.0303 0.0510 0.0106

•: Ref. [8] t; Ref. [7]

In particular, the 3p — 4s transition is a weak transition with some cancellation due to the CI mixing of 45 and 3d states, and the oscillator strength is very

sensitive to the accuracy of that mixing. We note that, when we include relativistic

effects, our // and each increase from 0.007 to 0.009. This variation is small compared with the discrepancy between the various theoretical results. In our calculations,

we made small adjustments to the diagonal elements of the Hamiltonian matrix, in

order to reproduce experimental energy separations and thereby refine the CI mixing

coefficients. This does not seem to have been done in the other calculations.

It is more surprising to find the structure and collisional calculations disagreeing for

the length form of the 3p ^ S — 3d ^ P° transition, which has a large oscillator strength.

The same 3d — 4s mixing which led to cancellation effects in the transition considered

above gives rise to an enhancement of the oscillator strength in this case. Normally

such enhancement situations are rather insensitive to the accuracy of the mixing.

However, we note that in some rather simple CI calculations we have made for other

purposes, the oscillator strength of this particular transition can vary markedly from

what we believe is a reasonably accurate value as given by our result in Table I. The other possible comparison is between length and velocity forms. From Table

I, we see that for the 3^ — 3p transitions, the agreement between // and is better in

the calculations of LP than in ours. However, for the 3p — 3d and 3p — 4s transitions, our results show much better agreement than theirs.

./-dependent effects

The calculations of LP are in LS coupling. We find that for some transitions, there

are substantial departures from the standard statistical weight dependence of the J — J'
28

lines in a multiplet. We show in Table II the A- values of individual lines in the 2p^

^P — 2p4s '^P° multiplet, comparing our values ("actual") with what would be obtained

if our LS A-value of 9.17 x lO^s"^ were distributed according to ''statistical" factors.

The "ratio" column shows that the inclusion of spin-orbit mixing, principally that of

2p4s and 2p3d (which lie close in energy), both reduces the "multiplet" value

and also creates substantial deviation from the "statistical" values.

Table II. Transitions in the 2p^ - 2p4s ^P" multiplet

A- values (in lO^s"^)

J J' Actual Statistical Ratio

2 2 0.616 0.688 0.90

1 2 0.321 0.229 1.40

2 1 0.348 0.382 0.91

1 1 0.183 0.229 0.80

0 1 0.334 0.306 1.09

1 0 0.845 0.917 0.92

Acknowledgements

It is a pleasure to thank Dr. W.L. Wiese for his interest and critical analysis of our results. The Belgian National Fund for Scientific Research (FRFC Convention

2.4533.91) and NATO (Collaborative research grant CRG 890225) are acknowledged

for their financial support.

References

1. Hibbert, A., Biemont, E., Godefroid, M.R. and Vaeck, N., Astron. Astrophys.

Suppl. Ser. 88, 505 (1991); J. Phys. B. 24, 3943 (1991).

2. Biemont, E., Froese Fischer, C. Godefroid, M.R., Vaeck, N. and Hibbert, A.,

Atomic Spectra and Oscillator Strengths for Astrophysics and Fusion Research^

(ed: J.E. Hansen). 59 (1990); Biemont, E., Hibbert, A., Godefroid, M.R., Vaeck,

N. and Fawcett, B.C., Astrophys. J. 375. 818 (1991).

3. Grevesse, N., Lambert, D.L.. Sauval, A. .J., Van Dishoeck, E.F., Farmer, C.B.

and Norton, R.H., Astron. Astrophys. 232, 225 (1990); Astron. Astrophys.

242, 488 (1991).

4. Hibbert, A., Biemont. E., Godefroid, M.R. and Vaeck, N., submitted to Astron.

Astrophys. (1992).

5. Biemont, E.. Hibbert, A.. Godefroid. M.R. and Vaeck, N., to be submitted to

Astrophys. J. (1992).

6. Hibbert, A., Comput. Phys. Commun. 9, 141 (1975); Glass, R. and Hibbert,

A., Comput. Phys. Commun. 16 19 (1978).

7. Nussbaumer, H. and Storey, P.J., Astron. Astrophys. 140, 383 (1984).

8. Luo, D. and Pradhan, A.K., J. Phys. B. 22, 3377 (1989).
Relativistic study of lifetimes for the

ns2np^(n+l)s levels in heavy systems

Jacek R. Bieron

Institute of Physics, Jagelloniaii University

30-059 Krakow, Reymonta 4. Poland.

Jacek Migdalek

Institute of Physics and Computer Science

Pedagogical Academy. 30-084 Krakow. Podchora/ych 2. Poland.

We report on the theoretical study of El transitions from the levels

of ns^np^(n+l)s configurations in heavy systems. The following

spectra are analysed: Gel, SnI, Pbl. AsIL Sbll. Bill for k=2; Asl,

Sbl. Bil for k=3 and Sel, Tel, Pol for k=4. Multiconfiguration DiracFock computer code of Oxford group /I/ has Ix-en used to obtain

wavefunctions and energy structure. The multiconfiguration basis

set includes configurations from within the Layzer complex as well

as several additional configurations, whose considerable interaction

with the reference configuration had been established earlier.

Various options of MCDF code has been tested and their influence on the calculated electronic structure and radiative properties has been analysed. These include the possible choice of energy

functional to be minimized, the model of the nucleus and the QED

corrections /2/.

29
30

The modification of configuration interaction api)roach proposed

recently /3/ has been employed. It is. basically, a combination of the

standard multiconfiguration (MCDF) method with the configuration

interaction (CI) approach. The attempt is made to Ix-nefit both from

more accurate MCDF formulation and from relati\ ('ly fast and easily

convergent CI approach.

The computed lifetimes have been compared with other available

theoretical and experimental data.

1. Grant LP., McKenzie B.J., Norrington P.H.. Ma\ers D.F.,

Pyper N.C., 1980 Comput. Phys. Commun. 21. 207

2. McKenzie B.J., Gr mt LP., Norrington P.H..

1980 Comput. Phys. Commun. 21, 233

3. Bieroh J.R., Marcinek R., Migdalek J.. 1991 J. Phys. B: At. Mol. Opt. Phys. 24. 31
Oscillator strengths for the transitions in singly ionized KrII

P Anantha Lakshmi* and K S Baliyaii'

*ScHOOL OF Physics, University of Hyderabad, Hyderabad 500 134, INDIA

^Laboratory for Astronomy and Solar Physics

NASA/Goddard Space Flight Center, Greenbelt Md 20771

Owing to its application in defining the unit of length 'meter', the neutral krypton at- tracted a lot of attention resulting in considerable amount of atomic data in the form of

energy levels, collision cross sections etc. The motive was to determine a set of energy levels

of Kr®^ that could be used to estabUsh a set of standard wavelengths. Relatively less attenion was focussed on ionized krypton as opposed to the neutral krypton. The spectrum of singly

ionized krypton was analysed as early as in 1933 by de Bruin et al.[l], followed by Boyace[2]

and Minnhagen et al.[3] and Bredice et al.[4]. Most of these levels have been tabulated by

Sugar and Musgrave [5]. Here we intend to present preUminary results of the calculation of

oscillator strengths among the various levels of Kr II ion.

The oscillator strengths and lifetimes of the ions of krypton are of considerable importance

for their appHcation in astrophysics, laser and plasma physics. In this study we use configuration interaction wavefunctions to calculate f- values for some transitions. The wavefunctions

are generated by making use of atomic structure program written by A Hibbert [6] which incorporates electron correlation effects via configuration interaction. These CI wavefunctions

may be expressed as, m

^,{LS) = J2a,,M<^,LS) (1)

1=1

in the LS coupling, or m

*i(J) = E^'i<?^*K^^LiSiJ) (2)

i = l

in the Breit-Pauh approximation. For a given set of {(pi}, the variationally optimal values

of the mixing coefficients aij/bij are the components of the eigenvectors of the Hamiltoinian

matrix. The configuration state functions {4>i} are built using the one electron orthogonal

orbit als:

Unlm,m,{r) = i P.; ( r jV^' ( ^ . </>),\'"" ( ^ ) (3)

r and radial functions are expressed in analytic form as:

k Pni{r) = ^cyexp{-(ir).

i=l

(4)

31
32

The orbital parameters { c,}, {p,} and are obtained variationally.

We use Is, 2s, 2p, 3s, 3p, 3d, 4s, and 4p orbitals published by Clementi and Roetti [4] for

the ground state 4s^4p^ of the singly ionized Kr II ion. In addition to these, 4d, 4f, 5s,

5p, 5d, 5f and 6d orbitals are used in this calculation, parameters of which are obtained by

the optimization procedure using CIV3 code. In this procedure we minimized the energy of

4p''4(i ^D^ to obtain radial function parameters for the 4d orbital. The 5s orbital parameters were obtained by minimising the energy of 4p'*55 ^P^ while those of 5p were obtained using

4p^5p ^P'' state. The 5d orbital was optimized on the energy of 4p'*5(i ^F^ state. The ground

state energy was used to optimise the parameters of 4f and 5f orbitals. The radial orbital

parameters of 6d orbital were obtained on the ground state keeping 4d and 5d configurations.

Table 1

Transition AE Oscillator strength Trans. Prob.

^ - f au Length Velocity

4s24p5 2po 4s4p« 0.4620 1.4431(-2) 2.3635(-2) 2.9688(8)

AsHpHd 25 0.7781 2.8124(-1) 2.2900(-l) 1.6411(10)

AsHp^bd 25 0.8913 2.8148(-1) 1.7507(-1) 2.1555(10)

isHp^^P)5p ^P° 4:sHp^5d 25 0.1786 1.8697(-2) 1.2467(-2) 5.7456(7)

Asip^bp 0.5634 1.7497(-1) 1.3189(-1) 5.3538(9)

4sHp^^D)bp ^P° AsHpHd 25 0.0110 2.1799(-2) 1.8537(-2) 2.5610(5)

isHp^bd 25 0.1243 1.4458(-1) 8.4774(-2) 2.1533(8)

4s4/5p 25 0.5092 7.5274(-3) 8.2210(-3) 1.8811(8)

4s4/ 25 AsHpHf ^P° 0.4002 6.0631(-3) 5.0257(-3) 1.0402(7)

4g24^5 2po AsHp\^P)Ad 0.6704 1.0601(-1) 9.5208(-2) 9.1844(8)

4sHp\^D)id 0.7487 7.7252(-l) 6.4013(-1) 8.3490(9)

4:sHp^''P)bd 0.8150 3.9959(-2) 3.2391(-2) 5.1170(8)

4sHp^^S)id 0.8486 6.1375(-1) 4.8676(-l) 8.5203(9)

isHp^CD)bd 0.8806 9.4155(-1) 6.5340(-l) 1.4076(10)

AsHp^{^P)4:d 2p 0.6532 3.6733(-3) 3.0360(-3) 5.0351(7)

4sHp\'D)4d 2p 0.7634 4.2599(-l) 3.5138(-1) 7.9771(9)

AsHp'{^P)bd 2p 0.8281 2.2805(-l) 1.8181(-1) 5.0246(9)

AsHp\^D)bd 2p 0.8876 6.5659(-l) 4.3569(-l) 1.6622(10)

4s4/5p ^P 1.2708 1.1930(-4) 1.3898(-4) 6.1906(6)

Now the major problem in applying the confijjuration interaction method Ues in t] choice of the configuration state functions. Since Kr II is an almost neutral open shell ion, one should normally include the three major correlation effects: internal, semi-internal and

all external. However, a very extensive configuration set would result with this prescription

which is prohibitively difficult from the computational viewpoint. We therefore restrict ourselves to keeping a minimum of 1-electron in 4s shell and 3-electrons in 4p shell and use a very limited 'all external' correlation configuration set. A more elaborate set with aU major configurations is still under consideration. It is observed that there is a strong mixing

between the configurational states. In the event of almost equal mixing coefficients coining

from two configurations, it is difficult to label the state. For the relativistic calculation, we
p. Anantha Lakshmi and K. S. Baliyan 33

have included spin-orbit, spin-spin, spin-other-orbit, mass correction and Darwin term of

the Breit-Pauli operator. In the intermediate coupling different LS states couple with large

mixing coefficients for a particular value of J. This mixing allows the transitions which are otherwise forbidden in LS coupling.

These wavefunctions are used to calculate the dipole oscillator strengths for the transitions between the initial and final states of the singly ionized krypton. The expression for

the oscillator strengths in length and velocity forms can be written as

fl' = '-^^^\<%\f:r,\^,>\' (5)

'^9i p=i

where gi = (2Li-rl)(2Si +l) is the statistical weight of the initial state and the summation

is over all the N electrons of the ion. The initial and final states must be of different parity.

The calculations have been performed in both the length and velocity forms of the dipole

operator which should give identical results for allowed transitions in LS coulpling provided

exact wavefunctions are used. For approximate wavefunctions agreement between these two

is a measure of the accuracy of the wavefunctions used. The f- values obtained in the present

calculation for some of the transitions are given in table 1. The details will be presented at the conference.

1. de Bruin TL, Humphreys CJ and Meggers WF 1933 J Res. Nat. Bur. Stand. (US) 11

409.

2. Boyce JC 1935 Phys. Rev 47 718.

3. Minnhagen L, Strihed H and Petersson B 1969 Ark Fys 39 471.

4. Bredice F, Raineu M, Reyna Almandos J And Gallardo M 1988 Spectrosc Lett 21 11

5. Sugar J and Musgrave A 1991 J. Phys. Chem. Ref. Data 20 875.

6. Hibbert A 1975 Comput.Phys.Commun.9 141.

7. Clementi E and Roetti C 1974 At. Data Nucl. Data Tables 14 177.
I

I
Lifetimes-measurements

Transition Probabilities and Line Shapes: Usage and Needs at the University of Illinois

Alexander Scheeline* and Cheryl A. Bye, (Dept. of Chemistry)

1209 W. California St., Urbana, IL 61801

Herman Krier, Jyotirmoy Mazumder, Xiangli Chen, Tom Duffey, Sudhir Tewari, and David Zerkle (Dept. of

Mechanical and Industrial Engineering), Mark J. Kushner (Dept. of Electrical Engineering)

The authors of this paper are consumers of fundamental

atomic and molecular reference data. Assorted

research which uses transition probabilities and other

reference data is presented, highlighting current sources

of information, adequacies and limitations of the data,

and suggesting areas for additional measurement or

calculation.

1. Pulsed Discharge Plasma Diagnostics: Sparks

and Theta Pinches

In pulsed discharges used for elemental analysis,

sampled species are excited by collision with an ambient

plasma (usually argon or helium, but sometimes

nitrogen or air). Excitation varies as a function of

space, lime, support gas impurities, sampled species

identity and concentration, and interactions among

sampled species. If excitation behavior is understood,

internal standard lines can be chosen, interferences

anticipated, and measurement quality assured. Our

work has focused on pulsed discharges in argon, sampling ferrous alloys, copper and its alloys,

aluminum, and aluminum oxide ceramics. Wavelength

and linewidth data are important, but the major

limitation in elucidating the behavior of the plasmas has

been access to adequate transition probability data.

Because of the availability of plentiful and precise

transition probabilities for Mo l\ we have on occasion

used Mo as a proxy for ferrous alloys. Were data

available for Mo II to the same degree as Mo I, this would be an ideal material for study of spark discharges

since both Mo I and Mo II have rich spectra in the UV

and visible spectral regions. NIST 1265 electrolytic iron

is a frequently used sample, because transition probabilities for iron are also readily available^. Copper

and aluminum data are helpful because of the massive

amount of research since 1961 on sparks to their alloys,

and the common use of AI2O3 as a proxy for many

refractory compounds. The most common source is the NIST/CRC tabulation-', now also available in computerreadable form'*.

Typictilly, analyte is excited to a lower temperature than

the support gas. Ar I data in the near UV and visible are now in reasonable order^. Ar II transition

probabilities"''^'^'^ have not been as well characterized,

though new data will appear shortly^. The next step in extending Ar I and Ar II data should be in increasing

wavelength coverage, particularly between 190 nm and

260 nm. Additional highly useful data would come from

a re-examination of Cu I and Cu II, and perhaps a thorough survey of Cr I. With Cr data, together with Fe

and the well-studied Ni system^^, one would be in a strong position to study Ar plasma interactions with

stainless steel. For examining refractory materials, SiOz

can be used^' instead of aluminum, but the spectrum is sparse, meaning that line interferences (of which there

are several with Ar) can reduce the number of useful

lines below that needed to determine if Boltzmann plots are linear.

2. Laser-Supported Plasmas for Space Propulsion

A spin-off from the Strategic Defense Initiative was the design of spacecraft propulsion systems based on large,

orbiting lasers whose output would be used to remotely

heat gases carried by small satellites. The heated gas would then steer the small satellites*^'^^. For this idea

to work, efficient lasers and efficient conversion of light to kinetic energy are necessary. Atomic gases are

preferred, so that energy is not consumed by molecular

internal degrees of freedom. One desires a highly non- LTE system. To date, argon has been the most studied

support species. The comments made about the need

for additional Ar I and Ar II data in connection with

sparks and pinches holds here for many of the same

reasons. While existing data ' ' • are adequate when

experiment bandwidth limits observation to only a few

lines, wider-bandwidth detection becoming available with charge-transfer detectors will facilitate measurements for which adequate supporting data are note available.

3. Laser Cladding of Nb-Al Alloys on Niobium

Substrate .

Laser-ablation is used to create to a plasma of Nb or

Hf, which are then vapor deposited on Nb-Al alloys.

Ideally, one would like to know the absolute

concentration of atomic species in the laser-generated

plasma. This requires knowledge of transition probabilities for both Nb and Hf. Data are available for Nbl^l

4. Laser-Ablation Generation of Nanocrystalline

Powder

Nanocrystalline materials are a current subject of

intense study for their structural, catalytic, electronic,

and optical properties. In our particular case, an

excimer laser ablates Nb and Al targets. The atoms

condense on a collection plate, forming mixed Nb-Al

alloys. In addition to Nb and Al atomic data, molecular

data on Nbz, NbO, NbAb and NbaAl are required. The

literature is devoid of data on any of these species

except NbO, and those data^^'^^'^^ are quite old and

fragmentary. Any data on wavelengths, level identifications, term symbols, and vibration/rotation constants would be an improvement.

37
38

5. Laser CVD of Ti and TiN Films on Si Substrates

Ti and TiN thin films are frequently deposited on Si substrates to serve as transitions for contact bonding or

as dielectrics. Laser decomposition of precursors to

yield free atoms is one means for fabricating the films. Understanding of the deposition process requires

spectral diagnostics of numerous species including Si, Ti, Br, CI, N, N2, TiN, Br2, CI2, TiBrx and TiClx where x = 1 to 4. While some transition probability data are

available for N2, such data for all other molecular

species are inadequate. Atomic data are available for Sv\ Tr'^^, eic. In addition to atomic and molecular

transition data, collisional quenching data for all species

in the pressure range 0.1 to 100 torr would be helpful.

6. Plasma Modeling

Models under development include those for plasma

etching and deposition reactors, gas lasers, pulsed

power devices and plasma remediation of toxic waste.

Oscillator strengths and transition linewidths are used in these plasma chemistry models in two ways. The first use is in formulating the continuity equations for atomic

and molecular species in the plasma. The knowledge of

oscillator strengths leads directly to radiative lifetimes which, in some cases, is the dominant depopulating

mechanism for excited states produced by electron

impact in low pressure plasma etching reactors^^.

The second use is in calculating the small signal and

saturated gain of plasma excited lasers. A system

currently of interest is the electron beam excited Xe

laser using Ar/Xe and He/Ar/Xe gas mbctures^*^. This

laser operates on 6 infrared transitions (1.73 fm to 3.65 fm) between the 5d and 6p manifolds of Xe I (see

Figure 1). The dominant laser transitions are, in order

of efficiency, 1.73 fm (5d[3/2]i ->6p[5/2]2), 2.03 fm

(5d[3/2]i^p[3/2]i), and 2.63 fm (5d[5/2]2-^p[5/2]2).

The upper laser levels of the Xe laser are populated by

1. W. Whaling and J. Brault, Phys. Scr. 38, 707 (1989).

2. G. A. Martin, J. R. Fuhr, and W. L. Wiese, NIST

Atomic Transition Probabilities Data Files (Scandium

through Nickel), Standard Reference Data Base No. 24

(also in /. Phys. Chem. Ref. Data 17, Suppl. 3 and 4

(1988).).

3. J. R. Fuhr and W. L. Wiese, "Atomic Transition

Probabilities" in CRC Handbook of Chemistry and

Physics, 13"^ Ed., D. R. Lide, editor (CRC Press, Boca

Raton, FL, 1992) P. 10-128 -- 10-179.

4. NIST Spectroscopic Properties of Atoms and Atomic

Ions, NIST Standard Reference Database 38.

5. W. L. Wiese, J. W. Brault, K. Danzmann, V. Helbig,

and M. Kock, Phys. Rev. A, 39, 2461 (1989).

6. J. Shumaker and C. Popenoe, /. Op. Soc. Am. 59, 980

(1%9).

a collisional radiative cascade following dissociative recombination of dimer ions such as ArXe"*". For

example, direct excitation of the Xe(7p) manifold by

dissociative recombination leads to pumping the Xe(5s)

manifold by a collisional radiative cascade. The lower

laser levels are depopulated by radiative decay to the Xe(6s) and Xe(6s') levels and by heavy particle

quenching collisions.

Since the Xe laser is usually operated in high pressure gas mixtures (> 0.5 - 1 atm), collisioned broadening of

the laser transitions are exceedingly important in calculating the gain of the system. In spite of the fact that this is a rare gas atomic laser, there have been

surprisingly few measurements of broadening

coefficients by either heavy particle or, more

importantly, electron collisions. Recent measurements

of the broadening of the 1.73 fm transition by collisions with He, Ne and Ar yielded values of 20.3, 12.7 and 19.7 MHz/Torr respectively, with uncertainties of

approximately ±(10-25%)^^ These yield broadened

linewidths of ~ 20-30 GHz at normal operating

pressures. Broadening coefficients for the other laser transitions have only been implied from measurements

of saturation intensity.

Perhaps the most important issue in scaling this laser is the broadening and quenching of the laser transitions by

electron collisions'^. The scaling of the optimum pump

rates for the xenon laser lead one to conclude that electron collisions (either dephasing or quenching)

lower gain and lead to termination of the laser. For

example, the premature termination of lasre gain in a

fission fragment excited laser is believed to be a result of electron collisions (see Figure 2)^'. To date, there are no direct measurements of electron collision broadening coefficients of the laser transitions, which

represents one of the greatest uncertainties in modeling

and scaling the laser.

8. G. Garcia and J. Campos, Phys. Scr. 33, 321 (1986).

9. V. Vujnovic and W. L. Wiese, /. Phys. Chem. Ref Data

21, 919 (1992).

10. J. E. Lawler and M. Salih, Phys. Rev. A 35, 5046

(1988).

11. T. R. O'Brian and J. E. Lawler, Phys. Rev. A 44, 7134

(1991).

12. D. K. Zerkle, S. Schwartz, A. Mertogul, X. Chen, H.

Krier, and J. Mazumder, /. Propuls. and Power 6(1)

(1990).

13. D. K. Zerkle and H. Krier, "Non-Local

Thermodynamic Equilibrium in Laser Sustained

Plasmas," AIAA 92-2991, Proc. AIAA 23rd

Plasmadynamics and Lasers Conf. (1992).

14. M. Kwiatowski, P. Zimmermann, E. Biemont, and N.

Grevesse, Astron. Astrophys. 112, 337 (1982).

15. K. S. Rao, Nature 170, 670 (1952).

7. G. Garcia and J. Campos, /. Quant Spectrosc. Radiat

Trans. 34, 85 (1985).

16. K. S. Rao, Nature 173, 1240 (1954).
Alexander Scheeline et al. 39

17. K. S. Rao, Proc. Nat. Inst. Sci. India 21A, 188 (1955).

18. W. L. Wiese and J. R. Fuhr, /. Pliys. Chem. Ref. Data

4, 263 (1975).

19. L. E. Kline and M. J. Kushner, "Computer Simulations

of Materials Processing Plasma Discharges", in CRC

Critical Reviews in Solid State and Materials Science,

16, 1 (CRC Press, Florida 1989).

20. M. Ohwa, T. J. Moratz and M. J. Kushner, /. Appl.

Phys. 66, 5131 (1989).

21. G. A Hebner and G. N. Ways,, Appl. Phys. Lett. 59, 537

(1991).

22. J. W. Shon, G. A. Hebner, G. N. Hays, and M. J. Kushner, "Predictions for Gain in the Fission

Fragment Excited Xe Laser", 2ubmitted to /. Appl.

Phys.

II -

>-O 10

LlJ

e - Xe(6s

ot

-Xe*

-Xe**

-Xe(7p/7s)

-ArXe* -Xei

Figure 1. Energy levels and transitions in the atomic xenon (5d— 6p) laser.

CM

I

E

O

<

-3

1 1 1 1

' -.^PUMP PULSE

/ ' 'A'll

\ V, •

-

experiment' V- / /

Ar/Xe = 99.7/0.3 THEORY

529 TORR. 87 W/cc

1 1 I r 0 12 3 4

TIME (ms)

Figure 2. Experimental and modeling results for gain

gain at 2.03 /xm in a fission fragment excited xenon

laser. The termination in gain is believed to be a result of electron collisions.
New measurements in the spectrum of neutral lithium (Li \) by Fourier

Transform Spectroscopy.

LEON J. RADZIEMSKI, Physics Department, Washington State University

ROLF ENGLEMAN, Chemistry Department, University of New Mexico

JAMES BRAULT, National Solar Observatory

The neutral lithium spectrum plays a pivotal role in modelling the solution for a

four-body problem. Also it provides a good test for specific mass shift calculations

(SMS), because SMS and the normal isotope shift are the only contributions. The

most recent improvement in Li I energy levels appeared in the late 1950's. Since then

energy level spacings due to electronic structure and electron-nuclear interactions

have been measured by many spectroscopic techniques. The energy levels are of

uneven accuracy due to variable wavenumber accuracy primarily due to the infrared

data measured with 1950's grating technology. To remedy this situation we

remeasured the ^Li and ^Li spectra (3,000 to 30,000 cm""!) using the 1 -meter McMath

Fourier Transform spectrometer at Kitt Peak. The measurements have been

completed but the level analysis has not been finished.

A by-product of the FT measurements will be a consistent set of relative

oscillator strengths.

40
The Atomic Branching Ratio Project at NIST

J. Z. Klose and W. L. Wiese

National Institute of Standards and Technology

Gaithersburg, MD 20899

The Atomic Physics Division of the National Institute of Standards and

Technology has a project underway to compile branching ratios for transitions in atomic

ions of interest. So far, data have been published on H-, He-, Li-, Be-, and B-like ions,

providing such ratios for transitions in ionic species of light elements. These elements

(H, He, C, N, O, Ne) occur as impurity ions in high-temperature plasmas or may be

conveniently introduced as trace elements for diagnostic studies. Further tabulations are planned to provide additional data on these elements.

Table 1, which contains branching ratios for the ion N II, is a typical presentation

of such data. In the table the intensity ratio Ishon/Iiong = A^hort^iong/Aion/ shortReferences

[1] J. Z. Klose and W. L. Wiese, J. Quant. Spectrosc. Radiat. Transfer 42, 337 (1989).

[2] J. Z. Klose, J. R. Fuhr, M. S. Price, and W. L. Wiese, J. Quant. Spectrosc. Radiat.

Transfer 48, 33 (1992).

[3] D. Luo and A. K. Pradhan, J. Phys. B 22, 3377 (1989).

[4] K. L. Bell, C. A. Ramsbottom, and A. Hibbert, J. Phys. B 25, 1735 (1992).

41
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h1
PRECISION MEASUREMENT OF THE MEAN LIFE OF THE

Ar II 4p' 2FO7/2 LEVEL

Jian Jin and D. A. Church

Physics Department, Texas A&M University, College Station, Texas 77843

A variant of the collinear laser beam - ion beam spectroscopy technique has

been used to measure the mean life of the 4p' 2FO7/2 level of Ar II to a relative precision of 3 X 10*3. Our result is T = 8.414 ± 0.025 ns, in excellent agreement with the

recent result of Marger and Schmoranzer^ v = 8.41 ± 0.03 ns, obtained by a crossed

laser-ion beam technique.

Our technique enables a measurement without either mechanical motion or laser sweeping. The apparatus is shown schematically in Figure 1. The beam

from an etalon-stabilized ring dye laser is directed anti-parallel to a 30 keV Ar+

ion beam. This ion beam contains metastable 3d' ^009/2,7/2 states produced in the

ion source. With the laser fix- tuned to 6124.39A, measured with a Burleigh

wavemeter, and a voltage-controlled velocity change of the ions, the Doppler effect

enables resonant excitation of the 4p' 2FO7/2 level from either of the lower levels.

Optical decays of the upper level were observed near 4610 A and 4906 A, and a

prompt cascade transition near 672 A, which follows the 4610 A decay, was observed as well. The fluorescence was collected perpendicular to the beam direction using a condensing lens for the visible transitions.

Precise electric field plates^.S were used to accelerate the ions in the

observation region, resulting in laser excitation only in a limited spatial region.

By adjusting the potential of the whole electric field plate assembly, this excitation

region was scanned in space. The emissions of ions selectively excited upbeam

from the detection region were collected after a delay determined by the distance

between excitation and detection regions, and the ion velocity. This delay

corresponded to times in the ns range, resulting in an ion intensity variation with

accelerating potential from which the mean life was extracted. Figure 1 shows

schematically this variation in space, or time relative to excitation.

The ion spectrum was obtained by setting the electric field to zero and scan- ning the potential of the field plate assembly. This spectrum is shown in Figure 2.

The width is determined by the velocity distribution of the ions in the source, vari44
Jian Jin and D. A. Church 45

ations of the potentials, and the laser line width (about 30 MHz). Mean life measurements were initiated only when this spectnmi was stable and reproducible.

Figure 3(a) shows the excitation as a function of scan voltage. Only that portion of the decay curve which is not influenced by the excitation distribution was

useful for the mean life determination. The logarithm of the photon counts vs. scan voltage is shown in Figure 3(b), for this part of the intensity variation.

Measurements were made imder various test conditions to define the possible

existence of systematic effects. Since the laser light was partially polarized, and

the residual magnetic field was not shielded, quantum beats were a possibility.

Measurements with predominantly linearly and also circularly polarized light

were completed, and found to result in mean lives which differed by slightly more

than the standard deviation of the means of the measurements. This was the

largest component of the error assigned to the final result. Table 1 shows other

components of the error analysis. The 38 measurements made a statistical contribution of only 1.2 X 10"^ to the total error. Figure 4 shows the distribution of the

results of these independent measurements. Only one measurement lies more

than two standard deviations away from the mean result.

scan voltage (volt)

Fig. 1. Principle of the rapid Doppler switching Fig. 2. Ar II 3d' ^G9/2 - 4p' ^F^7/2

technique, (a) Schematic of the apparatus, (b) Ion resonance spectrum.

kinetic energy as a function of position between

the field plates and the potential C. (c) Expected

fluorescence intensity change as the potential U

is scanned.
46

iJOO 1200 nOO 1000 »00 SOO 700 600 scan voltage (volt)

Fig. 3. (a) An example of data of the

fluorescence decay curve of the Ar II 4p'

F^7I2 level, (b) The useful portion of the

decay curve for extracting mean life information. The plot is semi-logarithmic

with a constant background subtracted.

Ttbl»-1 Lilt of »Y3tem»tic erron

sourc* eormtion (in 10"') error (in 10"')

Colluioa with rat gu +0.17 ±0.17

E-Seld ±1.4

Aligninent of ionb«tjn uid E- field +0.44 ±0.44 U detcrminfttion ±1.1

Staxic effect negligible negligible Quantum bekt ±2'

Statistics ±1.2

Total +0.61 ±3.0

(In sum) (in quadrature)

10.0 98

9«

9.4

9.2 90

88

8.«

8.4

8.2

8.0 78

78

7.4 7270

Ar II 4p' F^/g mean life

T«8 414i0.025n8

3 10 IS 20 29 M JS 40 measurement trials

Fig. 4. Mean life measurement trials. All

solid symbols represent the measurements done

using partially linearly polarized laser light,

and open ones for elliptically polarized light.

Similar symbols designate trials made during

a continuous sequence of measurements. The

raw measurement result was r s 8.409 ± 0.012

ns. After systematic corrections* the final

result is T = 8.414 ± 0.025 ns.

References

1. D. Marger and H. Schmoranzer, Phys. Letters A146, 502 (1990).

2. M.L. Gaillard, D. J. Pegg, C. R. Bingham, H. R. Carter, R. C. Mlekodej, and J.

D. Cole, Phys. Rev.^ASfi, 1975 (1982).

3. D. J. Pegg, M. L. Gaillard, C. R. Bingham, H. R. Carter, and R. C. Mlekodej,

Nucl. Instnmi. Meth. 2112, 153 (1982).
Accurate Oscillator Strengths for Interstellar Ultraviolet Lines

of CI I

R.M. Schectman, S.R. Federman, D.J. Beideck, and D.G. Ellis

Department of Physics and Astronomy, University of Toledo,

Toledo, OH 43606

Work Supported in Part by NASA Grant NAGW-2457

We have recently begun a re-examination of the CI chemistry in diffuse interstellar clouds,

incorporating both older satellite UV data and recent HST results. As a preliminary to this work,

we report here measured f-values for the astrophysically important lines of CI I at 1088, 1097, and

1347 A. For 1088 and 1097 A, only f-values estimated from astronomical data or from theoretical

calculations were previously available. However, the astronomical observations indicated that the

f-value of X1097 was significantly smaller than that of /\,1088, while the calculations of Ojha and

Hibbert, based upon the classification scheme of Radziemski and Kauffman, predicted the reverse. VUV transitions were studied using the beam foil spectroscopy facility at the University of

Toledo Heavy Ion Accelerator. Beams of CI* ions at energies of 130 keV and 180 keV were

neutralized and excited by traversal through thin (2 ijg/cm^) carbon foils. Time-resolved decay

curves were obtained by recording the intensity of the radiation selected as a function of the

distance between the exciter foil and the monochromator entrance slits. Decay curves for transitions from the 3p'*(^P)4s ^Pg^ level to both the 3p^^P°3/2 ground state (1347.24 A) and to the higher-lying fine structure level 3p^^P°i;2 (1363.45 A) were measured. These

decays were observed to be essentially single exponential for times after excitation of less than 10

ns, with deviations due to cascade repopulation observed only for longer delays. The value obtained

for the meanlife of the 3p''4s(^P) ^Pg^^ excited level was 1.51 ± 0.07 ns. To extract A-values for the

two competing transitions, the branching ratio 1(1347)71(1363) was measured as 5.77 ± 0.23,

independent of distance from the foil, as required. The detection efficiency of the monochromatorphototube combination varies by less than 1% over this small wavelength interval. The resulting

f-values are shown in Table 1. Next, the resonance transitions from the J = 5/2 levels at 1088.06 and 1097.37 A were

measured. The spectral feature at 1088.06 A is strong and unblended. As for the two previous

transitions, decay curves were measured at two energies and for different directions of travel. To

improve the statistical accuracy, data from a number of decay curves measured with different foils were superimposed. The resulting experimentally determined meanlife was 3.3 ± 0.3 ns. On the other hand, the line at 1097.37 A is very weak. It appears only as a shoulder on the

stronger transition 1098. 07A, The spectra were fit by a superposition of Gaussians and the ratio of

the intensities of these two lines R( 1088/1097) was obtained at a number of times after excitation.

The ratio varied slowly with time and extrapolation to t=0 gave a value for R as the atoms exited

the foil of R = 9.3 ± 1.1. Making the assumption that the two J=5/2 levels arising from the same

2p^(^P)3d configuration are equally populated initially results in a meanlife for the excited state leading to the 1097 A transition of 31 ± 5 ns. The measured intensity of the 1097 A line as a

function of time is indeed consistent with a single exponential decay of 31 ns, qualitatively

confirming the assumptions made concerning the nature of the foil excitation process. Because of

the very small transition energies involved, the branching ratios to the lower-lying levels of the

3p*(^P)4p configuration are small and may be neglected when computing a transition probability

for X1088 from the measured meanlife. The f-values for X1088 and A,1097 are compared with

previous results in Table 2.

47
48

Conclusions:

Our f-values for >.1347 and X1363 (fn347) = 0.153±0.011 and fll363) = 0.055±0.004) are the

most precisely measured values available. They are systematically some 40% larger than those

reported earlier, necessitating a re-evaluation of astrophysical conclusions based upon the older,

less accurate, results. In particular, f-values obtained from astronomical observations which rely

upon knowledge of fll347) must be revised. Agreement between our measurements and the recent

theoretical predictions of Ojha and Hibbert (1990) is, for these lines, quite satisfactory.

Our f-values for U1088, 1097 (fn088) = 0.081±0.007 and f);i097) = 0.0090±0.0015)

represent the first laboratory measurements for these lines. These results resolve the issue

regarding the relative strengths for ?lX1088, 1097 in favor of those indicated by astronomical

measurements, showing that X1088 is by far the stronger of the two lines. We will discuss the consequences of these measurements for understanding the diffuse

interstellar medium in a subsequent paper, where a study of the chlorine chemistry based upon

our new f-values will be described.
R. M. Schectman et

Table 1 Oscillator Strengths

I347.2A 1363.A

This Work 0.153 ± 0.011 0.055 ± 0.004

Previous Results:

Schwab and Anderson 0.109 ± 0.010

Hofmann 0.090 0.035

Lawrence 0.113 0.039

Clyne and Nip 0.10 ± 0.03 0.038 ± 0.006

Ganas 0.138 0.028

Ojha and Hibbert 0.132(Lr 0.049(L)^

0.117(Vr 0.04 l(Vr

"(L) is length form and (V) is velocity form.

Table 2

Oscillator Strengths

This Work

1088.06

0.081 ± 0.007

1097.37

0.0090 ± 0.0015'

Previous Results:

Federman 0.069 ± 0.020=" Federman 0.094 ± 0.026"

Jura and York 0.014 ± o.om

Jura and York 0.019 ± 0.005" Ojha and Hibbert 0.0160^)" 0.0420.)"

Ojha and Hibbert 0.006(V)'^ 0.017(V)''

^redetermined from original data. "revised using f(1347) obtained in this work.

'using assumed excitation. ^(L) is length form and (V) is velocity form.
RELATIVE INTENSITIES OF RESONANCE TRANSITIONS IN B-LIKE IONS

J. Doerferl, E. Tr&bert, P.H. Heckmann, G. MOller, J. Gran^ow, C. Wagner

ExperimentaJphysik III, Ruhr-Uuiversit&t Dochum

W-4630 Bochum 1, Germany

The relative inleneltles of the resonance transitions 26 '2p ^ _ -282p' _ would

be expected to show a ratio of 1t2 for pure LS-coupllng states. As especially the 'S^^

and . levels are strongly mixed by spin-orbit-interaction, the intensity ratios

deviate from these given ratios. We measured the intensity ratios of the fine fine structure components of the 26*2? - 2s2p' resonance transitions in the 'P" - caec, where the effect should be strongest, and for the 'P* - ''P transitions. Using the

beam-foil technique, we thus follow up on a similar study on the Al-like ions [l], expecting that the effect of configuration interaction should be stronger in the

homologous sequence of B I. As the configuration mixing varies with the nuclear charge

of the ions, we undertook to study this B I Isoelectronic trend as far as possible with our

experimental set-up, i.e. from oxygen through chlorine. Some of our results are shown in

fig. 1, alongside the theoretically predicted trends.

This particular case has been treated by theory before,e.g. using the Cowan Code and

including only the mixing of the configurations within the n=2 shell [2] or ualng the

Multi-Configuration Hartree-Fock method (MCHF) and including several

configurations in the n=3 shell (3]. For low Z, the results of all these calculations agree

with the experimental intensity ratios very well. For higher nuclear charges, however,

there are some deviations; thus it seemed interesting to investigate whether the

configuration interaction with some configurations in higher shells would be important

as well.

Our own calculations were based on the Froese Fischer MCHF code. After first considering only configurations within the n=2 shell, we then included more and more

configurations with one electron in the n=3 shell: at first only configurations with the

electron core 2s' were included, then configurations with the core 2s' and 2s2p were

added, and in the next step configurations with electron cores 28', 262p and 2p'. In the

50
J. Doerfert et al. 51

most complex calculation we ivlso -took configurations into account with ieature one

electron in the n=4 shell with electron cores 2s* and 2s2p. For all states of the same quantum number J the energy matrix was set up and diagonalif«ed including the

spin-Orbit interaction.

In order to test for the influences of relativislic effects, we included all Breit-Pauli

interactions in the most simple case of our calculations. It turned out, however, that even at higher nuclear charges these effects are negligible. As has already been observed

by Dankwort and Trefftz [3], configuration mixing is more important for allowed

transitions than relativistic effects.

Our calculations including the n=2 states only or configurations up to n=3 reproduced

the results of the comparable earlier calculations [2, 3], respectively, fairly well. The

effect of configurations of the n«»4 shell, however,turned out to be smaller than we had

expected and is rather insignificant. Therefore fig. l besides the experimental ones only

shows the theoretical intensity ratios obtained from computations which included

electrons up to the n=3 shell. For low nuclear charges it is apparently sufficient to include configuration mixing only within the n=2 shell, but for higher nuclear charges

the mixing with configurations of the n-3 shell becomes important to match the

experimental findings.

1. L. EngstrOm, N. Reistad, C. Jupen and M. WesterUnd, Phys. Scr. 39, 66 (1989).

2. B. C. Fawcett, At. Data Nucl. Data Tables 16, 135 (1975).

3. W. Dankwort and E. Trefftz, Astron. Astrophys. 65, 93 (1978).
52

Pig. 1: InteaBity ratio - '^j)/I('''J - '^») of Ihe line pair 2«'2p - 2fl2p* *S as

t function of nndear charge Z. W Experimout (Error bara reflect itatlsUcal uncottaintiee ouly.)

theory

RcBuUs of our own MCHF calculations wilh varying numbon of conDgurationa.

(•) Mixing within tlvo n«=2 shell only,() mixing with conOgurations of the n=*3 shell with

electron cote 2i',(*)mlxiug with couflgurations of the n*3 sheU with electron cores 2s«

and 282p,Wmixiug with configurations of the nt=3 shell with electron cores 2s*, 2s2p and

3P«.
ACCELERATOR-BASED SPECTROSCOPY

PROJECTS AT BOCHUM

E. Trabert

Experi mental physi k III, Ruhr-Universitat Bcxihum

D-4630 Bochum 1, Germany

The Bcxhum accelerator laboratory houses a 4 MV Dynamitron tandem accelerator capable of

producing comparably high ion beam currents of many elements (about 40 have been tried so

far) as well as a 400 kV single stage accelerator. Both machines can serve ion beams to the

spectroscopy set-up which is run by P H. Heckmann and E. Trabert. This permanent

experimental set-up consists of a McPherson Mod. 247, R = 2.2 m, grazing-incidence

spectrometer with four interchangeable gratings (300, 600, 12(X) and 3600 1/mm), working best

in the wavelength range X = 4 to 80 nm. A mobile grazing-incidence spectrometer employs the same 1200 1/mm grating and covers the wavelength range X = 1 to 13 nm. Foil and gas targets can be used. This contribution concentrates on data obtained since the previous conference at Amsterdam, in particular from intercombination decay studies done at Bochum and Argonne.

2p^ *S03/2 decay in He"

The 2p3 "^8° state can be considered as being triply excited, as none of the electrons are in an

orbit occupied in the ground state configuration. Because of its particular symmetry, however,

it does not disintegrate rapidly by autoionization, but is expected to emit narrow band radiation

when decaying towards the ls2p 3po + e/ continuum ([1] and refs. therein). In neutral Li and in

the positively charged three-electron ions the 2p3 '^S^ level and the level it predominantly

decays to, \s2p^ '^P, are both bound. This has been discussed e.g. by K.T. Chung ([2] and

refs. therein), and it has been corroborated by wavelength and hfetime measurements in Li^ and

Be"^ [3,4] as well as by new experimental wavelength data for B2+ and C^"^ [5,6].

In the case of He" neither of the aforementioned levels is bound. The upper level, however, is narrow, because autoionization is suppressed for reasons of symmetry. The lower levels

(Is2p2 '^P, Is3p2 '^P, 2s2p2 '^P) autoionize rapidly and thus must be broadened. Of these lower

levels, we consider only the lowest one, because the decay branch to this level is the dominant

one. When a radiative transition from the 2p3 "^S^ level has populated the Is2p2 '^P level (a

shape resonance just above the ls2p 3po ionization limit of the two-electron system), one might

expect a radiationless transition, autoionization, to carry away the rest of the excitation energy

of the upper level. Nicolaides, however, proposed a more complicated process to take place,

radiative autoionization (RA) of the 2p^ ^^S^ level, in which a photon would be emitted

simultaneously with an electron. Nicolaides' prediction is that the photon energy distribution of

53
54

this transition has a peaked shape, with a notable maximum near the matching energy for

reaching the Is2p2 "^P shape resonance, that is near a wavelength of h=32 3\5 nm.

We have, indeed, observed a weak, line-like structure at X^(32.32±0.02) nm, in spectra of

foil-excited He ions at incident energies in the range 140 - 200 keV [7]. Our results agree with

the results of a parallel study by E.J. Knystautas (Quebec) [6]. This would be the first observation of this elusive decay in He". The present data are not sufficient, however, to distinguish between a radiative decay to the ls2p^ '^P resonance state and subsequent

(immediate) autoionization on one hand and a truly simultaneous emission of a photon and an

electron, as assumed in RA, on the other.

Intercombination transitions

The occurrence of spin-changing transitions is an indicator of the break-down of LS-coupling

and its replacement by intermediate coupling. The transition rates of such transitions, compared

to spin-conserving transitions between similar electron configurations, provide a direct measure

of relativistic interactions like spin-orbit coupling which effects multiplet mixing. Our study of

systems with only a few electrons outside of closed shells, but with different electron cores, aims at obtaining data for plasma diagnostics and at finding out about reliable calculations for

such cases.

The only available method to measure such transition probabilities in highly charged ions is beam-foil spectroscopy. This technique, however, requires fast ion beams and thus works

properly only for lifetimes shorter than, say, 50 ns. For intercombination transitions without a change of the principal quantum number, this typically is the case only for ionic charges higher

than about 12.

The inherent time resolution of the beam-foil light source permits to record delayed spectra by

simply displacing the exciter foil from the field-of-view of the detection system. In this way,

spectra are obtained in which the bright lines from the decays of short-lived levels have lost out

in comparison to the persistent decays from long-lived levels which are weaker per unit of

length of ion beam observed [8]. In a number of cases, intercombination transitions have been

identified first in such delayed spectra of foil-excited ions, which then could be singled out

from laboratory or astrophysical plasma spectra yielding higher precision wavelength data [9].

Kr I sequence

The present experimental program at Bochum proceeded from two-, three- and four-electron

ions with electrons in the n=3 shell (isoelectronic sequences Mg 1, Al I and Si 1) to those with

electrons in the n=4 (Zn I, Ga 1, Ge I sequences) or in the n=5 shell (Sm 1, Eu I-like). Most

recently, intercombination transitions in the rare-gas like spectra of the Kr I sequence have been

added. In this sequence, there are two intercombination transitions within the lowest shell.
E. Trabert 55

4p^ ^Sq - 4p54d ^P^i and ^D^^i, with quite different dependences of the transition probabilities on the ionic charge The measurements agree rather well with the predicted isoelectronic trends. In particular the long-lived level, -^P^i, the decay of which involves a much lesser degree of

mixing (which even decreases again towards higher nuclear charges) stands out [10].

Mg I, Al I, Si I sequences

At Argonne National Laboratory, the EUV spectrum of 120 MeV foil-excited Br ions was

studied close to and away from the exciter foil [11]. A multichannel detector was used which

permitted to obtain sufficient data rather quickly. Clearly the appearance of the spectrum varies

with the distance from the foil (time after excitation). The lifetime results for intercombination

transitions in the spectra isoelectronic with Mg I, Al I, and Si I are shown on the poster.

Work on the intercombination transitions in the Zn I, Ga I and Ge I isoelectronic sequences and on 3d^4s2 - 3d^ 4s4p transitions in Cu I-like spectra (which feed the laser transitions in the

Morley-Sugar laser scheme [12,13] is presently being continued by studying the spectra of Mo

and Rh. Also, the intercombination decay of the Is22s3p 3poj level in Be-like ions is being

studied indirectly by searching for the 2s3s ^S - 2s3p ^P*^ and 2p^ - 2s3p ^po transitions in

the spectra of Na through Si [14].

References

1. C.A. Nicolaides, J. Phys. B:2S L91 (1992). Corr.: 25, 2442 (1992).

2. B.F. Davis and K.T. Chung. Phys. Rev. A 42, 5121 (1990).

3. M. Agentoft, T. Andersen , and K.T. Chung, J. Phys. B: 17. L433 (1984 ). 4. S. Mannervik, R.T. Short, D. Sonnek. E. Trabert, G. MoUer, V. Lodwig,

P.H. Heckmann. J.H. Blanke. and K. Brand. Phys. Rev. A 39. 3964 (1989).

5. E. Trabert. DTL Annual Report 18 (Bochum 1992. unpublished preliminary data)

6. E.J. Knystautas (private communication 1992).

7. E. Trabert, P H. Heckmann, J. Doerfert, J. Granzow, J. Phys. B25. L353 (1992).

8. E. Trabert, P H. Heckmann, R. Hutton, and I. Martinson, J. Opt. Sac. Am. B5, 2173

(1988).

9. E. Trabert, R. Hutton, and I. Martinson, Mon. Not. R. astron. Soc. Ill, 21p (1987).

10. E. Trabert, Physics Letters A 167, 69 (1992), in collaboration with J. Doerfert,

J. Granzow, P H. Heckmann, G. Moller, and C. Wagner .

11. E. Trabert, H.G. Berry, R.W. Dunford. J. Suleiman, E.W. Kanter. C. Kurtz.

S. Cheng. A.E. Livingston, K.W. Kukla, E.G. Serpa, A S. Zacarias, and L.J. Curtis

(work in progress).

12. P.D. Morley, J. Sugar. Phys. Rev. A38, 3139 (1988).

13. G. Moller. E. Trabert, P H. Heckmann, J. Sugar. Physica Scnpta 46. 36 (1992).

14. J. Granzow. P H. Heckmann. E. Trabert, J. Doerfert (work in progress).
WORK IN PROGRESS AT THE LUND VUV-FTS

Ulf Litz^n and Sveneric Johansson

Lund University

Physics Department, Solvegatan 14

S-223 62 Lund, Sweden

Tel 46-46-10 77 33

1 . Introduction

A Fourier Transform Spectrometer specially designed for the

UV and VUV regions is being used at the Lund University

Atomic Spectroscopy Group. The instrument, manufactured by

Chelsea Instruments Ltd., UK, was purchased thanks to a grant from the Swedish Natural Science Research Council. In

the grant application, particular emphasis was put on the

possibility to produce accurate laboratory data for astrophysical research, and investigations with this purpose have

accordingly dominated during the first year. More general

atomic spectroscopy and atomic physics work will, however,

also be carried out at the instrument, and such projects

have already been initiated.

Besides the VUV-FTS, other instruments are also being used

in the work described here. Thus FTS spectra at longer

wavelengths, recorded at the Kitt Peak NSO FTS, have kindly

been put at our disposal for several years, and we look

forward to continued collaboration. For wavelengths below

the lower limit of our VUV-FTS, a 3-m normal incidence (NI)

grating instrument is available at our laboratory. Numerous

photographic spectra in the same region at higher resolution

have been recorded in collaboration with the NIST (National

Institute for Standards and Technology) atomic spectroscopists at the NIST 10.7-m NI spectrograph. A collaboration

with the Observatoire de Meudon has just been started,

comprising use of the Meudon 10.7-m NI spectrograph.

2. The Lund VUV-FTS

The Lund VUV-FTS, a Chelsea Instruments model FT500, is of

the type developed at the Blackett Laboratory, Imperial

College, London (Thorne et al. [1]). The instrument, which

has a 20 cm maximum scan length, is equipped with a silica

beamsplitter. This gives a short wavelength limit specified

as 1750 A. By making the mechanical and optical tolerances

sufficiently narrow, the instrument has been prepared for

^ A. A beamsplitter having sufficient

-^aiismittance and homogeneity for the region below 1750 A

is, however, not presently available.

Instrument control and data collecting is being handled from

a standard PC, where the transform itself is being carried

out on a transputer board.

56
Ulf Litzen and Sveneric Johansson 57

3. Light sources

The spectra recorded at the FTS are emitted from hollow

cathode (HC) discharges. Currents ranging from 200 mA to 8 A

have been used with different types of lamps. By selecting

proper mixtures of gases, charge transfer is used for

enhancement of spectra from singly charged atoms (see

below) . A Penning type light source, originally designed for

emission in the X-ray region, has also been tested. Using

iron cathodes, it produced strong Fe I and Fe II spectra

with good stability and reasonable noise when it was run at

a low voltage mode. Attempts to produce higher charge states

at high voltage, low pressure mode gave an enhanced Fe II

spectrum and numerous Fe III lines, not present in a cw

hollow cathode. However, the noise level was rather high.

Further development of a source of this kind is planned.

4. Term analysis

Besides the work specially directed towards astrophysical

applications, the FTS instrument is also being used for

general term analysis. In particular the complex spectra of

singly charged ions (and in some cases neutral atoms) of a

number of the 3d-, 4d-, and 5d-elements are on our program.

This far spectra of Ti, Mn, Ru, Pd, and Au have been

recorded for this purpose. In most cases extensions to other

wavelength regions are planned, by using the instruments

mentioned above.

The term analysis is being performed by means of line

identifications using already known energy levels,

establishment of new levels, and derivation of highly

accurate level values from the FTS wavenumbers . Classification of the levels and interpretation of the general

term structure as well as predictions of unknown levels are

made by means of extensive theoretical calculations.

5. Charge transfer at thermal energies

Charge transfer at thermal energies between noble gas ions

and metal atoms, resulting in enhanced population of certain

excited levels in singly charged metal ions, is a well known

phenomenon. Extended experimental studies are, however,

needed for a better understanding. A project has been

initiated, where the population enhancement in a plasma

(e.g. in a hollow cathode) will be studied through

measurement of line intensities. The enhancement will be

investigated as a function of the energy defect in the quasi

resonant process. Complex systems with a high level density

are expected to provide a possibility to derive the shape of

this function. The FTS method is well suited for this kind

of work, due to the high data collecting capacity and the

possibility for accurate relative intensity measurements. No

intensity calibration is needed, as the study only concerns

changes of intensity at different noble gas mixtures.
58

6. Measurement of oscillator strengths

Preliminary studies have been made regarding use of the VUVFTS for branching ratio measurements. In combination with

lifetime measurements, this would yield absolute oscillator

strengths. Our conclusion this far is that calibration of

the FTS efficiency is best made by means of well measured

branching ratios of groups of lines, emitted in the same

light source and at the same time as the spectrum being

measured. This will e.g. eliminate influence from wavelength

dependent illumination of the entrance aperture and changing

transmittance of the light source window, effects that are

particularly pronounced and hard to check in the UV.

Branching ratios of groups of Ar II lines in the UV,

suitable for efficiency calibration, have been measured e.g.

by Adams and Whaling [2], Danzmann and Kock [3], and

Hashiguchi and Hasikuni [4]. Further measurements, in

particular extended to the region below 2000 A are, however,

badly needed.

References

1. A. P. Thorne, C.J. Harris, I. Wynne-Jones, R.C.M. Learner

and G. Cox, J. Phys . E 20/ 54 (1987).

2. D.L. Adams and W. Whaling, J . Opt . Soc . Am. 7_1, 1036 ( 1981).

3. K. Danzmann and M. Kock, J . Opt . Soc . Am . H, 1556 (1982).

4. S. Hashiguchi and M. Hasikuni, J , Phys . Soc . Japan 54., 1290

( 1985) .
Radiative Decay Rates for the Ssdp^C^P) Metastable Levels of Si II

Anthony G. Calamai". Peter L. Smith, V. H. S. Kwong'^ fe William H. Parkinson

Harvard-Smithsonian Center for Astrophysics

_ 60 Garden St., Cambridge, Massachusetts 02138

1. Introduction:

The Si II, spin-changing, "intersystem' Unes at ~234 nm, emitted as the fine-structure levels of the 3s3p^{'^P) metastable term decay to the 3s^3p{^P) ground term, are prominent features in

astronomical UV spectra, e.g.. of the the solar chromosphere^ and planetary nebulae^. Because

the lifetimes of the metastable levels are comparable with the collision times in such regions,

intensity ratios involving these Si ii] lines can be apphed to determination of plasma parameters,

such as electron densities and tempertures, in solar and steUar atmospheres'^'"*.

The accuracies of such diagnostic techniques depend critically upon accurate knowledge of the

A-values for the allowed and forbidden transitions involved. At present, radiative decay rates of the SsSp^C^P) metastable levels of Si ll] are known only by theoretical means'*'^ that can be

quite uncertain until tested by measurements. In this report, we present the first experimentally

determined radiative decay rates for the ./ = |, |, and ^ levels of the Ss^p^C^P) term of Si ii.

2. Experimental Method:

Metastable Si''' ions were produced by electron bombardment of SiH4 vapor, at pressures

ranging from 2 to 25 x 10~^ Torr, and stored in a cylindrical, radio-frequency, ion trap. Radiative

decay rates for the metastable levels of the ^sSp^C^P) term of Si ii were determined by measuring

the time dependence of the intensity of ~234-nm photons emitted when the metastable ions

decayed to the ground term. The photons were focused onto a 12-nm-bandwidth interference filter in front of a photomultiplier tube operated in photon-counting mode. Beginning ~80 fxs after the

end of the electron-impact interval, photons were detected using a data collection technique^ that

incorporates a real-time background correction.

A logarithmic plot of one of our 29 'decay curves' is shown in Fig. 1(a); the solid-curve repre- sents the result of a nonlinear least-squares fit of three-exponentials plus a constant background,

which was small relative to the other components, to the data. To ensure that the fits converged

to a consistent set of 'best' parameters in the seven-parameter space, each decay curve was

fitted using three different sets of input seeds that varied by more than a factor of two. Generally,

the Xu statistics of the nonlinear fits were <1.0 and the variations of fit results were within the

expected uncertainties. Experimental parameters - including trap well depth, electron-impact

excitation energy, and the silane source pressure - were varied for several of the accumulated

decay curves. Plots of the mean decay rates vs. pressure for each of the three components are shown in Fig. 2. No other significant systematic effects were observed.

3. Discussion & Results:

The essentially pertubation-free environment of our low-energy rf ion trap, coupled with a

negligible probabiHty for systematic error from cascades and the outstanding signal-to-noise ratio

for each decay component, permits unambiguous determination of the radiative decay rates of

the Si ll] '*P levels. A measure of the accuracy of the results is evidenced by a decomposition

of the data in Figure 1(a) using the decay-rale and initial-population values determined by the

fits. Figure 1(b) shows the result of this procedure: The counts associated with the two fast- decay components and with the constant background have been subtracted from the data shown

in Fig. 1(a). The logarithmic plot of the remaining signal clearly indicates that only a singlecomponent is left in the data set. This is the result regardless of which two components are

59
60

subtracted from the data and is consistent from run-to-run. Moreover, if all three components

are subtracted from the data sets, the residual counts are uniformly distributed about zero with an amplitude consistent with Poisson statistics.

Our results for the radiative decay rates of the 'SsSp^C^P) metastable term of Si"'" are compared

with calculated values in the Table below. The assignments of the measured decay rates to the

various levels of the '^P term are based on: (i), good agreement with theoretical values'*'^ for the

J — 2 2 ^^^^IS' and, (iij, agreement with the observed relative intensities from a laboratory

spectrum'

Decay rates (sec ^) for levels of the SsSp^C^P) metastable term of Si Author Method -•^3/2

Nussbaumer^ (1977) theory 2398 1634 7576

Dufton et al.'^ (1991) theory 2703 1721 11236

this work experiment 2460 ± 8.2% 1233 ± 9.5% 9615 ± 15.4%

1

I I .

lot-' ' ' ' 1

2

' '

I H

_j I I I I I I i_ _J I I L_

Fig. 1 Decay curves - (a) Logarithmic

plot of the signal versus time as the

SsSp-C'P) J = I, I, and \ metastable

populations of Si ll decay. The solid- curve represents the results of a nonlinear least-squares fit of three exponentials plus a constant background

to the data. (b) Logarithmic plot

of the resdiual signal counts in the

data set after the results of the nonlinear least-squares fit were used to extract the fast- and medium-rate components from the data. The straightline behavior indicates only one exponentially decaying population remains

in the modified data set.

Time (ms)
Anthony G. Calamai et al. 61

Fig. 2 Mean decay rates versus SiH4 pressure: (a) Decay rates assigned to the Si ll] '* P1/2 level; the dashed line shows the mean value of the 29 measured decay rates, (b) Decay rates assigned

to the Si 11] '^Ps/o level, (c) Decay rates assigned

to the Si n] ^Pa/o level. In Figures (b) and (c), the solid lines represent the results of a linear least-squares fit to the measured decay rates vs. pressure.

SiH. pressure (10 Torr)

This work was supported in part by NASA Grants NAGW-1596 and -1687 to Harvard University.

[*] current address - Department of Mathematics & Physics, Philadelphia College of Pharmacy & Science

[t] permanent address - Department of Physics, University of Nevada at Las Vegas

References:

[1] G. A. Doschek ei ai, Astrophys. J. Supp. 31, 417 (1976).

[2] J. Koppen and L. H. Aller, Exploring the Universe with the lUE Sateliie, ed. Y. Kondo, Reidel,

Dordrecht, p.589 (1987).

[3] P. G. Judge et ai, Mon. Not. R. Astro. Soc. 253, 123 (1991).

[4] P. L. Dufton et a/., Mon. Not. R. Astro. Soc. 253, 474 (1991).

[5] H. Nussbaumer, Astron. Astrophys. 58, 291 (1977).

[6] A. G. Calamai et ai. Phys. Rev. A45, 2716 (1992).

[7] A. G. Shenstone, Proc. R. Soc. London, Ser. A 261, 153 (1961).
ATOMIC OXYGEN TRANSITION PROBABILITIES AND RECOMBINATION RATES

OF ASTROPHYSICAL AND GEOPHYSICAL INTEREST

V. ESCALANTE\ G. A. VICTOR^, and A. GONGORA-T.^

^ Institute de Astronomi'a, UNAM, Ap. Postal 70-264, Mexico, DF 04510, Mexico

^ Institute for Theoretical Atomic and Molecular Physics, Harvard-Smithsoninan Center

for Astrophysics, 60 Garden St., Cambridge, MA 02138

^ The University of Michigan, The Harrison Randall Laboratory of Physics, Ann Arbor,

MI 48109-1120. Permanent address: Instituto de Fisica, UNAM, Ap. Postal 20-364,

Mexico, DF 01000, Mexico

Dipole-allowed and spin-forbidden transitions of atomic O emit prominent lines in space and atmospheric

plasmas, and armrntp transition probabilities are needed to model and understand the excitation mechanisms

that produce iJn ni [n the atmosphere at night and in the interstellar medium, these lines are excited by

recombination of 0+ ions and thermal electrons, and information on recombination rates and transition

probabilities for a large number of excited states is needed.

We present results of calculations using a model potential method to produce accurate wave functions of

excited and continuum states with the ground core configuration O+C^S") that allow the calculation of the

recombination spectrum. Compnrisnn with other theoretical calculations are shown. We have also carried out calculations of some allow. .] spin-forbidden transitions using a multiconfiguration Hartree-Fock

procedure that includes Breit-Pauli corrections (Froese Fischer 1991).

MODEL POTENTIAL CALCULATIONS

We used a one-electron semiempirical model potential (MP) to describe the interaction of the active

electron with the core that includes a dipole polarization term and an additional term of the form

Uy(r) — a-y exp{ — kyr)

to account for exchange and other short-range corrections. The a-y and k-y parameters are calculated by a

least squares procedure that fits the calculated energies to the observed values of the Rydberg series of a given

symmetry 7. Experience with other open shell 2p core configurations indicates that the set of parameters for

the 2p^np series does not give an accurate description of the 2p'* terms due to the strong correlation between

the 2p electrons. Thus a different set of parameters must be calculated for the ground configuration terms.

Details of the calculations have been discussed by Escalante and Victor (1988, 1992a).

We have calculated transition probabilities for dipole-allowed transitions and photoionization cross

sections for states with n — 2 to 12 and i = 0 to 2. Hydrogenic values needed for the calculation of

the recombination cascade have been used for configurations with higher L Radiative recombination rates

62
V. Escalante et al. 63

have been calculated from the detailed balance relation for a thermal energy distribution of electrons. The

effective recombination rate of a state is the rate of population of the state due to direct recombination, with

rate a,-, plus cascades from all other states also populated by recombination:

k>i

where Ck,i is the probability of reaching state i from state k by successive transitions. The effective recombination coefficient times the branching ratio of a transition equals its emission rate. In calculating

effective recombination rates we have included dipole-allowed transitions and recombination rates to triplet

and quintet states of the ground core configuration. We also took into account some spin-forbidden (Egikyan

1984, Froese Fischer 1987), and dielectronic recombination rates (Nussbaumer and Storey 1984) that produce

lines involving the ground configuration and states with the excited core configuration 0'^{'^D°). Dielectronic

recombination does not have a noticeable effect in the emission rates for electron temperatures below 1000 K.

In table 1 we compare our MP results for the case in which there is no absorption of resonant photons in

the plasma with calculations of Julienne and Davis (1974), who used the quantum defect method (QDM),

and Hartree-Fock (HF) calculations by Chung et al. (1991). The QDM values show significant discrepancies

with the HF and MP results for low £. However there is moderate or good agreement between the HF and MP

results except for the 3s term where an order of magnitude disagreement exists. The difference in this

case can be attributed to severe cancellation in the dipole matrix element. We have found a Fano-Cooper

minimum in the 3s ^5° —* np photoabsorption cross section very near the continuum threshold. Thus

the value of the recombination cross section is very sensitive to the details of the calculation. Decay of the

3s term produce strong lines at 130.217-130.603 and 164.131 nm and experimental determination of the

cross section may help determine the correct value for the recombination rate.

MULTICONFIGURATION HARTREE-FOCK CALCULATIONS

Transitions between the ground state and excited states are important in the atmospheric dayglow and

nightglow. When photons from resonant transitions are heavily scattered, spin-forbidden transitions must

be taken into account. MCHF calculations for the transition probability of the — 2p^(^D°)3s ^5°

multiplet at 130.217-130.603 nm (Froese Fischer 1987) is close to the the MP value. The value of Egikyan

(1984) is a factor of 2 smaller than the value calculated by Froese Fischer (1987) for the transition probability

of 2p'^ - 2p^{'^D°)Ss at 164.131 nm. Our MCHF calculations agree with the values of Froese

Fischer (1987) even though we have used a smaller set of configurations. Nevertheless we have found some

sensitivity in the choice of configuration list. For example, when 2s^2p^4/ configurations are not included

in the composition of the 2p'^ states, the probability of the AS' ^ 0 transition at 164.131 nm decreases by a

factor of 4 while resonant transition probabilities vary less than 15%.
64

Table 1. Comparison of direct and effective recombination

rates (in IQ-^^cm^s-i) at 1160K.

Term CVTerm^ OTerm'" "Term'' ^Term^ '^Term''

35As

6s

3d

4d

6d 3£>°

3p

bp ^P

Qp ^P

1.5(-3)^

2.0(-3)

3.2(-3)

3.1(-3)

3p3p 6.1(-1)

4p^P 5.0(-l)

5p3p 3.5(-i)

6p^P 2.4(-l)

3.00

2.00

1.18

7.4(-l)

3s 1.3(-3)

4s ^5° 3.7(-3) 5s ^5° 5.9(-3)

6s 5.5(-3)

1.24(-2)

2.88(-4)

8.29(-4)

l.ll(-3)

1.05 6.41(-1)

4.01(-1)

2.64(-l)

2.98

1.84

1.11 7.05(-l)

3.95(-2)

1.02(-3)

8.85(-4)

1.39(-3)

9.00(-4)

6.66(-3)

7.31(-3)

5.96(-3)

6.08(-l)

4.56(-l)

3.10(-1)

2.12(-1)

3.23

1.95

1.16

7.32(-l)

5.05(-2)

8.32(-4)

3.31(-3)

3.72(-3)

4.89

7.9(-l)

2.9(-l)

1.5(-1)

7.1 9.5(-l)

3.3(-l)

1.5(-1)

4.51 7.0

9.7(-l) 1.1 4.6(-l) 4.8(-l)

2.8(-l) 2.7(-l)

1.56(+1) 2.4( + l) 4.71 5.1 2.05 2.2 1.10 1.1

4.93( + l) 4.8(+l)

8.80 8.1 2.32 2.5

9.1(-1) 1.0

2.85 2.53 2.50 4.77( + l) 4.8(+l)

1.63 1.49 1.53 9.67 8.9 9.6(-l) 9.00(-l) 9.26(-l) 3.24 3.1 6.1(-1) 5.78(-l) 5.94(-l) 1.44 1.4

Sd

Ad

5d

6d

4.90 5.24 5.62 2.68(+l) 2.8(+l)

3.49 3.20 3.37 8.24 6.9 2.02 1.91 1.98 3.53 3.2 1.25 1.20 1.23 1.86 1.7

^ Julienne and Davis (1974).

^ Chung et al. (1991).

" Escalante and Victor (1992b).

^ Numbers inside parenthesis indicate powers of 10.

References

Chung, S., Lin, C.C., and Lee, E.T.P., 1991, Physical Review A, 43, 3433.

Egikyan, A.G., 1984, Astrofizika, 20, 341 (English translation in Astrophysics, 20, 185).

Escalante, V. and Victor, G.A., 1988, Atomic Data and Nuclear Data Tables, 40, 203. Escalante, V. and Victor, G.A., 1992a, Atomic Data and Nuclear Data Tables, submitted.

Escalante, V., and Victor, G.A., 1992b, Planetary Space Set., submitted.

Froese Fischer, C, 1987, J. Phys. B, 20, 1193. Froese Fischer, C, 1991, Comput. Phys. Commun., 64, 369. Julienne, P.S. and Davis, J., 1974, J. Geophysical. Res., 79, 2540.

Nussbaumer, H. and Storey, P. J., 1984, Astronomy and Astrophysics Supp., 56, 293.
Transition Probabilities and Lifetimes of Ar I

V. Helbig

University of Kiel, Kiel, Germany

D. E. Kelleher and W. L. Wiese

National Institute of Standards and Technology, Gaithersburg, Maryland 20899

INTRODUCTION

Advances in modern atomic structure computer codes and reduced uncertainties in recent

lifetime and branching ratio measurements have yielded extensive sets of high-accuracy

atomic transition probabilities. However, most of these advances have been concentrated

on spectra of the light elements. For the neutral argon spectrum, none of the modern

atomic structure codes has provided theoretical data up to now nor have high precision

hfetime values been provided by experimental investigations. Nevertheless, we have shown

in a recent paper [1] that experiments done in recent years provide a greatly improved basis

for the compilation for the Ar I 4s - 4p and 4s - 5p transition arrays and yield transition

probabilities considerably more accurate than the most comprehensive earlier set of

transition probabilities for Ar I [2]. We have undertaken the present compilation to extend

the data given in [1] to the other prominent lines of argon.

METHOD

Following the routine discussed in detail in reference [1] we started by collecting all available lifetime values for levels of Ar I. Data have been published for 75 levels with

main quantum numbers n < 9 (see table 1). While for some of the 4p and 5p levels up to

13 different experimental results are available, for most of the other levels only one or two

experiments have been performed so far. Large differences between the data given by

various authors are found for the 2S5, 3si, 3d2, 4si, 5d2, Sdj, 56^, and Vdj levels (Paschen

notation). Complete sets of lifetimes are only available for the 4p, 5p and 4d

configurations, as shown in Table L Additional measurements to augment the known

lifetime data and to resolve the discrepancies in the data are therefore definitely needed.

The experimental set-up at the University of Kiel (see e.g., [3]) is well suited to provide

additional experimental data for a number of levels. Measurements for the 6p and 7p levels are in progress.

65
66

Table: Lifetime data available for Ar I. The numbers given after the

designation of the valence electron indicate the percentage of

levels measured with respect to the total number of levels (e.g.,

2/4 means lifetimes for 2 out of 4 levels have been measured).

ns np nd

4s 2/4 4p 10/10 3d 7/12

5s 3/4 5p 10/10 4d 12/12

6s 3/4 6p 3/10 5d 11/12

7s 1/4 7p 0/10 6d 8/12

8s 1/4 8p 0/10 7d 4/12

9s 1/4 9p 0/10 8d 0/12

To convert the lifetimes to absolute transition probabilities the respective branching ratios are required. With increasing main quantum number the branches in the infrared region

of the spectrum resulting from transitions between higher quantum numbers become more

and more important. This is inversely correlated to the availability of branching-ratio data.

We have therefore decided to use theoretical data whenever experimental values are missing

in literature. Though various papers have been published [4,5,6] that list transition

probabilities, no tables exist with a complete set of the data necessary for our purpose. We

therefore calculated the required transition probabilities using the Hartree-Fock code by

Cowan [7]. With the help of this program the data for all transition arrays leading to levels

for which experimental lifetime data are available have been calculated. These transition

arrays are indicated in Fig. 1. A total number of 3 370 transition probabilities has been

obtained in the course of our investigation. The accuracy of these theoretical transition

probabilities is estimated by comparison with the values for the 4s - 4p and the 4s - 5p

transition arrays. While for the 4s - 4p transitions very good agreement was observed,

considerable differences occur for the 4s - 5p transitions, especially for the weak lines. This

result was expected because of strong cancellation in the transition integral for these

transitions. Attempts to improve the agreement by adjusting the energy levels to the

observed ones and by including configuration interaction showed some promise, but were

not yet successful.
V. Helbig et al. 67

Fig. 1: Part of the Grotrian diagram for Ar I indicating those transition

arrays for which calculations have been carried out.

REFERENCES

[1] W. L. Wiese, J. W. Brault, K. Danzmann, V. Helbig, and M. Kock, Phys. Rev. A39,

2461 (1989).

[2] W. L. Wiese, M. W. Smith, and B. M. Miles, Atomic Transition Probabilities, Vol.

II, NSRDS-NBS 22 (1969).

[3j Z. Stryla, H. Pobee, W. Schade, and V. Helbig, Phys. Rev. A41, 512 (1990).

[4] R. A. Lilly, JOSA 66, 245 (1976).

[5] P. E. Grudzev and A. V. Loginov, Opt. Spectroc. 38, 411 (1975).

[6] N. V. Afanaseva and P. F. Grudzev, Opt. Spectrosc. 38, 450 (1975).

[7J R. D. Cowan, "The Theory of Atomic Structure and Spectra," University of

California Press, Berkeley (1981).
CALCULATED Ar XVII LINE INTENSITIES AND COMPARISON

WITH SPECTRA FROM THE ALCATOR C TOKAMAK

K. J. H. Phillips,^ F. P. Keenan,2L. K. Harra,^ S. M. McCann,^ E. Rachlew-Kallne,^

J. E. Rice* and M. Wilson^

Introduction: X-ray spectra from high-temperatiire plasmas such as those formed in tokamak

devices or in soleir flcires eire dominated by lines due to tremsitions in helium-like ions between

the ground {Is^ ^ So) level and 132/ levels. The four most intense lines are due to transitions

from the la2p^P^, U2p^P^, U2p^P^ and 1323 levels to the ground level (called here w,

X, y and z - see Gabriel 1972). The upper levels of these trjinsitions are mainly populated

by electron collisional excitation from the ground level, though cascade and recombination are

also important. The intensity ratio R = z/{x + y) is sensitive to electron density for certain

elements in a range that include those typical of tokamsik plasmas (see Gabriel and Jordan

1969). Also, the intensity ratio G = {x + y + z)/w has a rather weak dependence on electron

temperature Tg. Both the R suid G ratios are useful for diagnosing plasmas for which no direct

measurements are available.

High-resolution spectra from helium-like argon (Ar"*"^®) have been obtained using Mgon-seeded

plasmas in the Alcator C tokamak device at the MIT Plasma Fusion Center (e.g. Rice et ai,

1987). For the intermediate- Z element Mgon, dielectronic satellites due to l3'n/ - l32pn/

transitions in the lithium-like stage are fairly strong, and some of these satellites blend with

the chief Ar xvii lines, so aifFecting the R and G intensities.

X-ray spectra from Alcator C: The experimented details of the Alcator C tokamak are described fully by Rice et al. (1987). The deuteriimi plasma typically has Ng in the range

1 - 2 X 10^* cm"^, Te = 1 - 2 keV, and was seeded with argon atoms having a concentration of

10"^ - 10"'* X Ne- The X-ray emission was measured with a bent Bragg crystal spectrometer,

with spectral range 3.9-4.4 A, so including all the Ar xvii lines £ind Ar xvi dielectronic satellites

of interest. Standard diagnostic techniques were used to find and NeFor the spectra under discussion here, much of the emission originated from centre of the

plasma, where and Ne are highest, and for which any contribution from charge-exchange

(see Kato et al. 1991) is very small.

Calculated Ar XVII spectra: Electron excitation rates from the argon groimd level (l3^ ^Sq)

to the 132/ levels were c<ilculated by Keenan, McCarm, and Kingston (1987) by interpolating

from results for other He-like ions obtained with the iZ-matrix code of Burke and Robb (1975).

^ Astrophysics Division, Rutherford Appleton Laboratory, Chilton, Didcot, Oxon. 0X11 OQX,

U.K.

2 Dept. of Physics, Queen's University, Belfast BT7 INN, U.K.

^ Dept. of Physics I, Royallnstitute of Technology, S10044 Stockholm, Sweden

* MIT Plasma Fusion Center, Cambridge, Mass. 02139, U.S.A.

^ Dept. of Physics, Royal Holloway and Bedford New College, Egham Hill, Egham, Surrey TW20

OEX, U.K.

68
K. J. H. Phillips et al. 69

Other atomic data required in this ejaculation are described by Keenein et al. (1987). Using

these atomic data and a statistical equilibrium code, level populations were derived and hence

Ar XVII line emissivities for a range of and N^.

Dielectronic excitation of the Ar xvi dielectronic satellites was calculated from the pseudorelativistic Hartree-Fock (HFR) code, described by Cowan (1981). Collisional excitation is an

important excitation mechanism for dielectronic satellites of the Is^ 2s - Is2s2p eirray, and the

rates for this were taken from the collision strengths calculated for Fe and Ca by Bely-Dubau

et al. (1982a, 1982b).

"1 I I |- —1 I 1

1

1 1 1 ]

1 1 1

ALCATOR.ARIC

Broken line = Alcator-C spectrum

Electron lemp. = 1.451000e + 07

log Ne (cm"') = 14.5000

V.

3.92 3.94 3.96 3.98 4.00 4.02 4.04 Wavelength (A)

Figure 1. Calctdated spectrtun (sohd line) compared with an argon X-ray spectrum obtained from the Alcator C tokamak, with central values of Te = 1.25 keV and iV^e =

3 X 10^" cm-^

Theoretical spectra were formed by giving each line in the spectrum a profile that is a con- volution of the thermaJ Doppler profile eind the spectrometer's instrimiental width. The final

spectnmi is the addition of the profiles of aU the lines considered. and are free parameters

which cam be chosen for any synthesized spectnmi.
70

The Ar xvii line intensities «dter with Ne through the R ratio and with through the slightly

vMying G ratio, while the dielectronic satellites decretise in intensity with increasing Tg. As

mentioned, some satellites blend with Ar xvii lines, so that any measurement of the R and G

ratios to get densities of, e.g., solar-flare plasmas must take such blends into account.

Comparison of observed and calculated spectra: Several Alcator C spectra were used

for comparison with theoretical spectra as caJculated above. Fig. 1 shows the results of one

such comparison. The values of Tg 2md Ne used in the ctdculated spectrum are those measured

from diagnostic techniques, i.e. and have not been arbitrarily adjusted to obtain the

best agreement between cjJcvdated and observed spectra. Usually these values refer to central

values. Strictly, the theoreticjJ spectrvun should be formed by an integration across the plasma,

taking into account the radial variation of Te and Ne- This will be dealt with in a forthcoming

paper, but meanwhile it can be said that taking central vsdues for Tg and Ng is not expected

to result in large errors as the emission from outer parts of the plasma contribute only a small

amoimt to the intensity, the spectral intensity depending on N^

The agreement between the observed and cjJculated spectra is such that one can be confident

of the accuracy of the atomic ceilculations. The chief disagreement is a difference between the

calculated (too small) zind observed intensities of the collisionally excited satellite known as q. Possibly this is due to the fact that coronal equilibrium, assumed in the Ccdculations, is not

adequate and that particle transport should be taJcen into accotmt.

In simimairy, the good agreement between calculated spectra and those from a well- diagnosed

tokamak plasma lead one to suppose that Ar xvii spectra can themselves be used as temperature

and density diagnostics for plasmas without detailed measurements, such as solar-flare plasmas.

References

F. Bely-Dubau, J. Dubau, P. Faucher, and A. H. Gabriel, Mon. Not. R. Astron. Soc. 198, 239

(1982).

F. Bely-Dubau et ai, Mon. Not. R. Astron. Soc. 201, 1155 (1982).

P. G. Burke and W. D. Robb, Adv. Atom. Molec. Phys. 11, 143 (1975).

R. D. Cowan, The Theory of Atomic Structure and Spectra, Univ. California Press, Berkeley

(1981).

A. H. Gabriel, Mon. Not. R. Astron. Soc. 160, 99 (1972).

A. H. Gabriel and Jordan, C, Mon. Not. R. Astron. Soc. 145, 241 (1969).

F. P. Keenan, S. M. McCann, and A. E. Kingston, Phys. Scr. 35, 432 (1987).

J. E. Rice, E. S. Marmar, E. Kallne, and J. Kallne, Phys. Rev. A, 35, 3033 (1987).

T. Kato et ai, Phys. Rev. A 44, 6776 (1991).
Comprehensive measurements of Fe I oscillator strengths

T. R. O'Brian, M. E. Wickliffe, J. E. Lawler

University of Wisconsin, Madison, WI

W. Whaling

California Institute of Technology, Pasadena, CA

J. W. Brault

National Solar Observatory, Tuscon, AZ

We describe an efficient method for measuring absolute oscillator strengths of moderate precision (generally

10% or better) for essentially every classifiable transition in an atomic spectrum [T. R. O'Brian et al, J. Opt. Soc. Am. B 8, 1185 (1991)]. Both hfetimes and branching fractions are measured for 186 levels in Fe I, yielding

absolute oscillator strengths for 1 174 transitions in the range 225 to 2666 nm, most to 10% or better precision.

Level lifetimes are measured using time-resolved laser-induced fluorescence on a slow beam of atomic Fe. Branching

fractions are measured in emission with the one meter Fourier transform spectrometer at the National Solar

Observatory. The upper level energies of the transitions with measured oscillator strengths densely span the range

30,000 to 61,OCX) cm"^. The extensive set of oscillator strengths permits accurate interpolation of relative upper

level populations in an emission source operating near Boltzmann equilibrium, thus allowing accurate determination

of oscillator strengths for levels not directly interrogated for Hfetimes or branching fractions. An additional 640 Fe I

oscillator strengths are determined by this interpolation, for a total of 1814 accurately measured oscillator strengths.

Level lifetimes are measured using pulsed laser excitation of atoms in a beam generated by a modified

hollow cathode discharge. A pulsed, tunable dye laser, with second harmonic generation in crystals when necessary,

provides spectral coverage from about 205 to 700 nm. The laser is tuned to selectively excite a single upper level

and the subsequent spontaneous fluorescence decay is detected with a photomultiplier tube and fast transient recorder.

Huorescence decays from several hundred laser shots can be recorded and analyzed in less than one minute. Selective

laser excitation eliminates error from growing-in cascades from higher-lying levels, and potential cascade radiation

from decays through lower levels is blocked with simple spectral filtering. The hollow cathode discharge source

generates beams of neutral and singly-ionized atoms for virtually any element. The source has been used for more

than 30 elements so far, including highly refractory metals non-metals. Systematic error from radiation trapping or

non-radiative decay is eliminated by using the optically thin, collisionless beam. The beam also contains significant

populations of atoms and ions in long-lived levels of both parities, as well as the ground level, so that many highlying levels are accessible to excitation with photons of modest energy. In Fe, useful populations of long-lived

levels occur with energies as high as 30,000 cm" ^ permitting excitation of upper levels up to the ionization limit

(63,700 cm'^) without the technical difficulties of using VUV or multiphoton processes.

Branching fractions are measured from emission spectra obtained with the one meter Fourier transform

spectrometer (FTS) at the National Solar Observatory. The FTS provides rapid collection of extensive spectra with

71
72

excellent resolution, broad dynamic range, and accurate absolute frequency calibration. A million point spectrum

covering the spectral range 2,000 to 44,000 cm"^ is collected in about 8 minutes with resolution 0.04 cm'^ (see

Figure 1.). Several spectra are collected using hollow cathode Fe discharges in Ar, Ar + He, and Ar + Ne, and

spectra are also recorded from an inductively-coupled plasma (ICP) source. The high temperature ICP source (about

7000 K) produces broad lines less prone to self-absorption, while the sharper hollow cathode lines are better suited

for spectrophotometry of closely- spaced transitions of moderate or low intensity and for precise identification of peak

transition frequencies. Relative intensities and peak positions are measured automatically with the DECOMP

program, which fits a Voigt profile to all features with signal-to-noise ratios exceeding a specified value.

expanded on

next figure

1 1 1 1 1 I 1 -

resolution element HI0.04 cm"' 4 X

10"* nm

1 1 1 1 1 1 1 31260 31265 31270 31275 31280 31285 31290

Wavenumber

31277 31278 31279 31280

Wavenumber

31281

a. b.

Figure 1. A very small portion of the Fourier transform spectrum of an Fe + Ar hollow cathode discharge used for

measuring branching fractions showing the high resolution and wide dynamic range obtained.

Under appropriate operating conditions, the upper level populations in the ICP source approximate a

Boltzmann distribution, although deviation from local thermodynamic equilibrium is seen in the populations of

shorter-lived levels . Using oscillator strengths determined by measured level lifetimes and branching fractions,

relative populations of upper levels can be determined from ICP spectral line intensities, and a smooth curve fit to

the relative populations as a function of upper level energy. This curve deviates somewhat from the expected

(Boltzmann) inverse exponential dependence on upper level energy (see Figure 2.). However, since oscillator

strengths of transitions from 186 upper levels were measured, and since these upper levels densely span the

excitafion range 26,000 to 61,000 cm" ^ accurate interpolation can be made between relative level populafions based

on directly measured oscillator strengths. This interpolation determines the relative population of upper levels for

which lifetimes were not measured, but for which branching fractions were measured. Interpolation of the relative

upper level population combined with relative emission intensities from the FT spectra then determines the

oscillator strengths of transitions out of these upper levels relative to the directly measured oscillator strengths.
T. R. O'Brian et al. 73

Using this method, moderately precise (10 - 20% uncertainty) absolute oscillator strengths are determined for 640

additional transitions for which upper level lifetimes were not directly measured.

The Fe I spectrum provides a particularly stringent test of the accuracy of this interpolation method, since

precise oscillator strengths for 163 of these transitions have been previously measured by Blackwell et al [Mon.

Not. R. Astron. Soc. 201, 595 (1982)]. For 133 oscillator strengths measured in this experiment by the lifetime- branching fraction technique and by Blackwell et al, the mean value of the ratio g/this experiment / •S/Blackwell

0.95 with sample standard deviation 0.08. For 30 additional lines measured by the interpolation method, the

corresponding ratio is 0.90 ± 0.08. The 8% spread in the ratios is consistent with the fractional uncertainty in the

oscillator strength measurements in this experiment (typically about 10%). These results support the accuracy of the

lifetime-branching fraction measurements and demonstrate no significant difference in the accuracy of the

interpolation method compared to the lifetime-branching ratio technique.

The methods reported here are applicable to efficiently measuring and interpolating accurate absolute

oscillator strengths in the UV through near IR for virtually any neutral or singly-ionized atomic species. Further

understanding of departure from local thermodynamic equilibrium in ICP or other sources may lead to even greater

efficiency by minimizing the number of lifetimes needed for normalization.

-14 +

+

-16

4++

-18

-20

30000 40000 50000 60000

EXCITATION ENERGY (CM-^

Figure 2. Relative upper level population (N^) as a function of the upper level energy for Fe I levels, determined

from relative line intensities in a Fourier transform spectrum of Fe in an ICP source and measured oscillator

strengths. The solid line segment in a least-squares fit to populations of levels above 40,000 cm'^.
MEASUREMENT OF LIFETIMES OF EXCITED STATES OF SELECTED VUV LINES OF NI, Nil,

All I, AND Aim

Santosh K. Srivastava

Jet Propulsion Laboratory, California Institute of Technology,

Pasadena, CA 91109, U. S. A.

Delayed coincidence technique has been employed to measure lifetimes of

upper levels of transitions which give rise to spectral lines in the VUV

region of spectrum of NI, Nil, AlII, and AlIII. Two different instruments were used for these measurements. They are shown in figures 1 and 2. In the first

instrument (fig. 1) a fast pulsed electron beam (Khakoo and Srivastava, 1984)

with cut off times of the order of 0.5 nano seconds was employed to generate

excited NI and Nil states by dissociating N2 which then emitted in the VUV. At

the same time this electron pulse was also used to start a tme to pulse height

converter (TPC) . Emitted radiation was detected by a VUV sensitive fast

channeltron. Output of this detector was amplified and sent to the stop

teminal of the TPC. The TPC converted the time difference between start and

stop pulses into an electrical pulse whose height was directly proprtional to

the time difference. Pulses of varying heights corresponding to various times

of arrivals of photons were stored in a pulse height analyzer (PHA)

Collection of pulse height data over a period of time gave a time decay curve. A typical time decay curve is shown in fig. 3. Such decay curves were obtained

for each spectral line of interest. At least: five different sets of data were obtained to test the reproducibility of results. In the second instrument a fast pulse (100 ps wide) of a Nd:YAG laser was em.ployed to generate a laser

produced plasma of Al . This plasma emitted radiation in the VUV. Spectrum

analysis of the emitted radiation showd that it contained well defined

spectral lines of Al from its various stages of ionization. Details on the

characteristics of the plasma and method of its production are given in our previous publication (Timmer et al., 1991). Method of obtaining the temporal

decay curves for each spectral line was the same as described above for the

first instrument.

The upper level of a transition of interest is generally populated by

two mechanisms: one by the direct excitation from the ground state and the

other by cascade transitions from higher levels. Therefore, the time decay

curves such as shown in fig. 3 contain cascade contributions which lengthen

the true lifetime of the excited state. In the past the effect of cascading

has been estimated by plotting a log of the intensity of the spectral line as

a function of time. Without the effect of cascade this plot should be a straight line. Any departure from a straight line shows the contribution due

to cascading and its value can be estimated. For this purpose we have used the

two component decay method described by Corney (1977). This method combines

the cascading contribution of all of the upper levels into one and devides the

exponential decay formula into two parts: one for the direct excitation and

the other for the cascade contribution. The experimental decay curves are fitted to this formula by a ^ minimization technique. We have wrtitten

programs (Srivastava and Nguyen, 1986) which use this technique to fit the

present experimental curves to the two component formula of Younger and Wiese

(1978)

Our experimental results for NI and Nil are presented in Tables I and II

along with previously reported ones. As is clear from these tables that the

various results differ considerably from each other. We esimate that our results are accurate to within 20%. This error has been arrived at by

estimating the spread in our measured data and fitted data. A typical fitted

curve is shown by a solid line in fig. 3. We were able to fit our measured

74
Santosh K. Srlvastava 75

data to the two component formula of Younger and Wiese well. The main reason

for the differences in the results of various measurements lies in the fact

that all previous and present measurements have serious cascade contributions

which have been estimated differently by different investigators.

Values of lifetimes of AlII and AlIII lines are presented in Tablelll.

Previous experimental results are not readily available for these lines. Decay

curves for each spectral line were fitted to the theoretical formula of

Younger and Wiese (1978). A typical fitted curve is shown in fig. 3, It is

estimated that the present results are accurate to within 20%.

Acknowledgements : The research described in this paper was carried out at the

Jet Propulsion Laboratory, California institute of technology, and was sponsored by NASA. The help in acquiring and reducing the experimental data by

C. Timmer and H. Nguyen is greatfully acknowledged.

References :

Corney, A., in "Atomic and Laser Spectroscopy", Clarendon Press, Oxford,

England, ppl60(1977).

Khakoo, M. A., and S. K. Srivastava, J. Phys. E: Sci . Instrum. 17, 1008

(9184) . Srivastava, S. K. and H. Nguyen, "Paramt rization of Electron impact Cross

Sections for CO, C02, CH4, NH3 and S02" JPL Report #87-2 (1987)

.

Timmer, C, S. K. Srivastava, T. I. Hall, and A. F. Fucaloro, J. Appl . Phys

70, 1888 (1991) . Younger, S. M. and W. L. Wiese, Phys Rev. A17, 1944(1978).

'0

rtj

i-iVM Ijl PULSER

£CTION

II OL^^CTIO;,

LIMITING APE/mjRE

:p£ctrometer

PULSE 1 HEIGHT 1

i ?ULS

j ANALYSES j ISWPERf

'MCA I

I

I COMPUTER

XY <• t X*" Y

Fie. 1

nanomecer

Seam

Expanaer

MO VAG Laser

I

)w I Target^Sx

1^

vacuum

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Fig. 2

Fig. 3
76

TABLE I TABLE II

Lifetimes for 1134.6 A° Line of NT

Reference Lifetime (ns

Method

Lawrence and Savage (1966) 7.2 Phase shift Wiese et al. (1966) 4.34S Smith et al. (1970) 7.4 Phttse shift Berry et al. (1971) 7.0 Beam foil Hutchinson (1971) 9.9-1 Modified Phase shift Chang (1977) 3.18 Beam foil Hibbert et al. (19S5) 8.264 Present work 2.8=0.56 Delayed coincidence

Lifetimes for 1199.9 A' Muitiol of NI

Reference Lifetime (ns) .MetnOu Lawrence and Savage (1966) 2.5=0.3 Phase- shift Wiese et al. (1966) 1.852 Ben7 et al. (1971) 2.4±0.1 Beam foil Hutchinson (1971) 2.2±0.4 Phase shift Dumont et al. (1974) 2.35± Beam foil Brooks et al. (1977) 2.4±

Chang (1977) 2.27±0.11 Beam foil Hibbert et al. (1985) 2.32 Phase shift Present work 3.2±0.64 Delayed coincidence

Lifetimes for 1243 A" Line of NI

i Reference Lifetmie ( na i .Method

} Wiese et al. (1966) 2.174

1 Lawrence and Savsige (1966) 2.2±0.3 PhsLse shift Berry et al. (1971) 2.6 B«ajn foil Hutchinson (1971) 6.9=0.8 Phase shift Goldbach et al. (1986) 2.857 .\rc Present work 1.1±0.22 Delayed coincidence

Lifetimes for 671.48 A° L ine of NTT

Reference Lifetime (ns) Method

Buchet e tai. (1972) Smith et al. (1970) Hutchinson (1971) Chang (1977) Present work

0.82

1.08

1.08 0.67 1.3±0.26

Beam foil Phase shift Phase shift Beam foil Delayed coincidence

Lifetimes for 775.957 A" 1.ine of NTT

Reference Lifetime (ns) Method

Smith et ai. (1970) Chang (1977) Present work0.7 0.52 0.25=0.05

Phase shift Beam foil Delayed coincidence

Lifetime?^ for 748 A° Line of NTT Reference Lifetime (ns) Method

Hesser and Lutz (1968) 0.8=0.4 Phase shift Knystautas et al. (1973) 0.43=0.01 Beam foil Kemahan et ai. (1974) 0.213±0.01 Beam foil Dumont et al. (1976) 0.22±0.03 Beaxc foil Sorenson (1979) 0.35=0.01 Beam foil Baudinet-Robinet et al. (1990) 0.267 Bejun foil Tripp et al. (1991) 0.1125 Electron Impact

Present work 0.4±0.08 Delayed coincidenct

Lifetime-; for 10S5 A' Line of NTT

Reference Lifetime (ns i Method

Smith et ai. (1970) 0.92 Phase shift Hutchinson (1971) 2.7 Modified phase shift Chang (1977) 2.8 Beam foil Present work 3.0=0.6 Delayed coincdence

TABLE III

Lifetimes of upper levels of transitions listed below as utilizing the laser produced plasma of Al

measured by

Species Transition Wavelength (A) Lifetime (ns)

AlII 3s3p-3s7s 990, 991 2. 63

AlII 3s3p-3s5d 1049 . 9 3 . 45

AlII 3s3p-3s5s 1209, 1210 3.75

Aim 4s-7p 1262 3.49
OSCILLATOR STRENGTH MEASUREMENTS

OF NEUTRAL NITROGEN LINES IN THE 900 - 1200 A RANGE

C. Goldbach\ T. Ludtke2, M. Martin\ G. NoUezi

^ Institut d'Astrophysique, Paris, France

^ Institut fur Experimentalphysik, Kiel, Germany

The far UV rfinge offers two main interests: first, most of the lines of the elements of astrophysical interest lie in this spectral range, second a given element exhibits often lines with very different

oscillator strength VcJues, which allows to analyse absorption features corresponding to complex

lines of sight. On the other hand, the experunentcil techniques have greatly improved and it is possible to extend to the VUV the classical emission method of oscillator strength measurement

without ajiy dramatic loss of precision. The technical improvements relate to crucial experimental

points: realisation of high resolution VUV spectrometers, of efficient differential pumping units, of

VUV radiation stcindcirds, computer control in data acquisition and analysis. Also the accuracy

reached now on the lifetime data edlows the normcilisation to an absolute scale of the measured

relative /-values.

Having measured /-values of strong and weeik lines of neutral nitrogen and carbon in the

1200-2000 A reinge, we are now extending our measurements to the 900-1200 A range. Neutral

nitrogen lines of this region are of pcirticiilar interest for Lnterstellair medium and quasi- stellar object

absorption system studies and no reliable laboratory data are available: we present hereafter the

results of /- measurements for 19 lines of neutretl nitrogen, belonging to 9 multiplets, between 950

and 1200 A .

The experiment

The emission source is a wall stabilised arc operated in high-purity argon and at a 80 A

current(T=13000 K; ng = 1.1 lO^^cm"''). The arc radiation is observed axially through a threestage differential pumping unit which reduces the atmospheric pressure down to 10"'' mbar. The

first orifice (tungsten, 0.6 mm dizimeter, 0.6 mm length) is placed only 4 mm from the anodes

to keep the cool plasma boundary layer as short as possible. The mirrors and the grating of the

2.5 m normal incidence monochromator eire platimma coated. The entrance and exit slits are set to 50 fi cind the spectrcJ resolution is about 0.1 A . A windowless miiltiplier serves as detector.

The method

The method, ein advanced version of the emission method avoiding the difficulties associated

with an absolute nimiber density determination in a multi- component plasma, is based on relative

/-measurements. A reliable and precise /-value of the line standing for reference is required;

fortunately, the lifetime of the upper term of the NI miiltiplet at 1200 A is known with a good

accuracy: the lifetimes measured through different techniques ([1] to [6]) yield a weighted mean

value of 2.35 ±0.06 ns. In the case of strong lines, and in particulsir of resonance lines, the line optical depth is not

negligible. To take full account of this effect, the quantity we choose to determine is the optical

depth profile of the line Tx (see [7] eind [8]). The relative ^/- value of a line is deduced from the ratio

of the integrated optical depth of the investigated line (X) to that of a reference line (R) through
78

where g and E are the statistical weight and the excitation energy of the lower level of both

transitions, tx is determined from the end-on measured spectral radiemce Ix through

r, = -ln(l-^) (2)

where Bx is the Planck function at the plasma temperature. The blackbody saturation level Bx is measured at the top of the line by increasing the nitrogen concentration.

Most of the investigated transitions appear as multiplets of overlapping and blended lines

of nearly Gaussian shape. The determination of the integral of tx over the profile of each line

(including wing contributions) is performed using least-squares fitting technique of digital data.

For all the measured lines, but multiplet Uf3.06, we use as reference the 1200.71 A line of

multiplet uvl. For the weak forbidden multiplet uv3.06 at 952 A , we choose as reference the

965.04 A line of the multiplet uv3 with gf= 0.0131 ±5%, our present result. For resonance lines, as the temperature disappears from Eq.(l), the imcertainty on the absolute

gf-value is obtained by summing in quadrature the stcindard deviation of the distribution of the

measiired line ratios (between ±3 and ±10%), the uncertainty in the realisation of the blackbody

plateau (±2%) and the imcertainty in the y /-reference vaJue. For other lines, an uncertainty of ±3% in the Boltzmann factor arising from the imcertainty

in the temperature has to be added.

Results

The following table displays the results of our measurements, together with the largely used

values given by Lugger et al. [9], the results of the calculation of Bell and Berrington [10], of

Lernion and Burke [11] (Opacity Project) and the new results of Hibbert et al. [12].

Our absolute sczile is only 2.5% lower than Lugger et £j. eind 15% higher than Hibbert et

al., but discrepancies on forbidden lines may reach 50%. Comparison with the results of [10] concerns only the three allowed multiplets uv2, uvZ and uu3.05; because of LS-coupling depcirtuje

exhibited by our measurements, the noteworthy agreement stated for the multiplet values would

be significantly lower for the line values. The same remark applies also to the Opacity results with

which our measurements agree very weU with the noticeable exception of multiplet uv2.

A detailed comparison between our experimental values and the results of different theories

[10], [11], [12] shows that the agreement level vairies according to the data considered (multiplet- or line- values) ajid to the nature of the transitions (resonant or not, allowed or forbidden).

References

Lawrence G.M., Savage B.D., 1966, Phys. Rev. ,141, 67

Berry H.G., Bickel W.S., Bashkin S., DesesqueUes J., Schectman R.M., 1971,

J. Opt. Soc. Am., 61, 947

Hutchison R.B., 1971, JQSRT, 11, 81

Dumont P.D., Biemont E., Grevesse N., 1974, JQSRT, 14, 1127

Chang M.W., 1977, ApJ, 211, 300

Brooks N.H., Rohrlich P., Smith W.H., 1977, ApJ, 214, 328

Goldbach C, Martin M., Nollez G., Plomdeux P., Zimmermann J. P., Babic D., 1986,

A&A,161, 47

Goldbach C, NoUez G., 1987, A&A, 181, 203

Lugger P.M., York D.G., Blanchard T., Morton D.C., 19^8, ApJ, 224, 1059

[10] BeU K.L., Berrington K.A.,1991, J. Phys. B, 24, 933

[11] Lennon D.J., Burke V.M., 1992, private communication

[12] Hibbert A., Biemont E., Godefroid M., Vaeck N., 1991, A&AS, 88, 505
C. Goldbach et al. 79

Table 1. Absolute g/-values for neutral nitrogen resonance lines. Length and velocity values are given for theoretical results.

A (A)

This work HBGV[12] BB[10] LYBM[9] Opacity[ll]

9io 3/ gf gf gf gf

UV3.06 25^2^3 - 2a22p23£i

952.3037 4 6 0.0075 ± 7% 0.0160-0.0144 0.010 ± 12%

952.4151 4 4 0.0068 ±6% 0.0172-0.0156 0.008 ± 16%

952.5231 4 2 0.0024 ± 10% 0.0076-0.0068 0.0017 ± 12%

UV3.05 2a22p3 "^S^ - 2522p23d

953.8 4 12 0.30 0.264-0.239 0.312-0.277 0.27 0.28-0.26 953.4150 4 2 0.057 ± 8% 0.0444-0.0400 0.048 ± 8%

953.6548 4 4 0.108 ± 7% 0.0852-0.0772 0.084 ± 5%

953.9698 4 6 0.135 ± 7% 0.134-0.122 0.14 ± 9%

UV3.04 2*22^3 450 - 2522p23d 2_p

954.1040 4 6 0.027 ± 25% 0.0008-0.0004 0.034 ± 9%

uv3 2s'^2p^ ^ 5« - 2j22p24, 4 P

964.4 4 12 0.109 0.126-0.118 0.103-0.104 0.120 0.128-0.124

963.9904 4 6 0.059 ±8% 0.0644-0.0600 0.056 ± 7%

964.6258 4 4 0.037 ± 5% 0.0416-0.0388 0.040 ± 10%

965.0415 4 2 0.013 ± 5% 0.0204-0.0192 0.024 ± 7%

uv2 2s2 2p3 4 5« - 2a22p4 4p

1134.7 4 12 0.34 0.322-0.446 0.349-0.378 0.322 0.092-0.124

1134.1651 4 2 0.061 ±6% 0.0552-0.0760 0.054 ± 2%

1134.4147 4 4 0.114 ± 7% 0.109-0.150 0.107 ± 2%

1134.9801 4 6 0.162 i 6% 0.158-0.220 0.161 ± 2%

uv41 2s22p3 2pO 2522p235 25

1143.6458 2 2 }0.35± 8%

1143.6508 4 2 uv6 2s22p3 2 - 2522p23£i

1167.9 10 14 0.32 0.45-0.30 0.34-0.31 1167.4484 6 8 0.20 ± 7% 0.258-0.175

1168.4167 6 6 }0.12± 10%

0.0066-0.0054

1168.5358 4 6 0.186-0.124

UV6.01 2s22p3 2£)0 - 2s22p23ci *P

1168.3344 4 6 0.029 ± 8% 0.0012-0.0008

UV5.02 2s22p3 2j)0 - 2s22p24j 2p

1176.9 10 6 0.13 0.05-0.15 0.125-0.120

1176.5097 6 4 }0.088±8%

0.0276-0.0864

1176.6304 4 4 0.0036-0.0096

1177.6948 4 2 0.044 ± 11% 0.0184-0.0500

Sun and Stars

OBSERVED REDSHIFT OF O V LINES IN SOLAR UV SPECTRA

p. BREKKE

Institute of Theoretical Astrophysics, of Oslo

University of Oslo, P.O. Box 1029, BUndem, N-0315 Oslo 3, Norway

Ultraviolet observations of the Sun show a net redshift near disk center in the emission lines from the

transition region. During the last decades, this phenomenon has been observed with several UV instruments

with different spatial resolution (e.g. Doschek, Feldman, Bohlin 1976; Gebbie et al. 1981; Dere, Bartoe,

& Brueckner 1986; Hassler, Rottman, & Orral 1991). Systematic redshifts have also been observed in stellar spectra of late type stars (e.g. Ayres, Jensen, & Engvold 1988). Both solar and stellar flows in the transition region have been most extensively studied at temperatures around T = 10^ K. For the Sun, the typical value

of the average downflow velocity, derived from the C IV lines at 1550 A, is 5-10 km s~^. Measurements of the variation of the flow with temperature are somewhat ambiguous. However, the

net downflow velocity has been observed to increase with temperature, reaching a maximum at T= 10^ K

and then decreasing again at higher temperatures. The Ov lines at 1218 A and 1371 A define the highest

observable transition region temperatures available in the wavelength range of most high resolution, normal

incidence UV slit spectrometers. Of these two lines, which also form a density sensitive pair, the 1218 A

line is the one most readily available for observation. The reason being that the photographic density of the

intrinsically weak line is lifted up by the wing of the neighboring strong Lya line from hydrogen.

Some observers find no significant shift in the OV line at 1218 A at disk center (e.g. Doschek et al. 1976). It should be noted that the commonly quoted average velocity variation with temperature above 10^ K to a large extent depends on this particular observation of the 1218 A line. The result of Doschek et al. (1976) has been used in comparison with numerical simulations of flows in the transition region, where the

redshifted emission is replaced by blueshifted emission at temperatures around 2.5 x 10^ K where O V is formed (e.g. McClymont & Craig 1987, Spadaro, Antiochos, & Mariska 1991).

However, results from the observed wavelength of this line, as presented by Doschek et al. (1976) should

be regarded with some caution for the following reasons:

- The wavelength determination of the O V line may be influenced by the Lya line from hydrogen at 1215.67 A.

- The solar wavelength calibration is uncertain owing to few chromospheric reference lines in this wavelength region.

- The laboratory wavelength of the oxygen Une at 1218 A is uncertain.

The last point is crucial for the determination of absolute velocities. Doschek et al. (1976) tried to avoid

this problem by comparing the measured wavelengths with measurements of the same lines outside the solar limb where they expected no net shift of the lines. A detailed analysis of O V was presented by Bockasten & Johansson (1968). They recalculated the energy levels fitom measurements of 126 lines between 340 A and 7700 A observed with a theta-pinch

discharge as the light source. Their wavelength value for the 2s- ^Sq—2s2p ^Pj line was 1218.406 A. The

value of Bockasten and Johansson is commonly used in reference literature. It has been known for a long

time that the observed solar wavelength of the 1218 A line differs significantly from the wavelength reported

by Bockasten & Johansson (1968). Using the NRL 6.6 m spectrograph Brown (1980) found the wavelength

to be 1218.344 ± 0.010 A, which is in better agreement with solar observations.

In this paper we present measurements of Doppler shifts in the O V lines at 1218 A and 1371 A obtciined during two rocket experiments with the High Resolution Telescope and Spectrograph - HRTS. The result

is compared with corresponding measurements of the Si IV line at 1402 A and the OlV line at 1401 A. We

discuss variation of velocities in the O V lines over the entire field of view of the HRTS instrument, which

extended from disk center to outside the solar limb.

83
84

The High Resolution Telescope and Spectrograph - HRTS - is described by Bartoe &: Brueckner (1975).

The particular strength of the HRTS instrument lies in its high spatial, spectral, and time resolution combined

with the extensive wavelength and angular coverage. For this investigation we have used data from the two

first HRTS rocket flights which took place in 1975 and 1978 respectively. During both missions the slit extended from the solar center to the limb covering both quiet and active regions.

The spectrograms were registered on photographic film. Microphotometry of the spectrograms has been

carried out at the Institute of Theoretical Astrophysics in Oslo and at the US Naval Research Laboratory.

A description of the photometry and of the various steps in the reduction process is given by Brekke et al. (1991).

OV X1371 292 2000

1500

c

o« 1000 -

o

500

- Solar Limb

1

Sunspol

Plage

100 arcsec

Ref line C 1

\ ! 364 164 A

-20 -10 0 10 20 V (km/s)

-10 0 10

Figure 1. Spatial variation of Line-of-sight velocities in the OV Line at 1371 A and a chromospheric

reference line (CI A1364.164 A) observed with HRTS 1. To the left is a section of the HRTS 1 spectrogram

showing the O V profile extending from approximately disc center to the solar limb. The active region

McMath 13766 has been marked. The sceile along the spectrograph slit is given in pixel units where 1 pixel

corresponds to approximately 075.

In Figure 1 the spatial variation of the observed line-of-sight velocities in the Ov line at 1371 A is displayed together with a section of the HRTS 1 spectrogram showing the Ov profile. The image extends

from approximately disk center (cos^ = 0.99) to the solar limb and the location of the active region McMath

13766, including a sunspot, hcis been marked. The scale along the spectrograph slit is given in pixel units where 1 pixel corresponds to approximately 0'.'5. The O V line is clearly redshifted at most positions along the slit corresponding to an average line- of-sight velocity of 8 km s~^ in the quiet regions. Close to Sun center the measured redshifts give a net

radial downflow. There is considerable spatial variation along the slit, where the flow velocities are varying

between -3 km s~^ to almost 20 km s~^ at the solar disk. The blueshift is located above the sunspot umbra

and outside the limb. For comparison, the observed shift of a nearby chromospheric reference line (the Cl

line at 1364.164 A) has been plotted on the same velocity scale. The measured redshift shows no strong

center-to-limb variation. When measuring the 1218 A line we have adopted the laboratory wavelength from Brown (1980) of

1218.344 A. Using this value we find an average net redshift of approximately 3 ± km s~^ in the quiet

regions. This is approximately 5 km s~^ less than the Vcilue obtained from the line at 1371 A. The difference

is probably due to an error in the adopted laboratory wavelength of the 1218 A line, which is an intersystem
p. Brekke 85

line and thus, more difficult to measure in laboratory. The result suggests a laboratory wavelength close to 1218.325 A if the two lines are to have the same redshift. The observed Doppler shifts in transition region

and coronal lines has been summarized in Table 1. In addition to Ov we have also mecisured Si IV, OlV,

and Fe XII.

TABLE 1 Observed average redshifts in transition region; HRTS 1 Laboratory Temperature Line of Sight Line of sight

Wavelength of Velocity Velocity

Formation Quiet Region Plage

Ion (A) (K) (km s-i) (km s-^)

Sirv 1402.770^ 7.0 xlO^ 5 ± 2 14 ± 2 OlV 1401.156- 1.4 xlO^ 6 ± 2 14 ± 2 0 V 1371.292^ 2.4 xlO^ 8 ± 2 8 ± 2 O V 1218.344'' 2.3 xlO^ 3 ± 2 4 ± 2 FeXII 1249.40^ 1.3 xlO^ 7 ± 4

1 — Moore 1965, 2 — Bromander 1969, 3 — Bockasten & Johansson 1968

4 — Brown 1980, 5 — Sandlin et al. 1977, (Solar observation)

I am indebted to Drs. Guenter E. Brueckner and Kenneth P. Dere for making the excellent HRTS

material available. I will also thank Drs. Philip G. Judge and Charles M. Brown for interesting discussions.

I also wish to acknowledge support from the Norwegian Research Council for Science and the Humanities.

REFERENCES

Ayres, T. R., Jensen, E., & Engvold, O. 1988, ApJS 66, 51

Bartoe, J.-D. F., & Brueckner, G. E. 1975, J. Opt. Soc. Am., 65, 13

Bockasten, K., & Johansson, K. B. 1968, Arkiv f. Fys. 38, No 31. 563

Brekke, P., Kjeldseth-Moe, O., Bartoe, J.-D. F., & Brueckner, G. E. 1991, ApJS, 75, 1337 •

Bromander, J. 1969, Arkiv f. Fys., 40, 257

Brown, C. M. 1980, A&A. 88, 273

Dere, K. P., Bartoe, J.-D. F., & Brueckner, G. E. 1986, ApJ, 305, 947

Doschek, G. A., Feldman, U., & Bohlin, J. D. 1976a, ApJ, 205, L177

Gebbie, K. G., et al. 1981, ApJ, 251, L115

Hassler, D. M., Rottman, G. S., & Orral, F. Q. 1991, ApJ, 372, 710

McClymont, A. N., & Craig, I. J. D. 1987, ApJ, 312, 402

Moore, C. E. 1965, NSRDS-NBS, 3, Section 1

Sandlin, G. D, Brueckner, G. E., & Tousey, R. 1977, ApJ, 214, 898

Spadaro, D., Antiochos, S. K., & Mariska, J. T. 1991, ApJ, 382, 338
RUTHENIUM STELLAR ABUNDANCE DETCRMINED FROM FTS BRANCHING

RATIOS, LIE LIFETIMES AND HST OBSERVATIONS

S. Johansson, A. Joueizadeh, U. Litzen

Lund University

J. Larsson, A. Persson, S. Svanberg

Lund Institute of Technology

D.S. Leckrone, G.M. Wahlgren

Goddard Space Flight Center

1. INTRODUCTION

Selected intervals of the UV spectrum of the chemically

peculiar B-star x Lupi have been recorded with the Goddard

High Resolution Spectrograph (GHRS) onboard the Hubble Space

Telescope. In one of the intervals, two unidentified lines

at 1939 A were found to coincide with Ru II lines.

In order to firmly establish the Ru II identification and to

determine the ruthenium abundance in x Lupi, accurate

wavelengths and oscillator strengths for the two lines are

needed. The wavelength measurements are described in the

contribution by Joueizadeh and Johansson (A Progress Report

on the Analysis of VUV-FTS spectra of Ru I and Ru II).

For the oscillator strengths, lifetimes and branching ratios

have to be measured.

2. LIFETIME MEASUREMENTS USING LASERINDUCED FLUORESCENCE

2.1 Generation of ruthenium ions

Ruthenium is an expensive and brittle metal, evaporating

only at very high temperatures. A special method was

therefore used for producing the ruthenium ions in a laser-produced plasma. A smooth ruthenium surface was formed

by vibrating a container with ruthenium powder by means of a

small loudspeaker. A ruthenium plasma was generated by

focusing 10 - 50 mJ pulses from a Nd:YAG laser onto the

powder surface. Due to the vibration, a new smooth surface

was formed before the next laser pulse arrived 100 ms later.

2.2 Excitation and detection

The short, tunable laser pulse for the excitation was

generated by using the second harmonic from a Nd:YAG laser

to pump a dye laser. The output from the tuned dye laser was

then mixed with the fourth harmonic of the pump laser to

produce the radiation in the 1939 A region. By optimizing

the difference in optical path length between the dye laser

radiation and the fourth harmonic from the Nd:YAG laser, a

pulse length of 3 ns was obtained.

86
S. Johansson et al. 87

The fluorescence emitted when the exciting pulse was tuned

to resonance with one of the Ru II lines was recorded with a

microchannelplate photo-multiplier connected to the data

collecting system. Lifetimes were extracted by fitting a convolution of the system response function and an exponential to the recorded fluorescence decay.

The lifetimes of the upper levels for the two Ru II lines

were found to be 2.7 ns and 2.6 ns, with an estimated

uncertainty of 10%.

3. BRANCHING RATIOS FROM FTS RECORDINGS

The Ru II spectrum emitted from a hollow cathode (Ni cathode

+ Ru powder + Ne and Ar carrier gas) was recorded at the

Lund VUV FTS in the region 3000 - 1800 A.

The two Ru II lines at 1939 A have the upper levels

and z^D^^2' The decay schemes involve numerous decay

channels, but only 5 and 6 respectively are strong enough to

be observed, and to significantly influence the branching

ratios

.

Two different methods were used for the efficiency calibration of the spectrometer. In a separate recording an

efficiency curve was obtained from a calibrated D2 lamp. A

disadvantage with this method is the fact that the hollow

cathode window, which may be contaminated from cathode

sputtering, is not included in the calibration. For this

reason internal calibration points from accurately measured

Ar II branching ratios were also used. In an attempt to

extend the internal calibration to shorter wavelengths also

Ge I lines were used. The Ge lines were emitted from a small

amount of germanium powder placed in the cathode.

4. RESULTS

The branching ratios for the two 1939 A lines are found to

be very sensitive to the shape of the calibration curve at

the short wavelength end. More accurately measured branching

ratios for internal calibration below 2500 A are expected to

be available soon. Pending this information, we only state

that the measured lifetimes and the preliminary branching

ratios give the oscillator strengths 0.15 - 0.18, i.e.

log gf in the range -0.82 to -0.74.

A synthetic spectrum fitted to the observed spectrum of

X Lupi, using the new laboratory wavelengths and the

preliminary oscillator strengths, indicates that ruthenium

is about 2 dex (100 times) more abundant in x Lupi's

atmosphere than in the sun.
Investigating the Pt III Spectrum in Chemically PecuHar Stars

Glenn M. Wahlgren^ David S. Leckrone^, and Sveneric Johansson"^

1 Computer Sciences Corporation/GHRS Team, Code 681, GSFC, Greenbelt, MD 20771

2 Code 681, NASA/LASP, GSFC, Greenbelt, MD 20771

Lund University, Department of Physics, Solvegatan 14, S-223 62 Lund, Sweden

1. INTRODUCTION

Recent advances in astronomical instrumentation and laboratory spectroscopy have made

it possible to search for Pt III in stellar spectra. The chemically pecuUar star x Lupi (Bp,

HgMn) is known to display strong spectral features of very heavy elements, such as Pt, Au,

and Hg. Its extremely sharp spectral lines are due to minimal turbulence in its atmosphere and

an inherently slow rotational velocity. Its projected rotational velocity of 1 km sec"-"- is similar

to that of the Sun, but is two orders of magnitude below that typical for stars of its spectral

type. Our investigations of this star to date have been primarily concerned with determining

the abundance and isotope mixture of Hg (Leckrone et al. 1991). However, it is clear that

similar analyses are required for other heavy elements, as for example the 5d 6s configuration

elements, to test theories of abundance enhancement in the atmospheres of chemically peculiar

stars.

It has also become necessary to understand the platinuum spectrum as its many transitions

are a non-negligible source of Hne opacity in the ultraviolet which can therefore be blended

with other atomic lines of interest. The line-formation region temperature in the photosphere

of X Lupi is hot enough ( 6,500 - 11,000 K ) to expect the Pt III number density to be up

to a few percent of the total Pt present, and therefore produce observable Unes in the steUar

spectrum. A platinuum lamp, which provides standard wavelength calibrations for the Goddard

High- Resolution Spectrograph (GHRS) on-board the Hubble Space Telescope, has been used to

analyse the Pt I/II spectra (Reader et al. 1990) and serves as a map for the Pt II lines in the

X Lupi spectrum. But the lamp is not energetic enough to produce a Pt III spectrum. This

has now been partially remedied by the laboratory Pt III analysis of Ryabstev et al. (1992).

Pt III transitions can now be identified in high-dispersion ultraviolet spectra of Pt-rich stars,

which will allow the observed hne strengths to serve as constraints on theoretical calculations

and atomic models.

88
Glenn M. Wahlgren et al. 89

2. STELLAR SPECTRA

The GHRS was used, in its eclielle mode, providing spectral resolving powers between 80,000

and 90,000. Spectra were obtained at three wavelength settings, centered at 1741, 1848, and

1942 A, totalling approximately 30 A of spectral coverage. Signal to noise levels varied between

60 and 100 at the stellar continuum level. Included in the standard data reduction procedures

are wavelength corrections that account for spacecraft orbital motion, transformation of coordinates to the heliocentric rest frame, stellar radial velocity, and spectrum drifts across the

detector array due to the spacecraft magnetic and thermal environments. The wavelength scale

is established by Pt lamp spectra taken at standard wavelengths with an accuracy of 0.05 A for echeUe spectra. We have improved the accuracy of the absolute wavelength scale to ± 0.001 A

using Fe II and Mn II transitions appearing in the stellar spectrum, whose wavelengths were measured with the FTSs at Lund and Imperial CoUege, London.

3. ATOMIC PARAMETERS

This study was initiated as a result of recent work by Ryabstev et al. on the Pt III spectrum.

Their measurements of Pt spark spectra below 2020 A resulted in cataloging 850 transitions.

Their wavelength accuracy is quoted as 0.005 A, set by the Pt II analysis of Sansonetti et al.

(1992) for those transitions observable in our stellar spectra. The intensity calculations by

Ryabstev et al., using the Cowan code, produced values for gA which we have transformed into

the gf-values required by our synthetic spectrum code. Line broadening by thermal, Stark, and

van der Waals mechanisms is included in our synthetic spectra.

4. RESULTS

We have positively identified spectral hues resulting from Pt III transitions in the x Lupi

spectrum. A synthesized stellar spectrum was generated with the computer code SYNTHE

(Kurucz, private communication) for comparison with the observed spectra. The Pt III lines

were typically found at wavelengths near the measured values of Ryabstev et al.. Line strengths

were matched by varying the stellar Pt abundance. A total of nine lines, determined to be

relatively free of contaminant blending, were used in the abundance analysis. Averaging the

best fit abundances from these lines yielded a Pt III abundance by number relative to hydrogen

of [log N(Pt III) / log N(H)] = -5.75, which is nearly 30,000 times greater than in the solar

photosphere. The Pt III abundance is similar to the Pt II abundance of -5.95 which we obtained

in a similar manner from four Pt II lines, and which agrees with an earlier Pt II analysis for

this star (Dworetsky et al., 1984). The figure below displays a one angstrom segment of the x
90

Lupi spectrum compared with synthetically derived spectra for the two cases: 1) the best fit Pt abundance, and 2) the solar Pt abundance.

The Pt analyses for x Lupi will continue as further observations of this star are made, and

will be extended to other stars. A valuable, but missing, piece of the analysis is the isotopic

structure of Pt II/III Unes found in the ultraviolet, which would provide additional clues to understanding the anomalous abundance enhancements.

ACKNOWLEDGEMENT: The authors thank J.-F. Wyart for sending to us a copy of the

Pt III paper prior to publication.

REFERENCES

Dworetsky, M. M., Storey, P. J.., and Jacobs, J. M. 1984, Physica Scripta, T8, 39

Leckrone, D.S., Wahlgren, G. M., and Johansson, Se. G., 1991, ApJ, 377, L37

Reader, J., Acquista, N., Sansonetti, C. J., and Sansonetti, J. E. 1990, ApJ Suppl., 72, 831

Ryabstev, A. N., Wyart, J.-F., Joshi, Y. N., Raassen, A. J. J., and Uyhngs, P. H. M., 1992

submitted to Physica Scripta

Sansonetti, J. E., Reader, J., Sansonetti, C. J., and Acquista, N. 1992, J. Res. Natl. Inst.

Stand. Tech., 97, 1

1740.6 1740.8 1741.0 1741.2 1741.4 1741.6 1741.8

Wavelength (A)
Burst Models for Line Emission in the Solar Atmosphere.

J. M. Laming, SFA Inc. Landover, MD 20785.

U. Feldman, E. O. Hulburt Center for Space Research,

Naval Research Laboratory, Washington DC 20375-5000.

Earlier papers (Laming & Feldman 1992, Feldman et al. 1992) have analyzed spectra

which present problems of interpretation when the data are compared with model plasmas

which assume thermal and ionization equilibrium. The Lyman series of hydrogen-like He

II in an impulsive flare, and the resonance to intercombination line ratio R of magnesiumlike Fe XV (/ {3s3p ^Pj - 3^2 ^Sq) /I (3s3p ^ - 3s^ ^ So)), have both been understood

in terms of a burst model, in which these ions emit their radiation from an ionizing plasma.

The electron temperature is raised from some value at or below that where the ion in question is formed in ionization equilibrium, to a value, say, twice the equilibrium temperature.

In the case of He II, the fundamental problem regarding its observed strength, i.e. that much more radiation from He II is observed than predicted, is obviated in a burst

model, since the increase in the Boltzmann factor produced by the increase in the electron

temperature enhances the emission rate. Since the timescale of the increased temperature

is short compared to the ionization equilibration timescale, this increased Boltzmann fac- tor affects the emission before the He"*" is ionized to He"^"*", as it would be in ionization

equilibrium at this raised temperature.

The ratio R in the spectrum of Fe XV is observed to be about 12 in photon units,

but jjredicted to be a factor of two or so greater. This discrepancy is reduced in a burst

model, when inner shell ionization of the aluminium-like Fe XIV is taken into account.

This ionization from the 3s^3p configuration of Fe XIV to the 3s3p configuration of Fe XV

will enhance the population of triplets relative to singlets, hence bringing the ratio closer

to that observed. The effect is even bigger if one also postulates a non-Maxwellian electron

distribution immediately following the burst, with an excess of electrons at or just above

the Fe"*"^^ ionization threshold. In fact, such a deviation of the electron distribution from

a Maxwellian is required for absolute agreement between observations and theory.

Feldman (1992) has reviewed the effects of bursts on electron density diagnostics.

In the work presented here, following in part the ideas of Parker (1988), that the solar

corona, and presumably other solar regions as well may be thought of as being continuously

heated by a population of bursts, we investigate the electron density diagnostics relevant to what has been called the Unresolved Fine Structures by Feldman (1983, 1987), otherwise

known as the solar transition region. The densities inferred from line ratios formed at temperatures between 5 x 10"* K and 2 x lO^"* K are evaluated to test the notion that

this region obeys a constant pressure law, which would be most characteristic of a steady

state plasma in ionization equilibrium. We also review the non-thermal mass motions

associated with transition region lines formed over the same range of temperatures in

ionization equilibrium.

91
92

In our analysis, it appears quite clear that the region of the Unresolved Fine Structures

in the quiet sun and in the two active regions studied follows a constant density law much

more closely than a constant pressure law, contrary to what has generally been assumed

previously. Data from the 1973 June 15 flare are less conclusive, but there too, one can

argue that at certain times during the decay phase of the flare, a constant density law is appropriate. We believe that this variation of density with temperature is another piece of

evidence for the existence of bursts in the solar atmosphere. Moreover, it appears possible

that these bursts compress material as they heat it rather than expand it as in something

of an explosive nature. The morphology of this solar region, as observed by stigmatic slit spectra taken by the HRTS instrument, does not contradict such a conclusion. Features

apparent in the image of lines formed at 5 x 10^ K like Si III are also seen in images of

lines formed at much higher temperatures, e.g. O V at 2.5 x 10^ K.

Further, indirect, evidence for the existence of bursts comes from our analysis of the

non-thermal mass motions present in the transition region. When the lines are assumed

to be emitted from plasmas with temperatures about twice those where the lines would be

formed in ionization equilibrium, the non-thermal mass motions are approximately independent of temperature. This is in contrast to the case of lines emitted at their ionization

equilibrium temperatures, where the non-thermal velocities increase with temperature.

This behaviour is harder to understand, if, according to the HRTS data, the morphology

of transition region lines formed at difl"erent temperatures are very similar.

References

Feldman, U. 1983, ApJ, 275, 367

Feldman, U. 1987, ApJ, 320, 426

Feldman, U. 1992, ApJ, 385, 758

Feldman, U., Laming, J. M., Mandelbaum, P., Goldstein, W. H., & Osterheld, A 1992,

ApJ, in press

Laming, J. M., and Feldman, U. 1992, ApJ, 386, 364

Parker, E. N. 1988, ApJ, 330, 474
Photoionization Resonances of Si II

in the Spectrum of Ap Si Stars

T. Lanz\ M.-C. Artru^, M. Le DourneuP, and I. Hubeny^

1 NASA Goddard Space FUght Center, Code 681, Greenbelt, MD 20771, USA

- Ecole Normale Superieure de Lyon, 46 allee d'ltalie, F-69364 Lyon, France

^ UPR 261 du CNRS et DAMAp, Observatoire de Meudon, F-92195 Meudon, France

* Universities Space Research Association, NASA/GSFC, Code 681, Greenbelt MD 20771, USA

ABSTRACT: We present a study of the photoionization of Si"^ in stellar atmospheres. New theoretical

calculations provide detailed photoionization cross-sections, including autoionization resonances, for many

energy levels of Si II. They are included in synthetic spectra calculations of the far UV spectrum of A and late B stars, and they increase dramatically the opacity when silicon is overabundant. The most characteristic features of the far UV spectrum of Ap Si stars can now be reproduced, as illustrated by a comparison with

lUE data for HD 34452.

1. INTRODUCTION

The photoionization of Si"^ is expected to have a significant influence on the radiation transfer in the photosphere of A and late B stars (Toff = 10000 to 15000 K), especially for the Ap Si stars which exhibit silicon overabundances (5 to 50 times solar). Silicon may become the third most abundant species beyond hydrogen

and helium; moreover, the flux of the A and late B stars is maximum in the far UV, where the Si"*" cross- sections may be large. Besides the enhanced Si II lines, the UV spectra of Ap Si stars show characteristic depressions, with widths larger than 5 nm. It is likely that they may be due to autoionization resonances

of Si II, as first suggested by Jamar etal (1978). The strongest one at 140 nm has been identified to an

autoionization line from an excited level of Si II (Artru, 1986). Synthetic spectra including this transition

with its theoretical natural line width reproduce well the observed flux depression (Artru Sz Lauz 1987).

Other characteristic features in the ultraviolet (157 and 178 nm) and in the visible spectrum of silicon stars remained unexplained.

2. THE PHOTOIONIZATION OF Si+

Very accurate calculations on the photoionization of the Si II ground state have been performed in 1984 by

Taylor etal, using the standard i?— matrix code (Burke and Taylor 1975, Berrington etal 1978), to calculate consistent close couphng expansions of the initial bound state and the filial continuum states of Si"*" in terms of the 12 lowest states of Si'"*". These 12 states are represented by very accurate Configuration Interaction (CI) wave functions expressed in terms of 8 spectroscopic orbitals Is, 2s, 2p, 3s, 3p, 3d, 4s, 4p and 2 correlation

orbitals 4ci et 4/ optimised by Baluja and Hibbert (1974) and allowing all possible distributions of the 2 outer electrons in the n = 3, 4 shells. In the present extension of the photoionization calculation to aU the excited states relevant to the analysis of the spectra of silicon stars, we have used the OPACITY i?— matrix

code (Berrington etal 1987), similarly to the other calculations of the OPACITY project. However, the

present results are expected to be slightly more accurate than their OPACITY analogues, since they use more sophisticated L- expansions of the Si'"*" and Si"*" states. Typically, the 50 lower bound states of Si"*" have

been obtained in the experimental order, with relative energies accurate to within a few percents, and the agreement between the length and velocity forms of the oscillator strengths for the bound states of Si"*" and

of corresponding photoionization cross-sections agree within a few percents, except for very small transitions

subject to cancellation efl^ects. Several cross-sections have very strong broad resonances. In particular, a strong resonance from the level 3d -D occurs at 140 nm, which confirms the identification suggested by Artru (1986) and Artru & Lanz

(1987). This cross-section is displayed in Fig. 1 and shows other wide resonances. A strong threshold is found at 129.6 nm from 3p^ "D (see Fig. 1). This cross-section corresponds to the ionization toward the

ground state of Si"''', which is only possible due to configuration mixing between 3d and 3p-. This Limit has been observed by Artru & Lanz (1987) in the spectrum of Ap Si stars; moreover, they identified several

93
94

lilies of the corresponding series. A strong resonance, due to the transition 3p- "P - 4s" -P°, is calculated

around 155 uin; an observed depression in Ap Si spectra can be attributed mainly to this resonance. So far, we have been unable to identify the depressions at 178 niii and in the visible spectrum; we may nevertheless note that if these depressions should be attributed to Si II, then the initial level would be highly excited and

little populated.

Fig. 1. Cross-sections for two low-excitation levels of Si II, and theoretical spectra for typical model atmospheres of A and late B stars, with a full range of sihcon abundances.
T. Lanz et al. 95

3. ASTROPHYSICAL APPLICATION TO Ap Si STARS

We have computed some theoretical spectra for two model atmospheres typical of A and late B stars. We

have included these new detailed cross-sections, assuming different silicon abundances. Fig. 1 displays such

theoretical spectra, where a single cross-section is included at once to show its own effect. With a solar Si abundance, we found only rather small changes in the spectrum, but they could become dramatic for Ap Si stars with Si abundances larger than 10 times the solar abundance. We found observable effects only in the UV spectrum and for the cross-sections from levels with low excitation.

Fig. 2 displays a comparison with the observed lUE spectrum of HD 34452, an AOp Si star. We as- sumed the same stellar parameters than Artru & Lanz (1987): Tgfr = 13650K, log g = 4, c(Si) = 25x0,

£(ironpeak) = 10x0. We have included the cross-sections of the six lowest Si II levels (up to 10.4 eV,

without the ground state having a photoionization limit at 76 nm) and about 43000 metallic lines in the

computation of the LTE theoretical spectrum.' The agreement with the observed spectrum is striking! The

depression at 140 nm and the region below 130 nm are very well reproduced, although the predicted flux below 118 nm is still too high. Attributing to Si II the depression between 155 and 160 um is well supported.

Severed other calculated resonances are indeed observed in the stellar spectrum.

1200 1300 1400 1500 1600 1700

X [A]

Fig. 2. Comparison of the observed lUE spectrum of HD 34452 and a theoretical spectrum calculated with

the Si II photoionization cross-sections and about 43000 Unes. The dashed lines show the dramatic effect of

the Si II absorption.

REFERENCES

Artru M.-C, 1986, A&A 168, L5. Artru M.-C, Lanz T., 1987, A&A 182, 273. Berrington K.A., Burke P.O., Le Dourneuf M., Robb W.D., Taylor K. T., Vo Ky L., 1978, Comput. Piiys.

Commun. 14, 367. Berrington K.A., Burke P.O., Butler K., Seaton M.J., Storey P.J., Taylor K.T., Yu Y., 1987, J. Phys. B 20,

6379.

Burke P.O., Taylor K.T., 1975, J. Phys. B 8, 2620.

Jamar C, Macau-Hercot D., Praderie F., 1978, A&A 63, 155. Seaton M.J., 1987, J. Phys. B 20, 6363.

Taylor K.T., Zeippen C.J., Le Dourneuf M., 1984, J. Phys. B 17, L157.
PHOTOSPHERIC HEAVY ELEMENTS IN HOT, HYDROGEN-RICH

WHITE DWARFS (DA WD)

Stephane Vennes and Stuart Bowyer

Center for EUV Astrophysics, University of California at Berkeley

2150 Kittredge St., Berkeley, CA 94720

1 . Properties of Hot DA White Dwarf Stars

Hot, hydrogen-rich white dwarfs (spectral type DA) present extreme

photospheric chemical composition. Their atmospheres, fully radiative, are largely

dominated by hydrogen with, in some very hot stars, small heavy element traces (Z <

10"^). As defined by the assigned spectral type, they show no traces of helium in optical

and ultraviolet spectra (Y < 10"^) in contrast with neighboring spectral types, DO (Y > 10^) and DAO (Y = 10'2). This pattern is usually explained in the context of chemical

separation in a strong gravitational field, g = 10^ cm s'2, also known as gravitational

settling. The presence of heavy elements (C, N, Si, Fe) in very hot DA white dwarfs (Teff > 50,000 K) is naturally explained by radiative levitation in a strong radiation field (Chayer, Fontaine, & Wesemael 1989, 1991). The case of Feige 24 (WD 0232-(-035) is rather exemplary. Early high-dispersion spectroscopy with the International Ultraviolet

Explorer revealed the presence of C IV, N V and Si IV absorption features attributed to the photosphere of the star (Dupree & Raymond 1982). The inferred abundances are in the range 5x1 0"''

- 5x10"^ (Wesemael, Henry, & Shipman 1984). Surprisingly the

second most abundant element in Feige 24 was later found to be Fe (in the form of Fe V)

with an abundance by number, Fe/H = 10"^ (Vennes et al. 1992). These rather low trace element abundances as a whole help interpret one remarkable property of hot white

dwarf stars: all DA white dwarfs hotter than Teff ~ 25,000 K are sources of extreme

ultraviolet radiation extending in some cases in the soft X-ray range. These EUV

observations initiated with Apollo-Soyuz (Feige 24; Margon et al. 1976), were later refined and extended to a large group (-25 stars) of DA white dwarfs with EXOSAT

(Paerels & Heise 1989; Vennes & Fontaine 1992). More recently the EUV all-sky

survey performed in two EUV bandpasses (labelled SI and S2) by the UK Wide Field

Camera (Pounds et al. 1992) has extended EUV detections of DA white dwarf stars to about 100 objects. With this new data set we confirm one basic conclusion achieved with

EXOSAT, i.e. the apparent EUV/soft X-ray flux deficiency relative to the predictions of

pure hydrogen atmospheres found in most DA stars hotter than about 40,000 K (Fig. 1). This property can be understood if one postulates a direct filiation of the hot DA white

dwarfs with the DO/DAO spectral types (DO —> DAO —> DA). In this context He and H are separated in two distinct layers with hydrogen floating on top the helium envelope. The

thickness (i.e. transparency) of the hydrogen layers then determines the optical/UV

properties (He II >.4686, He I X447^, H I Balmer series) of the DO/DAO stars as well as

the EUV/soft X-ray flux from DA stars which then departs strongly from pure H

atmospheres (Vennes et al. 1988; Vennes & Fontaine 1992). The applicability of this

model to EUV/soft X-ray properties of DA stars is debatable, however, because, as we

have seen above, heavy elements are possibly dominating the EUV/soft X-ray spectra of

these objects. This is clearly the case of Feige 24, for which EXOSAT low-dispersion

spectroscopy is available (Paerels et al. 1986). Paerels et al.'s spectrum clearly shows

the signature of heavy element photoionization opacities (Vennes et al. 1989) probably

from ionized species of Fe. A more definitive answer may come from forthcoming

medium-dispersion EUV spectroscopy by the Extreme Ultraviolet Explorer.

96
Stephane Vennes and Stuart Bowyer 97

S2/S1

Figure 1. Interpretation of the VJfC observations (S2 normalized to an apparent

magnitude V = 15.0 vs S2/S1) of DA white dwarfs with pure hydrogen model

atmospheres (log g = 8, Teff = 25, 30, 35, 40, 45, 50, 55, 60, 65x1 0^ K) also

normalized to V = 15 and attenuated by ISM neutral hydrogen column density, nn = 0.1,

1.0, 10.0, 30.0, 60.0, 100.0 x lO^^ cm-2. The likely presence of heavy elements (C,

N, Si, Fe) shifts the apparent location of most hot (Teff > 40,000 K) DA stars to a very

soft location in the diagram (shown for representative cases with broken lines pointing

toward the lower right corner) unaccountable for with pure hydrogen models.

2. Far Ultraviolet Synthetic Spectra for Hot DA White Dwarfs

Most of the information about the chemical composition of hot DA stars is currently obtained in the far ultraviolet range using lUE as well as the Hubble Space

Telescope (Sion et al. 1992). In Fig. 2 we present synthetic spectra of the FUV range for different chemical compositions: hydrogen rich atmosphere (Tgff = 55,000 K, log g = 7)

with traces of Ni and Fe compared with the lUE spectrum of Feige 24. We confirm the

predominant role played by Fe in this star as Ni remains undetected. Similarly we found no traces of Ca in Feige 24.
1372 1376 1380 1384 1388

X (A)

Figure 2. Far ultraviolet synthetic spectra of Fe (IV, V, VI) and Ni (IV, V) for a model

atmosphere at Teff = 55,000 K, log g = 7 (oscillator strengths from Kurucz, R.L 1991,

private communication) compared with lUE high-dispersion spectroscopy of Feige 24.

3. Conclusion

1. Extreme ultraviolet spectroscopy in the range 70-800 A is necessary to fully

investigate the chemical composition of DA white dwarfs. The apparent flux deficiency

alluded to in EXOSAT an6 WFC photometric observations can be accounted for by either

stratified H/He models and/or photospheric heavy elements. The Extreme Ultraviolet

Explorer will fulfill this need.

2. Heavy elements, mainly Fe, are contaminating the UV, and most likely, the

EUV/soft X-ray photospheres of hot DA white dwarfs. Modeling of these spectral ranges

expose the need for accurate oscillator strengths and photoionization cross-sections of

species like Fe V. This requirement can be extended to several light elements (C, N, Si) as well as other elements of the iron group.

Chayer, P., Fontaine, G., & Wesemael, F. 1989, White Dwarfs, (Berlin: Springer), 253

. 1991, White Dwarfs, (Dordrecht: Kluwer), 249

Dupree, A.K., & Raymond, J.C. 1982, ApJ, 263, L63

Margon, B., Lampton, M., Bowyer, S., Stern, R., & Paresce, J. 1976, ApJ, 210, L79

Paerels, F.B.S., Bleeker, J.A.M., Brinkman, A.C., & Heise, J. 1986, ApJ, 309, L33

Paerels, F.B.S., & Heise, J. 1989, ApJ, 339, 1000

Pounds, K., et al. 1992, MNRAS, in press

Sion, E.M., Bohlin, R.C., Tweedy, R.W., & Vauclair, G.P. 1992, ApJ, 391, L30

Vennes, S., Chayer, P., Fontaine, G., & Wesemael, F. 1989, ApJ, 336, L25

Vennes,S., Chayer,P., Thorstensen, J.R., Bowyer, S., & Shipman, H.L. 1992, ApJ, 392, L27

Vennes, S., Pelletier, C, Fontaine, G., & Wesemael, F. 1988, ApJ, 331, 876

Vennes, S., Fontaine, G. 1992, ApJ (Dec. 10 issue)

Wesemael, F., Henry, R.B.C., & Shipman, H.L. 1984, ApJ, 287, 868
ATOMIC DATA NEEDS FOR OPTICAL REGION STUDIES

OF EARLY A TYPE STARS

Saul J. Adelman*

Department of Physics, The Citadel, Charleston, SC 29409 USA

and

Austin F. Gulliver*

Department of Physics and Astronomy, Brandon University, Brandon, Manitoba R7A 6A9 Canada

* Guest Investigator, Dominion Astrophysical Observatory

If there are any t3TDes of stars for which we should be able to derive reliable elemental

abiindances, it is the early A stars. The atmospheric modeling is now straightforward as the

atmospheres are in radiative equilibrium with hydrogen as the dominant opacity source. The line

opacities for the light through the iron peak elements are reasonably well calculated. Hotter stars exhibit strong non-LTE effects. Cooler stars have substantial convection zones as well as molecules in their atmospheres, situations which involve more complicated physics.

With model atmospheres which have the proper opacities and physics included such as those

calculated by the ATLAS9 program of Dr. Robert L. Kurucz, it should be possible to deduce high

quality abundances of many elements. As A type star lifetimes are much less than the age of the

Sun, the A type stars we see must have formed relatively recently on a cosmological time scale. Comparison of their abundances with solar values should yield important information about the

chemical history of matter in our Galaxy during the last five billion years.

In the last decade with electronic detectors such as Reticons and CCDs replacing photographic plates for spectroscopy, the signal-to-noise ratio of typical high dispersion astronomical observations has tended to increase from 20 to 100 or more. This suggested that a detailed comparison of a high dispersion spectra with minimal noise of a prototype A star with the best spectral synthesis

would be useful. As A type stars with effective temperatures of order 10000 K represent sources which are hotter than typical atomic laboratory sources, considerable atomic physics information can also be extracted from this data (see Leckrone et al. 1992).

The atomic line lists which one can realistically use for spectrum synthesis calculations are primarily the work of Dr. Robert L. Kurucz, whose generous policy of making them able to other

workers has lead to much of the progress that has been made in this area. Also of importance are

the critical compilations made at NIST by Fuhr, Wiese, and associates. When one performs a

calculation, one finds that most spectral features are blends, even those which are often attributed

to one primary line in line identification studies. Blending can be avoided to some extent by

working with the sharpest lined stars, but these are only a small fraction of the known stars. For

these calculations one can only use lines with good wavelengths and calculated or measured

oscillator strengths which in practice means one works with classified lines. Potentially there

are many still to be classified lines which also could make contributions to spectrum synthesis

calculations. Excluding them means that the derived abundances may be overestimates.

Optical region line identification studies with high signal-to-noise data often reveal lines

which are not in A Multiplet Table of Astrophysical Interest (Moore 1945). By using more recently

published atomic spectra studies, one can identify a number of these features. Other methods of

attack are to predict the wavelengths of lines to complete multiplets or even to predict wavelengths

of lines between known energy levels (Dworetsky 1971, Adelman 1987).

99
100

Beyond the identification of a line, one can use its profile (or equivalent width) to deduce an

elemental abundance. For an unblended line one needs to know its atomic parameters, in

particular, its lower excitation potential, its oscillator strength and (for non-weak lines) its line

damping constants as well as the ionization potentials and partition functions for the atom.

For these reasons we decided to compare as well as we could the spectrum of some relatively

sharp-lined A type star with the predictions of a state of the art spectrum synthesis code, SYNTHE

of Dr. Robert L. Kurucz. This we expected would allow us to assess the quality of the comparison,

including lines in the star missing in the code and systematics in the oscillator strengths. For the

spectrum synthesis input parameters we use stellar parameters derived from fine analyses of the same data. In some cases hyperfine structure and isotopic shifts can also be important and

detectable if not included in the spectrum synthesis calculations.

We obtained Reticon spectra of Vega, one of the brightest stars in the sky, with, the coude

spectrograph of the Dominion Astrophysical Observatory at a reciprocal dispersion of 2.4 A mm-^

to produce a high quality spectral atlas. After considerable experimentation we have achieved

signal-to-noise ratios of 3500 or more. Figure 1 illustrates the type of improvement in spectral

quality which has been achieved. Besides showing at certain wavelengths the telluric spectrum

which is weak or absent in most of the photographic region, the high signal-to-noise data have

revealed some important clues about the nature of Vega. Most importantly the line profiles of Vega

are not those expected from classical model atmospheres theory. There are a large number of weak

flat bottom lines. This may be evidence that this star is a fast rotator seen pole on according to one

interpretation of the non-classical line profiles. This interesting astrophysical observation

means that we are now working to model these profiles before we can examine the atomic physics

aspects of this data.

Thus, we selected another early A star which did not show peculiar line profiles for a second

atlas. The star Omicron Pegasi is one of the sharpest-lined stars, v sin i about 6 km s"^ It is about

100 times fainter than Vega and thus we can achieve signal-to-noise ratios of about 500 to 750 at

best. Its effective temperature is 9600 K and its surface gravity log g = 3.60. We now have

observations covering W4050-4880 and plan to extend these observations both longward and

shortward as long as we can achieve a signal-to-noise ratio of 500 in two hours. The must recent

abundance analysis is by Adelman (1988ab) based on coadding 12 IlaO nitrogen baked 2.4 A mm'

^ photographic region spectra obtained with the long camera of the DAO coude spectrograph. The

maximum signal-to-noise ratio of this data was about 80.

Figure 2 shows a comparison between the observations of o Peg (solid line) and a synthesized spectrum (dashed line) for XX4380 - 4390. Many of the defects of the comparison can be fixed

by changes in the oscillator strengths and/or assumed elemental abundances by factors of two or

less. We would expect slightly better agreement if our synthesized spectrum was calculated based

on parameters derived from a fine analysis of the Reticon S/N>500 data instead of the coadded

photographic data. The instrumental profile might need to be slightly broader in the wings.

However, we also see evidence for oscillator strengths being absent from the code and for errors in

the laboratory wavelengths. Study of the later may be useful in improving the values of atomic

energy levels. We would like to work with atomic physicists to improve the atomic data needed to synthesize such spectra.

REFERENCES

Adelman, S. J. 1987, PASP 99, 515 ' Adelman, S. J. 1988a, MNRAS 230, 671

Adelman, S. J. 1988b, MNRAS 235, 749

Dworetsky, M. M. 1971, PhD thesis, University of California at Los Angeles

Leckrone, D. S. et al. 1992, ApJ, in press

Moore, C. E., 1945. A Multiplet Tbble of Astrophysical Interest, Princeton University Observatory
Saul J. Adelman and Austin F. Gulliver 101

I—

1.00

0.95

0.90 -

0.85

0.80

T 1 T "1 1 1 r T r

-| 1 r

Photogrophic 1980

4520 4525

WAVELENGTH

4530

Figure 1. The spectrum of Vega as obtained with the long camera of the coude spectrograph of the

1.4-m telescope of the Dominion Astrophysical Observatory. The three spectra illustrate how the

improvement in the signal-to-noise ratio has resulted in revealing important details.

CMICPOr^ PZ3R3I

4380 438 = 4334 43oo

WaVELENGTH ',fiN3STR0M3)

43S8 4390

Figure 2. The spectrum of Omircon Pegasi XX4380-4390 as observed with the long camera of the

coude spectrograph of the 1.4-m telescope of the Dominion Astrophysical Observatory (solid line)

compared with a synthetic spectrum based on stellar parameters from an analysis by Adelman

(1988b) (dashed line). On the whole the agreement is quite good. However, we can see that if one

shifts stellar spectrum so that it agrees with the wavelength of the Fe I (41) X4383.547, the

wavelength of Fe II (27) X4385.381 is not in good agreement. The blend dominated by Fe II (32)

X4384.33, which is a predicted line, also shows a wavelength shift.
EXPERIMENTAL ISOTOPE SHIFTS IN NI II AND EE II

Maria Rosberg, Ulf Litz6n and Sveneric Johansson

Lund University, Department of Physics, Solvegatan 14, S-223 62 Lund

This work reports about measurements of isotope structure in Ni II and

Fe II. We have used spectra from hollow-cathode lamps that have been

recorded with the Fourier Transform Spectrometer at Kitt Peak National

Observatory. Measurements of isotope shifts yield useful information

about atomic and nuclear properties. With high-resolution spectroscopy

at modern telescopes it is also possible to observe isotope shifts in

stellar spectra (Leckrone et al 1991). The importance of a general

knowledge about isotope structure for studies of the solar spectrum has

recently been pointed out (Kurucz 1992). This is especially true for

elements having line-rich spectra and a high solar abundance. Ignoring

isotope structure when constructing synthetic spectra may introduce

systematic errors in the calculation of line profiles and may therefore

affect e.g. abundance determinations.

The nickel spectrum used covers the wavelength region 5800-7100 A and

it was emitted by a hollow-cathode lamp run at a current of 0.5 Amps

with argon as a carrier gas at a pressure of 2.5 Torr. The iron spectrum we used covers the region 8600-14200 A and in this case the light

source was run at 1.0 Amps DC with neon as a carrier gas at a pressure

of 4 Torr.

Some of the lines in the spectra show a nearly resolved isotope

structure. These lines correspond to the transitions in Ni II

3d^(¥)4p-3d^4s^ (Shenstone 1970) and 3d^(^D)4p-3d^4s^ in Fe II

(Johansson 1978). For both nickel and iron the measured isotope shifts

102
Maria Rosberg et al. 103

are negative, i.e. the heavier isotope is shifted towards smaller

wavenumbers.

Thirteen Ni II lines in the red region have been studied in detail,

see Figure 1. Natural nickel has the following isotope composition: 68%

^Ni, 26% ^Ni, 1% ^^Ni, 4% ^^Ni and 1% ^i. However, in the spectrum

we can only see four peaks for each line, as the ^^Ni isotope exhibits

hyperfine structure and its intensity is therefore spread out on a number of undetectable components. The measured splittings ^Ni-^^Ni,

^^Ni-^Ni, %i-^Ni are of the order of -100 mK with the largest

spread in the first one. The intensity distribution among the

8 3 7 2 components of the strongest 3d ( F)4p-3d 4s lines show a good

agreement with relative abundances of natural nickel.

14520 14521 14522 Wavenumber (cm"')

14523

Figure 1 Isotope structure in Ni II A6884.
104

Natural iron consists of 6% ^ Fe, 92% ^''Fe, 2% ^Te and 0.3% ^^Fe.

However, we can only see the two most abundant isotopes, ^"^Fe and ^^Fe,

which is illustrated by the strong Fe II line at 9997 A in Figure 2.

This line is very strong in emission in spectra of various stars and

extragalactic objects, probably due to fluorescence induced by H Lya

(Johansson 1990). We have studied the isotope structure of nine Fe II

lines in the near-infrared region, giving an average value of the

isotope shift of about -105±3 mK.

9999 10000 Wavenumber (cm"') Figure 2 Isotope structure in Fe II X9997,

References

Johansson S., 1990, ed. G. Wallerstein, in Cool stars, stellar systems

and the sun, ASP Conf. Ser. 9, 307.

Johansson S., 1978, Physica Scripta 18, 217.

Leckrone D. S., Wahlgren G. M., Johansson S., 1991, Ap. J. 371, L37.

Kurucz R. L., 1992, submitted to Ap. J.

Shenstone A. G., 1970, /. Res. Nat. Bur. Std. 74A, 801.
Accurate Wavelengths and Isotope Shifts for Lines of

Doubly-Ionized Mercury (Hg III) of Astrophysical Interest

Craig J. Sansonetti and Joseph Reader

National Institute of Standards and Technology

Gaithersburg, MD 20899

For thirty years it has been known from observations of the 3984 A line of Hg 11 that Hg is much more abundant in the atmospheres of some chemically peculiar stars than in the sun. The

wavelength of this line is seen to vary slightly from star to star, and Bidelmanl suggested that these

variations resulted from differing isotopic compositions. The most extreme isotope anomaly

occurs in the star chi Lupi^ where the observed wavelength is consistent with nearly pure ^^Hg.

Michaud et al.^ have proposed a diffusion model to explain both the enhanced abundance of

Hg and the isotope anomalies observed in Hg-rich stars. In this model the balance between

radiation pressure and gravity causes heavy isotopes to concentrate in a thin layer of the stellar

atmosphere as neutral and singly-ionized Hg, while the lighter isotopes exist at higher altitudes as doubly-ionized Hg or are driven away from the star by the radiation pressure. To test this model it is necessary to determine elemental and isotopic abundances for Hg by using lines of different

stages of ionization.

Using the Goddard High Resolution Spectrograph (GHRS) on the Hubble Space Telescope,

Leckrone and co-workers have made observations of the Hg III lines at 1738.4, 1738.5, 1740.2,

and 2354.2 A in chi Lupi. To derive abundances from ihese data, accurate wavelengths and

isotope shifts are needed. The accuracy of the best available wavelength data by Johns^ and

Foster^ is not adequate for the analysis. Although Foster^ in a subsequent paper reported isotope

shifts for 21 Hg III levels, no data were given that apply to the lines observed with GHRS.

The present work was undertaken to provide accurate wavelengths and isotope shifts for these

lines of Hg III to permit reliable interpretation of the spectrum of chi Lupi. A full description will

be pubHshed elsewhere.^

EXPERIMENT

The spectrum of doubly-ionized Hg was excited in sealed electrodeless-discharge lamps by

using a pulsed radio-frequency oscillator. Four lamps of identical dimensions were used: two

containing ^^^Hg and one each containing natural Hg and ^^Hg. Each lamp was filled under high

vacuum with a few mg of Hg and no earner gas. The lamp design is shown in Fig. 1. Rf power at a frequency of 13.5 MHz was coupled into the Hg discharge by a capacitively

tuned resonant circuit. Excitation of the Hg III spectrum was optimized by adjusting the duration

of the rf pulses, their repetition rate, and the peak pulse power. The metallic Hg was kept

concentrated at the rear of the lamp by a gentle stream of air. The entire body of the lamp was

cooled by diffuse air from a small fan. Under these conditions the lamp operated stably and

emitted a strong Hg III spectium with sharp unperturbed lines.

The spectrum was photographed

with the 10.7-m normal-incidence .vacuum Extension pFCoiU Air stream vacuum spectrograph at the National / . \, .A

Institute of Standards and Technology. ^ , Spectra of Pt I and 11^ and of Ar 11^ ^

were used as wavelength standards.

The observations were used to determine wavelengths of the four lines

of l98Hg III, given in Table I. Small

shifts between the Hg spectmm and the

• Plane Quartz Window

Hg Metal

Fig. 1. Schematic of Hg pulsed rf lamp.

105
106

Aril {

Pt and Ar reference spectra due to slightly different grating illumination were removed by using

accurate values for several ^^^pjg jj li^es given by Reader and Sansonetti.lO The final uncertainty

in our Hg wavelengths is attributable approximately equally to the uncertainty in the general

calibration based on the reference spectra and to the uncertainty in determining the shift between the

Hg and reference spectra. ^

Special exposures were made to measure the isotope shifts between lines of the 204 and 198

isotopes. For these exposures spectra from the ^^^Hg, ^^Hg, and Ar lamps were photographed

sequentially. By means of adjustable masks in front of the plate holder, the spectra were arranged

as shown in Fig. 2. The position of the plate in the

spectrograph was not disturbed between exposures.

The isotope shifts were determined by measuring

two parallel tracks on the photographic plate as shown in

Fig. 2. These tracks were defined by masks in the

optical system of the comparator so that the position of a

line could be measured in either track without moving

the comparator cross feed. The Ar lines served as a

reference to define zero isotope shift. For each Hg line, the displacement between the two isotopes was found as the difference of the

positions measured in the upper and lower tracks. The result was corrected by subtracting the

average displacement between the upper and lower track positions of the Ar lines. The corrected

displacement was multiplied by the plate factor to obtain the isotope shift. The measured

204-l98Hg isotope shifts are given in Table I. Shifts between natural Hg and i^-^^Hg were deteiTnined by the same technique described above.

The results are given in Table I. As the profile of the 2354-A line of natural Hg was broadened

and slightly asymmetric, the uncertainty of its shift was increased to ±0.003 A.

198

204 Hg

Hg

Fig. 2. Exposures for isotope shift

measurements.

SHIFTS FOR OTHER Hg ISOTOPES

For heavy elements, where mass-dependent effects are negligible, the relative shifts between

isotopic components of a spectral line depend only on the size and shape of the nucleus and are independent of the combining energy levels and the stage of ionization. By using relative isotope

shifts derived from lines of Hg ^'^2 and our measurements of the 204-l98Hg shifts, we are able to calculate shifts for the remaining stable isotopes. We have also calculated the shift for natural Hg

from the relative shifts by using the known abundances!^ for the stable isotopes. In Table II we summarize the wavelengths for all stable isotopes obtained from our measured

204-l98Hg shifts and the relative isotope shifts. The wavelengths for natural Hg in this table are those calculated from the relative isotope shifts and isotopic abundances, which we consider to be

more reliable than the directly measured values for natural Hg.

Table I. l98Hg III wavelengths and isotope shifts. Wavelengths shorter than 2000 A are vacuum.

Wavelength Wave Number 204Hg - 198Hg Shifta Natural Hg - 198Hg Shiftb

(A) (cm-1) (A) (cm-1) (A) (cm-1)

1738.4560(20)

1738.5207(20)

1740.2556(20)

2354.2160(20)

57 522.31(7)

57 520.17(7)

57 462.82(7)

42 463.99(4)

0.0218(20)

0.0190(20)

0.0221(20)

0.0398(20)

-0.72(7)

-0.63(7)

-0.73(7)

-0.72(4)

0.0091(20)

0.0078(20)

0.0093(20)

0.0201(30)

-0.30(7)

-0.26(7)

-0.31(7)

-0.36(5)

The wavelength for 204Hg is longer than for 198Hg.

The wavelength for natural Hg is longer than for l98Hg.
Craig J. Sansonetti and Joseph Reader 107

Table 11. Wavelengths (A) for natural Hg and stable Hg isotopes. Results for odd isotopes are the

center-of-gravity of the magnetic hypeiTine structure. Hg III Line

Species

1738 1738 1740 2354

196Hg ^ .4501(21) .5156(21) .2496(21) .2052(21)

198Hg .4560(20) .5207(20) .2556(20) .2160(20)

199Hg .4569(20) .5215(20) .2565(20) .2177(20)

200Hg .4628(21) .5267(21) .2625(21) .2285(21)

natural Hg .4647(22) .5283(22) .2644(22) .2319(22)

20lHg .4651(22) .5286(22) .2648(22) .2326(22)

202Hg .4704(24) .5332(24) .2702(24) .2422(24)

204Hg .4778(28) .5397(28) .2777(28) .2558(28)

ASTROPHYSICAL IMPLICATIONS

Based on our present measurements, Leckrone et al. have analyzed the two lines of Hg III at 1738 A in the GHRS spectra of chi Lupi. Their analysis shows the same isotope anomaly that was

found previously with the lines of Hg II; that is, the spectrum is consistent with pure ^^Hg. They

conclude that this result, which disagrees with some predictions of the diffusion model,^ reveals a need for a new or refined model to explain the elemental and isotope abundance anomalies for Hg

in chemically peculiar stars. ACKNOWLEDGEMENT

This work was supported in part by tlie National Aeronautics and Space Administration.

REFERENCES

1. Sky and Tel., 23, 140 (1962).

2. R. E. White, A. H. Vaughan, Jr., G. W. Preston, and J. P. Swings, Astrophys. J. 204,

131 (1976).

3. G. Michaud, H. Reeves, and Y. Charland, Astron. & Astrophys. 37, 313 (1974).

4. M. W. Johns, Can. J. Res. A 15, 193 (1937).

5. E. W. Foster, Proc. Roy. Soc. London A 200, 429 (1950).

6. E. W. Foster, Proc. Roy. Soc. London A 208, 367 (1951).

7. C. J. Sansonetti and J. Reader, submitted to Phys. Rev. A (1992).

8. J. E. Sansonetti, J. Reader, C. J. Sansonetti, and N. Acquista, J. Res. Natl. Inst. Stand.

Technol. 97, 1 (1992).

9. G. Norlen, Phys. Scr. 8, 249 (1973).

10. J. Reader and C. J. Sansonetti, Phys. Rev. A 33, 1440 (1986).

U.S. Gerstenkorn and J. Verges, J. Physique 36, 481 (1975).

12. S. Gerstenkorn, J. J. Labarthe, and J. Verges, Phys. Scr. 15, 167 (1977).

13. D. R. Lide, ed.. Handbook of Chemistry and Physics, 73rd Edition (CRC Press, Inc.,

Boca Raton, Florida, 1992).

14. D. S. Leckrone, G. M. Wahlgren, S. G. Johansson, and S. J. Adelman, "High Resolution

Ultraviolet Spectroscopy of Chemically PecuHar Stars with the HST/GHRS," in Proceedings

of I.A.U. Colloquium no. 138, M. M. Dworetsky, ed. (P.A.S.P. Conference Series, in press

1992).
LINE BLANKETING IN NOVA ATMOSPHERES

P. H. Hauschildt and S. Starrfield

Dept. of Physics and Astronomy

Arizona State University

Tempe, AZ 85287-1504

Introduction

We are currently using a spherical, expanding, non-LTE stellar atmosphere code to

analyze the early spectra of novae in outburst. We have found that nova atmospheres are dominated by an enormous number of overlapping spectral lines. These lines originate from

a large number of species in very different ionization stages due to the large temperature

gradients found in nova photospheres. The features which appear to be 'emission lines' are actually ''holes in the iron curtain". The conditions inside the line forming regions of

these photospheres imply very large deviations from LTE and, therefore, the line formation

process is a complicated multi-level non-LTE problem in a rapidly expanding shell. Spectral

synthesis and analysis of these spectra demonstrate the importance of line blanketing in

the early and late spectra of novae and require the best and most complete atomic data in

order to obtain accurate abundances for the elements in nova ejecta.

In the following sections we describe briefly the model assumptions, parameters, and

the model construction. We then show an example for the influence of line blanketing on

nova spectra.

Model Assumptions

• steady state, i.e., d/dt = 0, • power law density, i.e., p{r) oc r""^, • constant mass loss rate, M = const., with respect to time and radius,

• radiative equilibrium in the Lagrangian frame,

• full non-LTE treatment of H I (10 levels), Mg II (3 levels), and Ca II (5 levels),

• LTE occupation numbers for the ionization stages I-III of He, C, N, 0, Si, S, Fe, Al,

Na, K, Ti, Sc, Mn and Cr (treated consistently with the non-LTE species),

• all relevant b-f, f-f and b-b transitions are included (b-f, f-f: Mathisen 1984; b-b:

Kurucz &: Peytremann 1978, Kurucz 1988)

Model Parameters

• the reference radius i?, which refers to the radius where either the optical depth in

absorption or extinction at 5000A is unity,

• the effective temperature Teff , which is defined by means of the luminosity, L, and the

reference radius (Teff = {L/AnR"^ a)^^^ where a is Stefan's constant),

• the density parameter, ??, {p{r) oc r~"^), • the maximum expansion velocity, I'oo, • the density, /?outi at the outer edge of the envelope,

• the metal line threshold ratio, F,

• the albedo for line scattering (metal lines only),

• the element abundances.

108
p. H. Hauschlldt and S. Starrfield 109

Model Construction

Numerical Methods:

• Approximate A-operator iteration (ALI) method for the solution of the spherically

symmetric, special relativistic equation of radiative transfer (SSRTE) for continua,

LTE, and non-LTE hnes (see Hauschildt 1992a),

• ALI method for the solution of the special relativistic, multi-level, non-LTE continuum

and line transfer problem using a direct extension of the method of Rybicki & Hummer (1991) including overlapping hnes and active continua (Hauschildt, submitted to

JQSRT),

• a hybrid method (ALI combined with partial linearization) for the self-consistent

solution of the radiative equilibrium equation in the comoving frame (see Hauschildt

1992b).

Model Computation:

• solve dr/dr = — l/\5ooo to obtain the connection between the radius, r, and the

optical depth in extinction at 5000A, r, so that r(r — I) =

• select relevant metal lines from the line list of Kurucz Sz Peytremann (1978) and

Kurucz (1988) (typically 10^ lines are treated explicitly),

• solve the SSRTE for, typically, 2000-4000 wavelength points and up to 13-25 additional wavelength points per non-LTE line, • update departure coefficients and temperature structure,

• repeat the previous steps if the required accuracy is not reached,

• for a converged model, compute a high-resolution observer's frame spectrum (typically

5000-12000 wavelength points).

Acknowledgements: We thank S. Shore, R. Wehrse and G. Shaviv for stimulating discussions. This work was sponsored, in part, by NASA grants to Arizona State University.

References

Hauschildt. P. H. 1992a. JQSRT, 47, 433.

Hauschildt. P. H. 1992b, Astrophys. J., 398, 224.

Hauschildt, P. H.. Wehrse, R., Starrfield, S., k Shaviv, G. 1992, Astrophys. J., 393, 307.

Kurucz, R.L. 1988, private communication.

Kurucz, R.L. & Peytremann, E. 1975, "A Table of Semiempirical gf Values", Smithsonian

Astrophysical Observatory, Special Report 362.

Mathisen, R. 1984, "Thoto Cross-sections for Stellar Atmosphere Calculations — Compilation of References and Data", Inst, of Theoret. Astrophys. Univ. of Oslo, Publ.

Series No. 1. Rybicki. G. B. .L' Hummer, D. G. 1991, Astron. Astrophys., 245, 171.

Figure 1: Example of the influence of line blanketing on nova spectra. The upper panel

shows the continuum energy distribution of a nova model with the parameters Teff =

10000 K, L — 20000 L0, Voo = 2000 km s"-'- and solar abundances (the structure was taken

from a non-LTE, line-blanketed model). Only H I and Mg II (h-fk) hnes are considered

in this spectrum. In the subsequent panels the number of hnes is roughly increased by a

factor of 10, respectively.
110

1000 1500 2000 2500 3000 3500

X[A]
DENSITY SENSITIVE LINES OF BORON-LIKE IONS OF C, N AND 0

PHILIP JUDGE, High Altitude Observatory, National Center for Atmospheric Research^

RONG LU, Middlebury CoUege, VT.

PAAL BREKKE, Institute of Theoretical Astrophysics, University of Oslo.

ANIL PRADHAN, Department of Astronomy, Ohio State University.

INTRODUCTION

Lines from ions of the ns"^ np isoelectronic sequences (n = 2:Boron, n = 3:Aluminum) have proven to be extremely useful as spectral diagnostics of electron densities in certain astrophysical plasmas (e.g.

Feldman & Doschek 1979; Stencel etal. 1981). These include low density {Ng < 10^^ cm"^) plasmas

at temperatures between ~ 5000 and 2 x lO^K, regimes which are typical of steUar chromospheres

and transition regions. In this paper we discuss calculations of the UV spectra of the astrophysicaUy

abundant B-like ions C II, N III and O IV, using new MaxweUian- averaged collision rates (Blum

k Pradhan 1992). These rates were computed in the close- coupling approximation using a 10

state eigenfunction basis set and should be of high accuracy (±10%). Our aim is to compare these

Ccdculations with earlier theoretical results and with observations of a variety of astrophysical objects,

to determine the value of these lines as diagnostics of plasma electron densities.

W^HY UV LINES OF BORON-LIKE IONS ARE VALUABLE

The ground term of B-like ions is 2s^ 2p ^P°. The lowest excited term is 2s 2p^ "^P (the other terms

of this configuration are ^5 ^P). Parity-changing transitions between the two lowest terms are

therefore spin-forbidden. There are five lines within the multiplet 2s 2p^ '^^5/2,3/2,1/2 2s^ 2p ^P^i2 1/2 (see Table 1). These lines are useful for studying certain properties of astrophysical plasmas because:

(i) B-like ions of C, N and 0 are abundant, and they are quite easily observed; (ii) The multiplets are usually optically thin, and are excited by electron collisions from the ground term; (iii) Hence ratios of

line intensities within the multiplets themselves are simply dependent on the electron densities of the

emitting plasmas, when collision rates between the levels are comparable with the Einstein A-values

(between lO'^ and 10^^ cm~^ for C II, N III and 0 IV); (iv) The line ratios are almost independent of

the electron temperatures and abundances; (v) the lines are close together in wavelength, and they

are of similar strength so that calibration problems are minimized.

ANALYSIS

We wish to estimate the accuracy of electron densities derived from line ratios within the 2s 2p^ ^P —»• 2s^ 2p multiplet, and then to apply the results to the analysis of astrophysical plasmas. An

important step is to check the theoretical atomic data used against available measurements. In the absence of experimental collisional and radiative data, we make comparisons with spectra of

astrophysical sources (Table 3).

Since there are three upper levels in the 2s 2p^ '^P term, there are just three independent line intensity ratios which can be derived from the five lines. The other two ratios are from lines sharing

a common upper level (Table 2), whose intensities should remain fixed in the absence of blending or

radiative transfer effects. We proceed proceed as follows: (i) We examine line ratios in selected objects; (ii) We construct

atomic models and solve the statistical equilibrium equations to obtain line emissivities and hence

intensities; (iii) We compute the sensitivity of line intensity ratios as a function of Ne, Tg] (iv)

We identify objects in which lines are formed in the high density {NeCji > Aji) and low density

{NgCji < Aji) limits; (v) We identify blends from disagreements of observed line ratios in certain

^ The National Center for Atmospheric Research is sponsored by the National Science Foundation

111
112

objects; (vi) We compare low (high) density limits with observations, yielding constraints on the

ratios of acceptable collision rates (Einstein A-values).

RESULTS AND NEEDS FOR BETTER ATOMIC PARAMETERS

For the C II] lines, the results are essentially identical to earlier work of Lennon etal. (1985) who

also performed close coupling calculations. Available spectra which sample the high density regime

(Table 3) are consistent with the atomic data used here. For N III] the new collisional data yield

Ne a factor of 2 lower than earlier work (Nussbaumer & Storey 1979), because of increased collision rates between the levels. Blends are a problem at least in the solar atmosphere (e.g. Feldman &

Doschek 1979, also see Fig. 1). Disagreements between density-sensitive line ratios suggest that a new calculation of the Einstein A values is warranted (Fig. 1). For 0 IV] the new data yield Ng factor

of 3-5 lower than earlier work, again because of increased collision strengths between the '^P levels. These lines are unblended in most spectra, with the exception of a well-known blend with S IV line

which is easily treated (Feldman & Doschek 1979).

In summary, we believe that the C II and O IV density sensitive multiplets are practical and

simple density diagnostics. Ratios of lines of N III and 0 IV are sensitive at lower densities than

previously thought, near 10^ cm~^, an important regime for the quiet sun (Doschek 1987).

REFERENCES

Blum, R.D., & Pradhan, A.K., 1992, ApJS, 80, 425

Carpenter K.G., Robinson R.D., Wahlgren G.M., Ake T.B., Ebbets D.C., Linsky J.L., Brown A., Sz Walter

F.M., 1991, ApJ, 377, L45

Doschek, G.A., 1987. In Theoretical Problems in High Resolution Solar Physics II, eds. G. Athay, D.S. Spicer,

NASA CP 2483, p. 37

Doschek G.A., Feldman U., Van Hoosier, M.E., and Bartoe, J.-D. F., 1976, ApJS, 31, 417.

Feldman, U., & Doschek, G.A., 1979, AkA, 79, 359

Hayes, M.A., & Nussbaumer, H., 1986, AfcA, 161, 287

Judge, P.G., 1986a, MNRAS, 221, 119. Judge, P.G., 1986b, MNRAS, 223, 239. Lennon, D.J., Dufton, P.L., Hibbert, A. k Kingston, A.E., 1985, ApJ, 294, 200. Nussbaumer, H., k Storey, P.J., 1979, AkA, 71, L8

Nussbaumer, H., k Schild, H., 1981, AkA, 101, 118

Sandlin, G. D, Brueckner, G. E., k Tousey, R., 1977, ApJ, 214, 898

Stencel R.E., etal. , 1981, MNRAS, 196, 47P

Table 1. Intersystem Lines of Boron like ions

Levels C II] N III] O IV]

Upper Lower A(air) A(vac) A(vac)

2s2p^ ^P5/2 2s22p2po^2 2325.398 1749.674 1401.146

^P3/2 ^P3°/2 2326.930 1752.160 1404.812

^^3/2 ^P°/2 2323.500 1746.822 1397.20

^P^/2 2328.122 1753.986 1407.386

'^Pi/2 ^Pi°/2 2324.689 1748.646 1399.774
Philip Judge et al. 113

Table 2. Ratios of Lines in the 2s2p^ 2s^2p B-Like Multiplets

Name Transition AA(C II]) AA(N III]) AA(0 IV]) Diagnostic

Ri (5/2- 3/2)7(1/2- 3/2) 2325.4/2328.1 1749.7/1754.0 1401.1/1407.4

R2 (5/2- 3/2)/(3/2- 3/2) 23:^5.4/2326.9 1749.7/1752.2 1401.1/1404.8 Ne

R3 (1/2- l/2)/(3/2- 3/2) 2324.7/2326.9 1748.6/1752.2 1399.8/1404.8 Ne

i24 (3/2- 3/2)/(3/2- 1/2) 2326.9/2323.5 1752.2/1746.8 1404.8/1397.2 A-values blends

Rs (1/2- 3/2)/(l/2- 1/2) 2328.1/2324.7 1754.0/1748.6 1407.4/1399.8 A-values blends

TnKlp 3. Sources of Emission line data, and mean A^e and Tg

Object/type Spectro- Ion Log Pe Log Ne log Te Source

graph [cm-3 K] [cm-3]

Quiet Sun /Chrom. S082B C II] 15.3 11.3 4 1

<w^uiei sun / JLr. rteg. S082B N III] ~ 15.0 10 4.85 2 Active Sun /Tr. Reg. HRTS 0 IV] 15-16 10-11 5.15 3 a Aur/G5 III+GO III GHRS 0 IV] 14.8 9.75 5.15 3 a Boo /Kl III lUE C II] 13.15 9.3 3.85 4 a Tau /K5 III lUE C II] 12.8 9.0 3.8 4

GHRS C II] 12.8 9.0 3.8 5

(3 Gru /M5 III lUE C II] 12.3 8.5 3.8 4

RR Tel /Slow nova lUE C II] 12.0 ~ 8.0 4.0 6

lUE N III] 10.9 ~ 6.7 4.2 6

lUE 0 IV] 10.9 ~ 6.7 4.2 6 V1016 Cyg /Symbiotic lUE N III] 10.9 6.5 4.2 7

/proto-PN lUE 0 IV] 10.9 6.5 4.4 7

References 1. Judge et al. in preparation. 2. Doschek etal. 1976. 3. This work. 4. Judge 1986. 5. Carpenter

etal. 1991. 6. Hayes k Nussbaumer 1986. 7. Nussbaumer k Schild 1981.

q R^ 1753.84/1748 .49 o o

o 1752.00/1746.66 (. flO)

RR TtL V1016 DFVB SBT4

Object

Boron — like Intersystem line ratios for T=70000.

RR TEL

9?, 1749.51/1753.84 - v'loie

rsy;

M' 111' BLUM-VPRADHAKl 1992

SBr4

CIF/B

DFVB

R2 1749.51/1752.00.

Rj 1748.49/1752.00 RR1ja&-

10' 10 10=^ 10 10 10' 10 12

Electron density [cm

Fig 1. Ratios of N III lines sharing a common upper level {left panel) and those sensitive to electron

densities {right panel). The lines are computed ratios, circles are observed ratios. The left panel shows

that the weak A1746 line is blended in solar data (DFVB= Doschek etal. 1976; SBT4 = Sandlin etal. 1977). The right panel suggests that, if the lines are unblended, then the Einstein A-values deserve

further work (the adopted >1(A1749.5) may be too small).
THE NEED FOR ELECTRON / NEUTRAL-ATOM COLLISION CROSS SECTIONS AT

THERMAL ENERGIES

PHILIP JUDGE, High Altitude Observatory, National Center for Atmospheric Research^

MATS CARLSSON Institute of Theoretical Astrophysics, University of Oslo.

INTRODUCTION

Analyses of UV emission line spectra of ionized atoms have led to enormous advances in our understanding of solar and stellar chromospheres, transition regions and coronae (reviews by Doschek

1987; Jordan & Linsky 1987). The gas in these plasmas is far from LTE, so that to analyze the emission

Une data requires electron-ion collision cross sections, for the processes of excitation (collisions between

bound atomic states), ionization and recombination (between bound and free atomic states), as well

as radiative data. A great deal of effort has been devoted to the determination of these cross sections,

which can be accurate to ±10% at all energies of practical interest (e.g. Pradhan k Galagher 1992).

Much of the atomic data is nov^^ available to analyze lines of ionized species formed in

transition regions and coronae.

However, the situation is considerably worse for analyses of UV emission lines of complex neutral

atoms, which are formed in stellar chromospheres, because:

(1) Chromospheric plasma has low electron temperatures (Tg < lO'^K [<0.81 eV]), an order of

magnitude smaller than typical atomic energies at UV wavelengths. Collision cross sections for

processes involving thermal electrons must therefore be determined accurately in the low energy

regime {kT^ « AE, where AE is the threshold energy for the collision). Such cross sections are

in general unavailable.

(2) Point 1. casts doubt upon the rehability of calculations based upon the assumption of weak

coupling (e.g. the Born approximations, distorted wave approximation). Such approximations (or

semi-empirical cross sections based upon them) have almost always been used in quantitative analyses

of chromospheric lines (e.g. Mauas etal. 1989).

(3) Unlike positively charged ions, excitation cross sections of neutrals approach zero as the outgoing

electron energy approaches zero (e.g., Seaton 1962). Therefore excitation rate coefficients are sensitive to resonances in the cross sections. The figure shows the threshold behavior of the electron collision cross section for the transition 2p'^ ^Po,i,2 2p^3s ^Sf in 0 I. (4) Chromospheric radiation often controls the excitation state of neutrals. Thus, other processes

(photoionization, recombination, fluoresence, cascading) can control some lines of neutrals, especially

in low gravity stars (Jordan & Judge 1984; Carpenter etal 1992).

The purpose of this paper is to demonstrate the need for accurate electron-neutral atom collision cross sections at low energies in abundant atoms with high first ionization potentials (C,N,0). We

argue that vital new clues to the elusive chromospheric heating mechanism might be obtained by

studying UV spectra of neutral atoms, once accurate collision cross sections for important transitions

become available.

ULTRAVIOLET SPECTRA OF NEUTRAL SPECIES; SOME PROBLEMS

The table Usts prominent lines of neutral species observed in a variety of stellar chromospheres. We

do not include lines for which other mechanisms are definitely responsible for the observed emission

(e.g., some S I lines in low gravity stars which are photo-excited by H Lya [Judge 1988]). Studies of

the table, with additional data from a variety of sources, reveal several problems:

(1) The solar spectra cannot be accounted for by chance fluorescence processes, even though these can explain much of the emission seen in lower density stars (e.g., Jordan &: Judge 1984).

(2) The Rydberg series of C I lines are trying to tell us something. Are they excited from above, via a large C II population, or from below, by electron collisions within C I?

^ The National Center for Atmospheric Research is sponsored by the National Science Foundation

114
Philip Judge and Mats Carlsson 115

(3) Spatially resolved data from the HRTS and SKYLAB S082B spectrographs reveal that most

neutral emission lines listed do not behave very differently from collisionally excited lines of ionized

species (see, e.g., CapeUi etal. 1989). This suggests that electron collions are responsible for a large

fraction of the neutral line emission (e.g., Athay & Dere, 1991).

(4) Carlsson k Judge (1992) studied in detail the 0 I resonance lines near 1304A, and the intersystem

hnes near 1355A. The only available low energy cross sections were computed in a three state close

coupling calculation by Rountree (1977). They found that electron collisions from the ground term

were very inefficient in exciting these lines, owing to small threshold collision strengths {Cl ~ 0.5), and

that photo-excitation by H Ly0 dominates the exitation of A1304.

(5) If H Ly,d is responsible for exciting O I A1304, then what is exciting the other 0 I lines, and why

do the A1304 lines behave like collisionally excited lines?

(6) The HRTS data show tantalizing behavior of intensity ratios of O I intersystem lines to resonance

lines (see also Cheng etal. 1980): if these lines are really influenced by electron collisions (in

contradiction to present calculations), then valuable diagnostics of the chromospheric electron density

may become available. In summary, there exist UV data of neutral C, N, 0 and others, for which important questions

remain unanswered. Many lines behave in HRTS data like collisionally-excited lines, and yet computed

cross sections at thermal energies (available for O I only) are too small by perhaps an order of

magnitude to account for the observed intensities. At least two important possibilities arise: (1)

The available near-threshold collision cross sections are inaccurate, or (2) the chromospheric electron

distribution is not Maxwellian. A small population of non-thermal electrons (which presumably

result from the unknown chromospheric heating mechanism), at energies substantially higher than

kTe, might explain all of the above observations. Clearly, the possibility of putting quantitative

estimates of populations of non thermal electrons in the solar chromosphere is of central interest to

studies of the heating mechanism itself. The only way to answer these questions is through

calculations using accurate electron-atom collision cross sections.

IMMEDIATE NEEDS FOR BETTER ATOMIC PARAMETERS

The accompanying table is a good starting point for a "wish list" for studies of solar and steUar

chromospheres. With radiative data accurate to ±10% being routinely available for these transitions

from the OPACITY project, collision cross sections from highly populated lower levels of C,N and 0

atoms (including metastable levels) are needed to a similar degree of accuracy.

REFERENCES

Athay, R.G. k Dere, K.,P., 1991, ApJ, 379, 776

Carlsson, M., k Judge, P.O., 1992. ApJ (in press)

Cappelli, A., Cerruti-Sola, M., Cheng, C.C., k Pallavicini, R., 1989, A&A, 213, 226. Carpenter, K.G., Robinson, R.D., Wahlgren, G.M., Linsky, J.L., k Brown, A., 1992, In Science with the Hubble

Space Telescope, in press Cheng, C.C., Feldman, U., k Doschek, G.A., 1980, AkA, 377, 379

Doschek, G.A., 1987. In Theoretical Problems in High Resolution Solar Physics II, eds. G. Athay, D.S. Spicer,

NASA CP 2483, p. 37

Doschek G., Feldman U., Van Hoosier M.E. k Bartoe J.-D.F, 1976, ApJS, 31, 417

Feldman, U., k Doschek, G., 1991, ApJS, 75, 925

Jordan C. k Judge P.G., 1984, Physica Scripta, T8, 43

Jordan, C. k Linsky, J.L. 1987, in Exploring the Universe with the lUE Satellite, Ed. Kondo Y., Reidel:

Dordrecht, p. 259

Judge, P.G., 1986a, MNRAS, 221, 119

Judge, P.G., 1986b, MNRAS, 223, 239

Judge, P.G., 1988, MNRAS, 231, 419. Mauas, P.J., Avrett, E.H., k Loeser, R., 1989, ApJ, 345, 1104
116

Pradhan, A.K., ^ Galagher, J.W., 1992, ADNDT in press Robinson, R., etal. , 1992, The Seventh Cambridge Workshop on Cool Stars, Stellar Systems and the Sun,

Eds. J. Bookbinder & M. Giampapa, PASP Conf. Series 26, p. 31

Rountree, S.P., 1977, J. Phys. B.: Atom. Molec. Phys., 10, 2719.

Seaton, M.J., 1962. In Atomic and Molecular Processes, ed. D.R. Bates, New York: Academic Press, ch. 11 SOME PROMINENT ULTRAVIOLET CHROMOSPHERIC LINES OF NEUTRAL ATOMS (914-1940A)

Ion Lines Transitions Object

H I Lyman series (918-1215A) n=l -> n=2,12 Sun

C I Rydberg series (1114-1158A) 2s22p2 3p ^ 2s^2p{^P°)nd,ns i,3po i,3j^o i,3jro

2s22p2 i£) ^ 2s^2pl^P°)nd,ns ^P\^D°,^F°

2*2 2p2 3p _ 2s2p^ ^P°

Sun

Rydberg series (1256- 1481 A) Sun, AU Mic

1329A Sun

156lA 2s^2p^ 2p ^ 2s2p3 3^0 Sun

1657A 2s22p2 3p ^ 2s^2p3s ^P° Sun, Giants

193lA 2s22p2 i£) ^ 2s^2p{^P°)3s ^P° Sun

N I 1134A 2s2 2p3 ^5° ^ 2s2p^ ^P Sun

1143A 2s22p3 2^0 _^ 2s22p2(3p)3rf ^P,^D,^F

2s^2p^ 2s22p2(3p)3d4p^2£) 2p

Sun

1163-1170A Sun

1492A 2s22p3 2^0 ^ 2s22p23s 2p Sun

0 I 988A 2s22p4 3p _^ 2s^2p^(^D°)is

2s22p4 2s22p3(2D°)3s ^D"

Sun

1152A Sun

1304A 25^2^^ 3p _^ 2s22p33s ^5° (Many)

1355A 2s22p'' 3p ^ 2s22p33s (Many)

Sources: Solar data (914-1177A)- Feldman Sz Doschek 1991. Solar data (1175-

1940A)- Doschek etal. 1976. AU Mic (dMe flare star) data from the Hubble

Space Telescope- Robinson etal. 1992. Giant star data- Judge (1986a,b).

Energy above threshold [Unit is 10^ K]

0 2 4 6 8

0.00 0.10 0.20 0.30 0.40 0.50

Energy E above threshold [RYD], threshold = 0.63Ryd

Cross section {solid line) for coUisional excitation of the 3* level from the 2p'^ ^P ground

term of O I, from Rountree (1977), and a locus {dashed line) of energies Ehaif{Te) at which

/(f""'' Q{E)exp{-E/kTe)dE = 0.5 • Q{E)exp{-E/kTe)dE . Q{E) is the usual "collision strength"

(= ^^^^gi^^ [^-S-' Seaton, 1962], where (Tij{E) is the cross section for transitions from level i to level j

at energy E, and gi is the degeneracy of level i). The excitation rate is proportional to these integrals.

Notice that much of the excitation rate is determined at energies very close to threshold.
Laboratory Sources

Interpretation of the VUV Spectra of Some Iron

Group Element Ions

W.-O L. Tchang-Brillet. l J.-F. Wyart.^ V. Azarov,3 L.I. Podobedova,^ A. N. Ryabtsev^

^ Ddpartement Atomes et Molecules en Astrophysique,* Observatoire de Paris-Meudon,

92190 Meudon, France

2 Laboratoire Aim6 Cotton,** CNRS II, Batiment 505, 91405 Orsay, France

^ Institute of Spectroscopy Academy of Science, Troitsk, Moscow region, Russia

A great amount of observational data in the VUV wavelength region

(1050-3000A ) is provided by the lUE satellite and the Hubble Space Telescope.

The interpretation of the stellar spectra taken from space requires the

knowledge of a large number of atomic spectra. The data needed include accurate

wavelengths, oscillator strengths, collisional and photoionization cross sections

etc. As an example, the research program concerning the chemical-peculiar

stars for more accurate elemental abundance determinations requires improved

data for the first ionization stages of all the iron group elements.

We are investigating the VUV spectra (380 - 2000A) of three- and fourtimes ionized manganese Mn3+ (Mn IV) and Mn'*''"(Mn V). Previous

publications[l, 2, 3] concerned the transition arrays - 3d^4p (478 - 847A) in

MnlV, 3d3 - 3d24p (380-547A) and 3d^4s - 3d24p (1086 -1915A) in Mn V. The

present work concerns the 3d^4p - 3d^4d, 5s transitions in Mn V and the 3d34s -

3d^4p, 3d^4p - 3d^4d, 5s transitions in Mn IV. The spectrograms were obtained on photographic plates either in Meudon,

with a vacuum triggered spark, using the 10.7-meter normal incidence vacuum

spectrograph of the Paris-Meudon Observatory, or in Troitsk, using a 6.65-m

normal incidence vacuum spectrograph, with a similar triggered spark source,

which is operated in different conditions so as to enhance the emission of lower

ionization stages.

The plates were measured on semi-automatic comparators. Selected

impurity lines of oxygen, nitrogen, carbon and Mn^''" were used for wavelength

calibration. The uncertainty of the relative positions of the lines is estimated to

be ±0.005A. About 250 lines of Mn V and about 800 lines of Mn IV are newly

identified in the wavelength range 660-I900A.

i

* Also associated with CNRS (URA 812)

** Also associated with Universite Paris-Sud

119
120

The analysis, i.e., the identification and the classification of spectral lines

by the energy levels involved, was guided by theoretical studies of the atomic

structure, as developed in [4], which predict the level positions and the line

strengths. Isoelectronic comparisons were also a useful support. An automatic

search-for-level computer code was used, taking into account the theoretical

relative intensities of the transitions. Then the results were checked to avoid

fortuitous coincidences. 60 new energy levels, belonging to the 3d^4d and Sd^Ss

configurations of Mn V, and more than 100 levels, belonging to the 3d'^4s and

3d-'4d configurations of Mn IV, are determined. The determination of the 3d^5s

configuration is in progress.

All the configurations were interpreted by parametric studies. In the case of the Sc-like Mn^+ ion, a GLS (Generalized Least Square) calculation was

performed, by adding the data for Ti II[5], V III[6] and Cr IV[7] to the new Mn V

levels. Independent studies of the 3d^(4d+5s) group had shown that the Slater

parameters P increase nearly linearly with Zc, the charge of the ionic core, and

that the constraint of the expansion P = A + BZc + F/(Zc + 2) does not increase

substantially the deviations Eexp - Eth- The improvement of the ratio (number of

experimental levels)/(number of parameters) allows a better determination of

"small" parameters, i.e., the configuration interaction parameters R2(3d4d, 3d5s)

and R2(3d4d, 5s3d). Earlier systematic studies of the 3d^ core configurations

helped in fixing some parameters to reliable values[8]. The fitted parameter

expansions are summarized in the Table. They are of interest for prediction of

level positions, and thus transition wavelengths for higher members of the

isoelectronic sequence. The extension of the present work to the isoelectronic

ions of iron Fe^"*" (Fe V) and Fe^"*" (Fe VI) is also in progress.

References

1. W.-tl L. Tchang-Brillet, M.-C. Artru and J.-F. Wyart, Physica Scripta 33, 390

(1986).

2. V. I. Kovalev, A. A. Ramonas, A. N. Ryabtsev, Opt. Spectrosc. 43, 4 (1977).

3. L. I. Podobedova, A. A. Ramonas, A. N. Ryabtsev, Opt. Spectrosc. 45, 237 (1978).

4. R. D. Cowan, "The Theory of Atomic Structure and Spectra", University of

California Press, (1981).

5. S. Huldt, S. Johansson, U. Litzen, J.-F. Wyart, Physica Scripta 25, 401 (1982).

6. L. Iglesias, O. P. y Appl. 2, 132 (1969).

7. J. O. Ekberg and L. Engstrom, Physica Scripta 25, 611 (1982).

8. J.-F. Wyart, A. J. J. Raassen, P. H. M. Uylings, Physica Scripta 32, 169 (1985).
W.-U. L. Tchang-Brillet et al. 121

Table Expansion of energy parameters fitted from 237 levels of the

sequence Ti II - Mn V Sd^ (4d+5s)

P = A + BZc+CZc2 + DZc3+EZc'^ + F/ (Zc + 2)

Parameter values and standard errors in cm"^. Parameters without standard

error have been fixed.

The r.m.s. deviation is 82 cm' ^

Parameter A B C D E F

F(2)(3d,3d)d2d* 44684 (455) 9505 (96) -86240

F(2)(3d,3d)d2s* 45006 (501)

M

F4(3d,3d)d2d * 34053 (735) 5900 (156) -83790

F4(3d,3d)d2s * 35489 (808)

F2(3d,4d) -1671 (303) 3594 (78)

F^(3d,4d) -1657 (284) 1964 (79) _—__

G0(3d,4d) -416 (42) 1123 (11)

G2(3d,4d) -551 (225) 1423 (60)

G4(3d,4d) -145 (269) 955 (74)

G2(3d,5s) -4835 (2375) 1140 (265) 16204

(7672)

R2(3d4d,3d5s) 200 341 (75)

R2(3d4d,5s3d) 140 326 (77) a

* 20.75 4.61 -45.02

-105.25 0. 152.17

xi 0 120 (14)

80 (38)

C3d d^d * -24.82 (29) 2.271 (0.6) 0.6690 0.00506 0.00015

C3d d^s * -28.97 (31)

Ud -21.9 (43) 14.33 (12) 1.

* For those parameters relative to the core, Zc is to be replaced by Zc -i- 1 in the

parameter expansion.
VXrV—LiDiets of Low—Z Ions aLnd Ttie±ir

H.H. Bukow, A. Bastert, G. Rieger and M. Krenzer

Ruhr-Uni vers i tat Bochum, Exper imenta 1 phys ik III

Postfach 102148 NB 3 D 463 Bochum

Introduction. At the last conference of this series, Kurucz

[1] pointed out that "half of the lines in the solar spectrum are unidentified or unclassified". Laboratory observations of such lines are often hindered by the difficulty

of establishing an environment capable to produce similar

excitation conditions. The beam-foil technique [2] combines

very strong interaction inside the foil and aii interactionfree decay outside. The observation of numerous lines stemming from doubly-excited states [3] , hardly accesssible with

other light sources, indicates that beam-foil spectroscopy

approaches certain photospheric conditions. Therefore a

systematic spectroscopic study of the astrophysical ly important elements N, O and Ne at low ionization stages covering

a wavelength range from 40 nm to 120 nm was performed. As a

preliminary result we note a surprisingly large number of

up-to-date unknown lines. In this report the experimental

technique, the type of data and some selected results will

be described.

Experimental Procedures. State-of-the-art beam-foi 1 spectroscopy is used. A 400 keV accelerator yields ^A beams of the

ions in question. To get higher projectile energies some

measurements are done using 2+ and 3+ ions, respectively. A

2-m normal-incidence monochromator , designed to match the

requirements of fast-beam spectroscopy (ref ocal isation for

all wavelengths [4]), is used to scan the light emitted at

90" to the beam axis. With 80 ^m (equal) slits and a 2400

1 /mm grating a linewidth (FWHM) between 0.025 nm and 0.040

nm depending on the projectile energy and mass and the foil

thickness is realized. Once a spectrum is registered the

122
H. H, Bukow et al. 123

positions of the spectral lines are determined by fitting a

Gaussian profile to each feature. Then a number of wellknown lines (typically: 25) are identified and used for the

calibration, yielding a wavelength accuracy of 0.004 nm (one

standard deviation) for well resolved lines. The charge

state of the emitting ion can be deduced approximative 1 y

from the variation of the individual line intensity as a function of the projectile energy. The confidence level of

this procedure is good for most lines but deviations may

occur up to an uncertainty of ± 1 unit. To exhaust all

sources of information available with the beam-foil technique lifetime measurements are performed for a number of

transitions. Lifetime data (typical accuracy: 10 % to 20%)

are aimed as a supplementary information in the process of

line identification. These measurements are evaluated using

a mul tiexponential fitting program (DISCRETE [5]). Finally

it may be helpful to have a measure of a line's intensity

-2 -1 (photons. cm .s ) . To get meaningful numbers, the intensities

of most of the unknown lines together with a suitable reference line are measured using a recent efficiency calibration [6] . If an identification for a line is proposed, the measured

lifetime may be compared to what is expected theoretically.

Calculating population numbers from the intensities the

population of the state in question may be compared to the

reference state if some assumptions are made concerning the

dependence of the population on the main and angular quantum

numbers n and 1, respectively.

Results. The evaluation of the bulk of data being still

under work we present only some results concerning neon.

Two decades ago, Edl^n et al . [7] determined by extrapolation the relative positions of triplet and quintet spectra

in Ne V, and of doublets and quartets in Ne IV [8] . Both

numbers are the respective basis of the corresponding level

system as tabulated by Kelly [9] . To our best knowledge they
124

have not been verified experimentally. We have directly mea2 2 ^ 3 5 0 sured the 2s 2p P-2s2p S ground state transitions in Ne V,

estimated to 113.704 nm and 114.613 nm [7] and observed at

(113.627310.008) nm and (114.564810.008) nm, respectively.

Moreover we have identified other 16 transitions between

those systems and one singlet-triplet transition. In Ne IV

44 doublet-quartet transitions have been observed. The difference in wavelength between the present work and the value

calculated on the basis of Kelly's table [9] yields the uncertainty of the relative position of the spin-different

systems, named X in the case of Ne V and E for Ne IV [9] . From the total of observed intersystem lines we have

X=(0125) cm ^ and E=(0136) cm ^ thus confirming the estimates

of Edl6n [7,8].

To give an impression of the amount of identification work

still to be done we quote approximate numbers of unknown

(known) lines as oberved. They are: 460 (200) for neon, 50

(200) for oxygen and 80 (350) for nitrogen.

Acknowledgement. The authors wish to express their gratitude

to F.J. Meijers (Amsterdam) for his help and encouragement

in the identification of intersystem lines.

References

[1] R.L. Kurucz, in J.E. Hansen (Ed.): Atomic States and

Oscillator Strengths for Astrophysics and Fusion Research, North Holland, Amsterdam 1990, p. 20

[2] for a review, see: H.J. Andra, in W. Hanle and H.

Kleinpoppen (Ed.): Progress in Atomic Spectroscopy,

Plenum, New York 1979, part B, p. 829

[3] for a review, see: S. Mannervik, Phys . Scripta

40( 1989) 28

[4] J.O. Stoner, J. A. Leavitt, Optica Acta 20(1973)435

[5] S.W. Provencher, J. Chem. Phys. 64(1976)2772

[6] A. Bastert, H.H. Bukow, H.v. Buttlar, Appl . Optics (in

print

)

[7] B. Edl6n, H.P. Palenius, K. Bokasten, R. Hallin, J.

Bromander, Solar Phys. 9(1969)432

[8] B. EdUn, Solar Phys. 24(1972)356

[9] R.L. Kelly, J. Phys. Chem. Ref. Data 16(1987) Suppl.l
ANALYSIS OF THE (5s5p'+5s'5d) - [ 5p^+5s5p5d+5s5p6s ] TRANSITIONS OF I V

A. Tauheed and Y. N. Joshi

Physics Department, St. Francis Xavier University,

Antigonish, NS, Canada B2G ICO

Introduction and Experiment

The groundstate of four times ionized iodine (IV) is 5s^5p^. Kaufman et

al [1] revised the earlier work of Even-Zohar and Fraenkel [2] . They established

levels of the 5s^5p, 5s5p^, 5s^ ns (n = 6-8) , 5s^nd (n=5, 6) configurations and the

5p^ ^S. Ansbacher et al [3] investigated I V spectrum using Beam-foil technique

and reported the 5s^6p levels, revised 5s5p^ ^P levels of Kaufman et al [2] and

rejected the Sp-* level. During our recent investigation of the I IV spectrum

[4] we were able to achieve very reliable ionization discrimination between the

I III, I IV, IV and I VI lines. We observed that the line at 1168.8 A classified

by Goslin et al [3] as 5s^5p ^Pi/2 ~ 5s5p^ ^^3/2 in fact an I III line. This

lead us to study the 5s^5p^ ^P - 5s5p^ *P transitions in the Cd I isoelectronic

sequence from Sb III to La IX [5] . However, further confirmation of the *P system can be obtained only by studying the configuration systems containing

quartet terms. These configurations are Sp"*, 5s5p5d and 5s5p6s and consequently

their investigation was undertaken. The preliminary results and presented here.

The spectrum of iodine was photographed in the 300 A - 2000 A region on a 3-m normal incidence spectrograph (plate factor in first order 1.385 A/mm) . The source used was a triggered spark in which Li I salt was packed into the cavity

of an aluminum sample electrode. The second electrode was a pure aluminum

electrode. By introducing various turns of an inductance coil in the discharge

circuit we could enhance or suppress the lines of different ionization stages.

The polarity exhibited by the lines of higher ionization was also a reliable

criteria for the ionization discrimination. Further experimental details appear

in our earlier paper [4]. Accuracy of wavelength measurements for sharp lines

is ±0.005A.

5s5p6s

Results and Discussion

The 5p^,5s5p5d and 5s5p6s

configurations contain five

quartet terms which give rise

to strong transitions to the

5s5p^ *P term. These three

configurations were calculated

using Cowan Code [6] with the

scaling factors similar to the

ones in other iodine spectra

studied in our laboratory. The

E,^ (RHF) of the 5s^ 5s5p5d,

5s^6p and 5s5p6s configurations

in Cd I isoelectronic sequence

from Sb III to La IX are shown

in Figure 1. It is clear that

whereas the 5s5p6s configuration rises fast the Sp"" and

5s5p5d configurations collapse

along the sequence. Soon it was noticed that the 5s5p^ - (5p^+5s5p5d) transition array

appeared very strong where as transitions arising out of the

5s5p^ - 5s5p6s array were relatively weak. All levels

belonging to the 5p^ and almost

90% of the levels belonging to

the 5s5p5d and 5s5p6s configurations have been established

125
126

are listed in Table I. The 5p^ ^S^,^ level reported by Kaufman et al [1] and a revised value suggested by Ansbacher et al [3] were both incorrect. The levels

marked (?) are based on definite I V lines but need some further checking. One

also expects moderately strong lines arising out of 5s^5d - (5s5p5d+5s5p6s)

transitions. We could not see any of these lines in our line list. On

rechecking the data it was found that 5s^5d identified earlier [1,2,3] was incorrect. New values of 5s^5p are given in Table II. These levels gave

transitions to the 5s5p5d, 5s5p6s, and to the 5s^6p levels reported form the beam

foil study. Over 150 additional lines have been classified in the spectrum.

Complete analysis involving configuration interaction calculations will

follow soon. We wish to thank Natural Sciences and Engineering Research Council of Canada

(NSERC) for the financial assistance.

References

1. V. Kaufman, J. Sugar and Y.N. Joshi, J. Opt. Soc. Am. B. _5, 619 (1988).

2. M. Even-Zohar and B.S. Iraenkel, J. Phys . B. 5., 1596 (1972).

3. W. Ansbacher, E.H. Pinnington, A. Tauheed and J. A. Kernahan, J. Phys. B:

At Mol. Opt. Phys. 24., 587 (1991).

4. A. Tauheed, Y. N. Joshi and V. Kaufman, J. Phys. B: At. Mol. Opt. Phys.

5. A. Tauheed, Y. N. Joshi and E. H. Pinnington, J. Phys. B: At. Mol. Opt.

Phys . (in press)

6. R. D. Cowan, Theory of Atomic Spectra and Structure and Cowan Code

programs

Table I New energy level values (cm'M of I V belonging to the, 5p^, SsSpSd and 5s5p6s

configurations

Config Desig J Level (cm"M Config Desig J Level (cm"^)

5p' 'S 3/2 209984 5s5p5d 5/2 226526

3/2 204472 5s5p5d 5/2 236379

5/2 210092 5/2 245331

^P 1/2 228924 5/2 248068

3/2 233038 5/2 251760

5/2 274074

5s5p5d 1/2 237451 5/2 278712

5s5p6s 1/2 246459 5/2 281342

1/2 261368 7/2 230308

1/2 281051 7/2 244734

1/2 304619 7/2 258571

3/2 224080 7/2 278129

3/2 237300

3/2 246966

3/2 249250

3/2 264136

3/2 277513

3/2 283800

3/2 306461
A. Tauheed and Y. N. Joshl 127

Table II

New or revised level values (cm'M of the levels of

the 5s5p^ *P, Ss^Sd and 5s^6p of I V

Conf ig Desig J Level {cm"M

5s5p' 4p la) 1/2 81003

3/2 86899

5/2 92554

Ss^Sd • 2d"" 3/2 154050

5/2 155462

5s^6p 2p(c) 1/2 211216

3/2 215054

From ref , [5] , included for completeness

New levels

Revised value of beam foil data
New High Excitation Fe I Levels determined by Fourier

Transform Spectrometry

Gillian Nave, Sveneric Johansson

Department of Physics, University of Lund, Solvegaian I4, S-223 62 Lund, Sweden

Abstract

Seven new subconfigurations in Fe I, ranging from 56000 - 60000 cm~\ have been found

using Fourier transform spectra. The total number of levels is 166, giving lines in both the

infra-red and visible range. A summary of the methods of analysis, and comparisons with

solar and grating spectra are described.

1 Introduction

The high quality of recent solar IR spectra obtained with the ATMOS space experiment [1] has

illustrated the need for more identifications of atomic lines, with Fe I being particularly important.

Recent discovery of lines due to id^{^ D)4s'if — bg transitions in both laboratory and solar spectra

resulted in classifications of levels as high as 60300 cm~^, which have been used in confirming the

solar iron abundance [2]. The accuracy of the solar spectra means that high resolution Fourier

Transform (FT) spectra must be used for laboratory identifications. This paper describes levels from seven new subconfigurations of Fe I which have been analysed

using FT spectra, which range in energy from 56000 cm" Ho 60000 cm~^. Details of the levels and

identifications will be published separately in the near future. The work will also form part of a new multiplet table for Fe I that is currently being prepared.

2 Laboratory Measurements

The spectra used in this analysis were recorded with the IR-visible FT spectrometer at the National

Solar Observatory, Tucson, Arizona, and with the vacuum-ultraviolet FT spectrometer at Imperial

College, London. A hollow cathode lamp of pure iron was used as a source, and was operated

in neon or argon at pressures of 3 - 4 Torr, with a current of 400 - 1400 mA. The cathode was

water cooled for one infra-red spectrum. Details of the experimental setup are given in [3]. The

wavenumbers, intensities and widths of all the lines in each spectrum were determined with the DECOMP computer code [4], and the wavenumbers carefully calibrated from Ar II standard lines

[3, 5].

3 Term Analysis

Terms arising from five even parity subconfigurations and two odd parity subconfigurations have

been found, due to the lowest two parent terms, 3d^{^D)4s and Sd^C^F) in Fe II. They cover the

energy range 56000 cm~Ho 60000 cm~^ Figure 1 shows the energy ranges of the new levels, with

the most important transitions. Values for the lower levels of the transitions involved were taken from [6], or the atomic energy

level table (AEL) [7]. Eight levels due to the D)4sbd subconfiguration were discovered by

Brown et. al. [8], and levels from both this and the 3d^{'^F)Qs subconfiguration were found by

Zhu and Knight using laser spectroscopy [9]. The accuracy of these levels has been substantially

improved, and both subconfigurations are now almost complete. The D) and (^G) terms of

3d^{^ D)4s{'^ D)4d and one Zd^{^ D)As7s term are also listed in the AEL. No previous levels of the

3d^(''F)4/, 3cf^(^D)4s5/, or 3(i^(^F)5d are listed.

128
Gillian Nave and Sveneric Johansson 129

Figure 1: Partial Term diagram for Fe I showing energy ranges of the new levels, and major

transitions. Solid lines represent the transitions used to find the levels, and broken lines indicate

other important transitions. The terms Zd^{^D)4sAp and Zd'^{^F) 4p are much lower in energy

(19000 cm"^to 40000 cm~^), and hence their position is not shown.

The overlap of the configurations in Fe I results in strong configuration interaction. This means

that many inter-parent trcinsitions are seen, giving many lines throughout the visible and infra-red. The mixing is particularly strong between the Zd^{^ D)As5d and Zd^{'^F)6s subconfigurations, and

the 3<f^('D)4s7s, Zd'^{*F)5d and Zd^{^D)4s{'^D)4d subconfigurations. As no particular coupling

scheme adequately describes these levels, LS designations have been assigned. The two odd parity

subconfigurations - Zd'^{*F)4f and Zd^{^D)isbf - are best described in the JK coupling scheme.

Levels have been assigned to each subconfiguration according to both the calculations of Kurucz,

and according to the strongest expected transitions from each level. These transitions are marked

with solid lines on figure 1. Other transitions are useful in confirming the identifications, and are marked with dotted lines. Transitions to the 4d, two 5d, 6s and 7s subconfigurations from the lowest odd subconfigurations Zd^{^D)AsAp and Zd^{^F)4p fall in the ultraviolet and are not present in the FT spectra.

Some evidence was present in grating [8] and solar spectra. Transitions between Zd^{^ D)4s5f and

Zd''{^F)As were also observed in grating spectra, and work is continuing on these identifications. Comparisons were also made with solar spectra. The Zd^(^D)4s5d - 5/ transitions fall in the

infra-red above 2 fim, where the high quality ATMOS spectra referred to earlier were used. Work

is continuing in confirming the identifications. Between 1 and 2 fj,m, the Kitt Peak photometric

atlas [11], was used, but proved less useful due to strong atmospheric absorption in many of the regions covered. The Zd^{^ D)4s4p - 4s(^D)4d are strong in the visible region, and the Kitt Peak

Table of Photographic Solar Spectrum Wavelengths was used to obtain equivalent widths [10]. A

plot of the equivalent width in the solar spectrum against the log of the laboratory intensity is useful in verifying transitions and detecting blended lines [12].

4 Summary

Even terms of Fe I have been found up to 60000 cm"S with only a few terms of low J in the

described subconfigurations still to be found. Only one even subconfiguration - the Zd^{^D)4s6d
130

remains to be found in this range. Work has commenced on the odd terms with the Zd^{'*F)if

and 3(i^(^D)4s5/. The results of all this analysis will be published in the future as part of a new

multiplet table for Fe I.

5 Acknowledgements

G. Nave gratefully acknowledges a Research Fellowship from the European Space Agency, under

which this work was carried out. We also thank A. J. Sauval for his assistance with the solar

identifications, and R. C. M. Learner and J. W. Brault for provision of the laboratory spectra.

References

[1] Farmer, C. B., Norton, R. H. , NASA Ref. Publ. 1224, NASA Scientific and Technical Infor- mation Division, Washington D. C. (1989)

[2] Johansson, S., Nave, G., Geller, M., Sauval, A. J., Grevesse, N., Schoenfeld, W. G.,

Chang, Ed. S., Farmer, C. B., (1992) in preparation.

[3] Nave, G, Learner, R. C. M., Thome, A. P , Harris, C. J., J. Opt. Soc. Am. B8 (1991) p 2028.

[4] Brault, J. W. , Abrams, M. A., vol 6 of 1989 OSA Technical Digest Series (Optical Society of

America) p 110.

[5] Nave, G, Learner, R. C. M., Murray, J. E., Thorne, A. P., Brault, J. W., J. Phys. II France 2

(1992) pp 913

[6] O'Brien, T. R., Wickliffe, M. E., Lawler. J. E., Whaling, W., Brault, J. W., J. Opt. Soc. Am.

B8 (1991) pll85.

[7] Sugar, J., Corliss, C, J. Phys. Chem. Ref. Data 14 (1985) Suppl 2.

[8] Brown, C. M., Ginter, M. L., Johansson, S., Tilford, S. G., J. Opt. Soc. Am. B5 (1988) p 2125.

[9] Yang Zhu, Knight, R. D, J. Opt. Soc. Am. B9 (1992) p 27.

[10] Pierce, A. K., Breckinridge, J. B., Kitt Peak National Observatory contribution no. 559.

[11] Delbouille, L., Rolemd G., Brault, J. W., Testerman, L., "Photometric Atlas of the Solar

Spectrum from 1850 to 10000 cm-^". (Tucson:KPNO) (1981).

[12] Johansson, S., Learner, R. C. M., Astrophys. J. ,354 (1990) p755.
A PROGRESS REPORT ON THE ANALYSIS OF VUV-FTS SPECTRA

OF RU I AND RU II

All Joueizadeh and Sveneric Johansson

Lund University, Department of Physics, Solvegatan 14, S-223 62 Lund, Sweden

1- INTRODUCTION

High-resolution spectra of the chemically peculiar star % Lupi obtained

with the Goddard high-resolution spectrograph (GHRS) on board the

Hubble Space Telescope (HST) have revealed the existence of singly

ionized ruthenium in the stellar atmosphere [1]. Spectral lines at

1939 A of Ru II in the stellar spectrum were shifted about 16 mA

compared to laboratory data, and the difference seemed to be

systematic. A revision of previous experimental results would help to

clarify these wavelength shifts. The latest measurements of the Ru 1

1

spectrum were performed by A.G. Shenstone and W. F. Meggers [2].

In this paper we report on new recordings of the Ru spectrum, emitted

by a hollow-cathode lamp, with the VUV-FTS at Lund.

1.2

I I I I I I I I I I [ I I I I I I r I I I I I I

' ' ' I ^1^

I I I I t I ' ' '

I 'I I I I 'I'll''''''

Pt

I ' ' I I I I I I i' 0.0

1938.8 1939.0 1939.2 1939.4 1939.6 1939.8 1940.0

Wavelength (A)

Figure 1. HST/GHRS spectrum of x Lupi, showing the Ru II lines.

Solid line = observed spectrum, dashed line = synthetic spectrum

131
132

2. MEASUREMENTS

We have registered Ru I and Ru II lines with the new VUV-FTS at Lund in

the following regions: 1750-3162 A, 2113-4215 A, and 4160- 6325 A. A

hollow-cathode has been used as a light source. We inserted ruthenium

powder in a nickel cathode and ran the source with neon. The spectrum,

which contains emission lines of Ru I , Ru 1 1 , Ni I, Ni II, Ne 1 1 and

Ne III, has been calibrated against Ni and Ne lines. The accuracy of

the measurements is about 0.005 cm'^ (0.2 mA at 2000 A). Totally 213

Ru 1 1 and 1053 Ru I lines have been measured.

In Table 1 we compare new FTS wavelengths with those from [2] for a number of Ru II lines to illustrate the systematic shift, which appears

below 2230 A.

When the new wavelength values were used in the calculation of the

synthetic stellar spectrum of x Lupi, a good agreement was obtained

whith the observed spectrum, as illustrated in Figure 1.

Many energy level values have been improved for both Ru I [3] and Ru 1

[2], see table 2, where also some new levels are included. The analysis

is in progress. The term analysis is guided by theoretical calculations

of energy levels and line intensities of Ru 1 1 by means of the Cowan

computer codes.

FTS wavelengths

(A)

Shenstone & Meggers [2]

(A)

difference

(A)

3177 0488 3177. 048 0 001

2778 3888 2778. 388 0 001

2887 4939 2687. 494 0 000

2571 0899 2571. 09 0 00

2455 531

2455. 53 0 00

2396 7103 2396. 71 0 00

2281 7212 2281. 72 0 00

2218 5333 2218. 552 -0 019

2192 8634 2192. 889 -0. 026

2113. 8708 2113. 895 -0 024

2107. 3074 2107. 322 -0. 015

2074. 5518 2074. 581 -0. 029

2049. 0912 2049. 111 -0. 020

1966. 7313 1966. 746 -0. 015

1966. 0660 1966. 076 -0. 010

1939. 5053 1939. 521 -0. 016

1939. 0432 1939. 056 -0. 013

1844. 1340 1844. 138 -0. 004

Table 1. Improved Ru II wavelengths. Note the systematic

shift below 2218 A of the previously measured wavelengths.
All Joueizadeh and Sveneric Johansson 133

Ru I

Level Energy(cm M

old new

4d''(a*F)5s aV

2 2713 24 2713 275 aV

I 3105 49 3105 520 aV4 6545 03 6545 048

2 20933 75 20933 772

4d'5s^

4 21543 09 2 1643 071

4d' b'D

2 23453 47 23453 377

7 4 4d (a F)5d e^)

3 47188 32 47188 348 48521 77 48521 860 48727 68 48727 749

4d*5s6s ^\ 50016 70 50016 813 4d'5s5p z'd 254^4 49 25464 520 4d''(aV)5p 27506 59 27506 623 4d*5s5p 35046 77 35046 814 ^\ 35471 15 35471 206

4d"'(a^D)5p

2 41182 94 41182 951 4d''(a^H)5p x='g

3 43975 79 43975 830 4d'(a^P)5p

2 43509 17 43509 209

Ru II

Energy(cm ^

)

Level old new

4d^ aV7/2 1523 1 1523 269 aV5/2 2494 9 2493 937 aV

3/2 3104 2 3 104 267 4d*(*D)5s a'D

7/2 10150 4 10150 925

a'D

5/

2

10851 7 10852 170 4d'(*D)6s e'D

9/2

7/2

5/2

84510 g 84511

85411 86137

455

1 12 668 e^3/2 86602 315

7/2 86440 4 8644

1

216

e*D

S/2 87523 4 87523 595

4d*5d 9/2 89347 373

4d'5d 7/2 91036 427 4d'(*D)5p

9/2 46471 9 46472 527 ^\/2 46711 5 467]] 916

11/2 50758 3 50758 676 54794 3 54794 672

3/2 56664 9 56665 349

1/2 57263 8 57264 022

Table 2. Examples of improved and new energy levels in Ru I and Ru II.

REFERENCES

1 D.S. Leckrone, S.G. Johansson, and G. M. Wahlgren,

in "The first year of HST observations",

Eds A.L. Kinney and J.C. Blades,

(Space Telescope Institute, Baltimore, 1991) p. 83

2 A.G. Shenstone and W.F. Meggers, 1958, J.Res.NBS 61, 373

3 K.G. Kessler. 1959, J.Res.NBS 63A. 213
Diagnostics of Electron Temperature and Density in High Density Plasmas

Using L-shell Xenon Emission Spectroscopy

C.J. Keane, B.A. Hammel, A.L. Osterheld, D.R. Kania

Lawrence Livermore National Laboratory

K- and L-shell x-ray spectra have long been of use in diagnosing the fuel

conditions in both directly and indirectly driven ICF targets.! To date, spectral

diagnosis of the fuel region of capsules indirectly imploded using the Nova laser

has relied on K-shell emission from H- and He-like Ar.2 K-shell Ar emission is used to diagnose the fuel region through Stark broadening of the Ar Ly-p and

He-p lines (which gives fuel Nq) and the ratio of Ly-p to He-p (which gives fuel

Te). In these experiments Arand Xe are placed as dopants in the deuterium fuel

at the 0.02-0.1 atomic percent level. Typical fuel plasma conditions in current

implosions inferred from Ar line emission are Ne~1024 cm-3 and Te~l-2 keV; the

latter depends strongly on laser energy.

While K-shell Ar emission has been of valuable diagnostic use in implosions to

date, future implosion experiments are expected to achieve pusher opacities high

enough to prevent Ar emission from escaping the capsule. The consequent need

for higher photon energy diagnostics has motivated our work in developing Lshell Xe emission as a measure of electron temperature and density. Previous

work^ with Xe in direct drive implosions showed emission from ionization stages near Ne-like; a number of F-like transitions included in the model used here were

identified. Using a state of the art Xe modeH of the type originally developed for

Ne-like ion x-ray laser research, we have developed spectral diagnostics of

electron temperature and density based on ratios of clusters of Xe lines.^These

methods require spectrographs with relatively low (-500) spectral resolving

power. Specifically, ratios of F-hke resonance lines and Ne-like satellites to Nelike resonance lines and Na- and Mg- like satellites are found to be temperature

and density sensitive. The temperature and density sensitivity reflects the

changing ionization balance with plasma conditions. Experimental Xe spectra

from Nova indirect drive implosions are in good qualitative agreement with

calculated spectra; inclusion of spatial gradients in temperature and density is necessary before a full comparison with measurement can be made. Finally,

pressure broadening of Xe 4-2 transitions also appears feasible as a electron

density diagnostic for Ne~1025 cm"3.6 it is necessary to include ion motion effects

here; this is in progress.

References

1. R.L. Kauffman, "X-ray Radiation from Laser Plasma", in Handbook of Plasma

Physics, Vol. 3: Physics of Laser Plasma, A. Rubenchik and S. Witkowski, eds..

North Holland Publishing Co., 199L

134
C. J. Keane et al. 135

2. B.A. Hammel, C.J. Keane, D.R. Kania, J.D. Kilkenny, R.W. Lee, R. Pasha, and

R.E. Turner, to be published in Rev. Sci. Inst. 3 Y. Conturie, B. Yaakobi, U. Feldman, G.A. Doschek, and R.D. Cowan, J. Opt.

Soc. Am. BZL 1309 (1981).

4. A.L. Osterheld, B.K.F. Young, R.S. Walling, W.H. Goldstein, J.H. Scofield, M.

Chen, G. Shimkaveg, M. Carter, R. Shepherd, B.J. MacGowan, L. DaSilva, D.

Matthews, S. Maxon, R. London, and R.E. Stewart, in Proceedings of the 3rd

International Colloquium on X-ray Lasers, Schliersee, Germany, May 1992.

5. C.J. Keane, B.A. Hammel, A.L. Osterheld, and D.R. Kania, to be submitted for

publication.

6. C.J. Keane, R.W. Lee, B.A. Hammel, A.L. Osterheld, L.J. Suter, A. Calisti, F. Khelfaoui, R. Stamm, and B. Talin, Rev. Sci. Inst. ^

2780 (1990).

Acknowledgment

Work performed under the auspices of the U.S. Department of Energy by

Lawrence Livermore National Laboratory under contract No. W-7405-ENG-48.
120-keV Kr^" - Li collisions

studied by near UV and visible photon spectroscopy.

E. Jacquet*, P. Boduch*, M. Chantepie*, M. Dmetta"^, D. Hennecan", X. Husson",

D. Lecler*, N. Stolterfoht* \ M. Wilson?

• Laboratoire de spectroscopie atomi que CNRS-Ufi4 19

ISXIRA Bd Marechal Jiiin F- J 4050 CAEN CEDEX FR.4\CE

ir Laboratoire de iraiteitient du signal et instrumentation CSRS-UFLA 842. Universite de Saint-Etienne

23 rue du Docteur Paul .\ lichelon F-42023 SA1\'T-ET1ESNE CEDEX, FRANCE

t Hahn-.Vfeitner Institut. Gleinicker Strasse 100. D- 1 000 Berlin 39. GE}l\L4M'

I Department ofPhysics. Royal Holloway and Bedford New College

University ofLondon. Egham Hill. Eghani. Surrey T\V20 OEX. ENGLAND

Introduction.

Collisions of multiply charged ions on a neutral atomic or molecular target produce ex'cited

multiply charged ions following the reaction:

Aq+ + B -* A(q-'^)^ + B^^ + AE

when k is the number of electrons which have been captured.

It has already been shown that near UV and visible photon spectroscopy is a convenient

tool [1] to observe charge exchange collisions. Following previous work (Kr^"^ - He, Hi [2], .Ar^"*"

- Li [3]), we present results for collisions between Kr^"^ ions and lithium atoms at 120 keV The

three electrons lithium target allows us to study single, double and triple electron captures The

outermost 2s electron of the lithium target is very loosely bound and population of relatively high

Rydberg states is therefore expected in Kr VIII. The 2s and one or two Is electrons are transferred dunng double and triple electron captures. The relative population of the outgoing

channels allow an estimates of the importance of correlation effects (electron-electron interactions)

in the exchange process.

After a description of the experimental set-up, we present a detailed spectroscopic analysis

of the recorded spectra. The analysis was made using collisional models (Niehaus [4], LandauZener [5] and Stolterfoht [6]) and spectroscopic ab initio pseudo-relativistic Hartree-Fock (HFR)

calculation (Cowan [7]).

Experimental set-up.

120-keV Kr^"*" incident ion beam provided by an ECR source of the GANIL test bench is focused on an efHisive jet of lithium. The ion beam current was of the order of 20 ^A, the pressure

in the collision chamber of the order of 10"^ mbar. The emitted photons were observed at nght

angles to the directions of the incident beam and of the lithium jet with a normal grating incidence

spectrometer.

136
E. Jacquet et al. 137

240.0 260.0 280.0 400.0 420.0

wavelength in the 2nd order Spectral analysis. (nm)

Single electron capture lines.

The classical over-barrier model of Niehaus [5] predicts that the 2s electron of the

target is preferentially captured into a n=9 orbital. Lines corresponding to An=0, An=l and An=2

transitions are expected to be observed in the 200-600 nm wavelength range. Observed transitions are presented in Table I. Double electron capture lines.

Observed lines corresponding to 4snl - 4snT Rydberg transitions are indicated in Table IL The 4snl configurations in Kr VII are produced by a one-step process involving electronelectron interaction.

Triple electron capture lines.

We observed two lines corresponding to 4s^6h - 4s27i and 4s^6g - 4s27h

transitions.

4s26g-4s27h X=338.17 nm

4s26h - 4s-7i X=339.47 nm

1 P. Boduch, M. Chantepie. M. Druetta, B. FawcetL D. Hennecart, X. Husson, H. Kucal, D. Lecler, N. Stolterfoht,

M. Wilson. Physica Scnpta, 45, 203 (1992).

2 P. Boduch, M. Chantepie, M. Druetta, D. Hennecart, X. Husson, D. Lecler. M. Wilson, Physica Scripta, to be

published (1992).

3 E. Jacquet, P. Boduch, M. Chantepie. M. Druetta. D. Hennecart, X. Husson, D; Lecler, N. Stolterfoht, M. Wilson,

Physica Scnpta, submined (1992). A. Niehaus, J. Phys. B: At. Mol. Phys., 19, 2925 (1986).

^ E.E. Nikitin, Theory of elementary Atomic and Molectilar Processes in Gases, Clarendon Press, O.xford (1974).

6 N. Stolterfoht, K. Sommer, J.K. Swenson, C.C. Haveneur, F.W. Meyer, Physical Review A, 42, 5396 (1990). 7 R.D. Cowan, The Theory of Atomic Structure and Spectra, University of California Press, Berkeley (1981).
138

1 Transitions

in Kr Vin

.J- (rim)

in air Sf^F,,, -6d 'D^,

5f-F ' - 6d -D,'

227,65

225.93

6d 2D,,, - 7p 2p,^^

6d 2D<,^ - 7d 2?,

,

229.22

225.64

6f 2F<^ - 7d 2D,.,

6f2F,,,-7d 2D5,,

375.90

372.74

6g-7f 191,61

6h - 7i 192.84

j

7p 2?,^ - 8s 2S,,, 229.57

7d 2D,,, - 8p 2?,^^

7d 2D,^ - 8p 2?,^

7d 2D5,^ - 8p 2P,,^

377.07

367.78

370.29

7f - 8e

269.62

or i 269.80

7g-8f 318,94

7g-8h 294,92

7h-8i 297,04

7i - 8k 297.35

8p 2p,^.9s2S,„

8d 2p,„ . 9s 2S ^

350.62

359 00

8d 2D - 9f 2F

8d 2D5^-9f2F,^

241 83

8f-9g 392.92

8g-9h 429.95

8h-9i 433.27

81 -9k 433.77

8k -91 433.81

6s 2S,^ - 6p.2p,^ 355 88

6s2S,,, -6p 2p,,^ 333.74

6p 2P,^ . 6d 2D,,, 206.87

6p 2P,^ - 6d 2D,^ 215.23

6p 2P,^-6d 20,^ 213.78

i 6d 2D,o - 6f 2F<« 99 1 99

6d2D5^-6f2F,^

1 mil

7s 2S,^ - 7p 2p,^ 584.88

7p 2P,^ - 7d 2D,^ 356,08

7p 2?,^ - 7d 2D,^ 370.07

7p 2P,^ . 7d 2D5^ 367.53

7d2D,^-7f2F3^ 368,41

7d 2D5^-7f2F5.^ 371.05

7d 2D5^ - 7f 2F,,, 371.27

9k- 101 605.63

Ql - 1 Om UvO.JO

8i- 10k 252.78

1 oK. - 1 UI

9k- 111 348.35

91 - 11m 348.69

10m -12n 466.79

Table \.

1 Transition exn^ (nm)

inKr Vn

1 4s6g - 4s7h 249.44

1 4s6h- 4s7i 249.63

4s7g - 4s8h 382.20

4s7h - 4s8i 382.99

4s7i - 4s8k 387.28

4s8i - 4s9k

j 4s8k - 4s91 565.88

j Table n
Photon and Auger Spectroscopy of Single and Double Electron

Capture following 90-keV C^^ - Li Collisions

F.Fremont, E.Jacquet, P.Boduch, M.Chantepie, G.Cremer, D.Hennecart, S.Hicham, X.Husson,

D.Lecler and N.Stolterfoht ^ Laboratoire cie spectroscopie atonuque. 1SMR.A, bd du A/arechai Juin. 14050 CAEN

M.Druetta

Laboratoire de Iraitement du signal et instrumentation CNRS-URA 8-(2, Universite de Samt-Etienne

23 rue du Docteur Paul Michelon F-4202S S.A1NT-ETIENNE CEDEX. FR.ANCE

M.Wilson

Royal HolloM'ay and Bedford New College, Department ofPhysics, University ofLondon, Egham Hill, Egham,

Surrey TW20 0E\, LONDON, ENGLAND.

The system 90-k:eV C^"*" - Li has been studied recently using an ECR ion source of the

GANIL*. Lithium is an interesting target because it has three active electrons. The single electron

capture of the outermost 2s electron, which is loosely bound produces configurations nl (n=7, 8)

in C^"''. The states of these configurations are radiative states which give rise to photon emission in the visible and near UV wavelength range. Double electron capture is expected to produce 2121',

21nl' (n=4, 5...) in C"^^ (Figure 1) by the electron nucleus interaction and 2131', 2141', 3131' by the

electron nucleus interaction (Figure 2) and the electron-electron interaction (correlated transfer

capture). Most of the states of these configurations are autoionizing states and give rise to electron emission by Auger effects.

Single electron capture

The observed spectra in the 250-600 nm wavelength range is presented in Figure 3. According to the theoretical predictions, nl (n=7, 8) configurations in C^" are produced. The

experimental wavelengths and the emission cross sections are given below.

Transitions Experimental wavelengths Emission cross sections

(10-17 cm2)

n=7 n=6 343.49 ± 0.04 nm 50

n=8 ^ n-7 529.21 ± 0.04 nm 9

n-9 -> n=7 313.88 ± 0.04 nm 1.7

n=10 n=8 450.00 ± 0.04 nm 0.3

Double electron capture

Photon spectroscopy

We observed lines corresponding to ls5g - ls6h and ls6h - ls7i or to 2p5g - 2p6h

and 2p6h - 2p7i 'l transitions. We cannot observe 2s5g - 2s6h and 2s6h - 2s7i transitions

because 2s6h and 2s7i are autoionizing states. Is5g - ls6h and ls6h - ls7i transitions can correspond to the second step of radiative de-excitation.

^ also Hahn-Meitner-Institut Berlin GmbH, Glienickerstr. 100 Berlin 39

* Grand Accelerateur National d'lons Lourds, Caen, France. 139
140

Auger spectroscopy

As seen from the spectaim (Figure 4), we actually observed the expected configurations,

but we also observed un-expected configurations Between 0 and 20 eV, we can see 41nl' configurations which were not expected. First, we thought that double collisions can contaminate

the real double capture, but an estimate of the jet pressure excludes this possibility. No explanation can be given yet. We have a similar problem with 2121' configurations, which caji come from

double collisions as well as double capture.

In the range [20-80eV], we find 31nr (n=3,4,5) configurations. However, for a given

intensity of the peaks corresponding to 3131' and 3151' configurations, the 3141' configurations

intensity changes strongly with the pressure.

Between 300 and 380eV, we observed 21nr configurations. As expected, the peaks

corresponding to 2131' and 2141' configurations are weak. The biggest peak corresponds to 2151'

states.

10 100

Internuclear distance (a.u

10 100

Internuclear distance (a.u.)

•5'ure. -2.
F. Fremont et al. 141

100 -

0

>- 300

1:1

c'

caa

CO

o

egCOn

312 324 336 348

wavelength in the 2nd order (nm)

360

200 -

(Ow

C)

tn

JO

CM

00Gl

I.. 100 412 424 436 448 460

Bectron Energy (eV)
Measurements of Electron Emission From

Collisions of MeV Energy N, C, and He Ions

With He Gas

N. A. Guardala, J .L. Price, and D. J. Land

Naval Surface Warfare Center/White Oak, Silver Spring MD

M. F. Stumborg and D. G. Simons

The Catholic University of America

G. A. Glass

University of Southwestern Louisiana

1 . Introduction

Experiments involving collisions between neutral gas targets

and ion-beams produced by positive-ion accelerators have become a useful means of gathering information pertinent to the modeling and

understanding of both astrophysical and laboratory plasmas [1].

Typical experiments may involve emergent projectile charge state

distributions, energy loss and various spectroscopic measurements

of both target and projectile excited states. Measurements of the

electron emission spectra produced in collisions of energetic

projectiles with relatively simple targets such as: H, and He

gas have become a powerful tool in the study of the dynamics of

ion-atom collisions [ 2 ]

This brief paper reports on measurements of electron emission

spanning kinetic energies typically from 200-3000 eV and involving

projectile energies that range from 0.2 0-1.4 0 MeV/u. Two types of

emitted electrons are almost always observed regardless of the

charge state and velocity of the projectile, these are: "cusp"

electrons [3] which involve electrons moving with zero velocity in

the projectile's reference frame and therefore have the same

velocity in the laboratory frame as the projectile and Binary

Encounter electrons [4] which originate from bound target electron

states. The cusp electron peak can be due to either capture of a

target electron to a Rydberg-like state of the projectile, this

process is referred to as Electron Capture to the Continuum (ECC)

or to the excitation of a projectile bound electron to a similar

excited state. This later process is known as Electron Loss to the

Continuum or ELC.

A third kind of electron transition is possible when the

projectile is capable of forming a Li-like i.e. a three electron

excited-state configuration, that excited state will have some

probability of decaying via the Auger emission process. Typically,

this excited state involves a K-shell vacancy so that the emitted

electron represents some type of K-shell Auger transition. Figure

1 shows an ejected electron spectrum involving 0.92 MeV/u C*^ ions

colliding with He gas. Cusp, KLL, KLM and Binary Encounter

electrons are clearly identifiable.

2 . Experimental

142
N, A. Guardala et al. 143

In order to measure discrete transitions such as Auger lines

and cusp electrons without significant Doppler broadening this

series of electron measurements were carried out at 0° with respect

to the beam axis [5]. Therefore, the peaks have observed widths

that are determined primarily by the instrumental resolution which

is ca. 2 % . The measurements were carried out using the 3 MeV Tandem

Pelletron at the Naval Surface Warfare Center/White Oak Lab. Beams

of N""^, C*^, He*^ and He*^ were produced from the accelerator and were

mass, charge and energy analyzed magnetically before being focused

through the target interaction chamber. This chamber contained a gas jet which allowed pressures of 1-4 torr to be maintained in the

jet with a background chamber pressure of typically 2 x 10'^ torr.

The electrons were energy analyzed using a double-focusing,

hemispherical electrostatic analyzer coupled to a channeltron

electron detector [6]. The gas jet was positioned at a distance from

the entrance to the analyser which approximated the entrance focal

point. Integrated beam currents were collected in a Faraday cup.

3 . Conclusion

Measurements of ejected electron spectra involving MeV energy

projectiles and neutral He gas have begun at NSWC/White Oak. These

measurements are preliminary to a proposed collaboration between

NSWC and the University of Maryland's Laboratory for Plasma Physics

to perform similar measurements which will substitute a laboratory

generated plasma target for a neutral gas target. The scientists at

NSWC/WO acknowledge the Independent Research Fund of the U. S. Navy

in supporting this work.

References

[1]. G. Hoffmann, A. Muller, K. Tinschert and E. Salzborn, Z. Phys.

D 16, 113 (1990)

o

[2]. K. Tinschert, A. Muller, G. Hoffmann, E. Salsborn and S. M.

Younger, Phys. ReV A 40, (1991).

[3]. R. Shakeshaft and L. Spruch, Phys. Rev. A 20, 367 (1978).

[4]. D. H. Lee, P Richard, T. J. M. Zouros, J. M. Sanders J. L.

Shinpaugh and H. Hidmi, Phys. Rev. A 41, 816 (1990).

[5]. A. Itoh, D.Schneider, T.Schneider, T. J. M. Zouros, G. Nolte,

G. Schwieitz, Z. Zeitz and N. Stolterfoht, Phys. Rev. A 31,

684 (1985) .

[6]. K.D. Sevier. Low Enerav Electron Spectrometry , Wiley, New York

1972 .
144

(BpUDBnOL|_L)

SlNflOO
UPDATE ON THE NIST EBIT

J.D. Giliaspy* and J.R. Roberts

National Institute of Standards and Technology

Atomic Physics Division, Gaithersburg, MD 20899

and

CM. Brown and U. Feldman

E. O. Hulburt Center for Space Research

Naval Research Laboratory, Washington, D. C. 20375

I. Introduction to EBIT.

A decade ago, the Electron Beam Ion Source (EBIS) was hailed as the most

advanced method for producing highly charged ions [1]. A few years later, the

EBIS concept was reevaluated and optimized for use as a spectroscopic source. The new device, the Electron Beam Ion Trap (EBIT) [2], produced a high density

of ions in a relatively small volume with radial access ports. With this new

geometry, plasma instabilities were removed and very high electron beam densities

were achieved. These improvements boosted both the spectral brightness and the

maximum attainable charge state, and furnished the atomic spectroscopy

community with an important new laboratory source. The spectra produced with an EBIT are very pure, consisting of lines from

only a few charge states of essentially a single atomic species. The choice of

charge state can be continuously varied by adjusting the electron beam energy.

The ability to literally "dial up" a particular charge state greatly simplifies the

identification of spectral lines. Virtually any highly charged state of any atom on

the periodic table is accessible in this way.

in addition to operating the EBIT in a static mode where the electron beam

energy is held constant and a spectrum is collected in order to determine accurate

wavelengths, one can also use the precise and rapid control of the electron beam

energy to carry out temporal studies of the emitted photons. This feature allows

one to directly determine excited state lifetimes and to map out dielectronic

recombination cross-sections.

A summary of the advantages of EBIT over conventional sources include:

1. Relatively few charge states.

2. No Doppler shifts

3. Insignificant Doppler broadening.

4. Insignificant density effects.

5. Very high charge states attainable.

6. Control over dielectronic satellites.

7. Slit-like source dimensions (60 um x 2 cm) ideally

suited to spectrometers.

8. Very little background signal.

145
146

9. High accuracy (21 ppm) wavelength measurements

demonstrated.

10. Ultrahigh vacuum (10'^° Pa) maintained by cryogenic

environment.

1 1 . No cascade contamination in lifetime studies.

Although the spectral brightness of an EBIT is much weaker than that from

powerful sources such as Tokamaks, the photon flux from an EBIT is nevertheless

quite adequate for spectroscopic work when reasonable effort is taken to make

use of efficient modern detection methods. A typical x-ray spectrum recorded with

a solid state detector on an EBIT may only take a few seconds to collect. Very

high precision studies of weak lines using crystal detectors may require many

hours of data collection, however. Even in such cases the brightness is not

usually of overriding concern since the source is under local control and operates

reliably for long periods of time. Because the source is run by computer control,

ions can be dumped from the trap and reloaded automatically at periodic intervals.

II. Present status of superconducting EBIT facilities.

The only full-scale EBIT devices in operation at this time are those at Livermore. The mechanical components for the NIST EBIT were made in Oxford

England where an identical device is being put into operation [3]. The NIST EBIT

will go into operation in Gaithersburg, Maryland during the coming year through

a collaborative effort with the Naval Research Laboratory. An EBIT project is reportedly underway in Japan, although information about this project is scarce. A major EBIT project has been underway in the former Soviet Union at Dubna."*

Charge states as high as fully stripped Uranium are being actively pursued

at Livermore where the prototype EBIT has been upgraded to operate above 150

keV. The NIST EBIT will begin operations under 50 keV, with possible upgrades

in the future. Even at 50 keV, most of the states of any ion can be accessed.

The design of the NIST EBIT was developed by M. Levine and is based on

his highly successful original work with the Livermore prototype. Detailed

drawings, a discussion of the improvements that have been made, and a table of

the projected operating conditions will be published in the proceedings of the Vlth

International Conference on the Physics of Highly-Charged Ions (HCI-92).

*Bitnet: Gillaspy@NBSenh, Internet: Gillaspy@enh.NIST.gov

[1]. H. Winter, "The Production of Multiply Charged Ions for Atomic Physics

Experiments" in Atomic Physics of Highly Charged Ions, R. Marrus (Ed.),

1983.
J. D. Gillaspy et al. 147

M.A. Levine, R.E. Marrs, J.R. Henderson, D.A. Knapp, and M.B. Schneider,

"The Electron Beam Ion Trap: A New Instrument for Atomic Physics

Measurements," Phys. Scr., T22, 157 (1988).

J. Silver, private communication.

Y. Aglitskiy, private communication.
PERFORMANCE AND RESOLVING POWER OF CONCAVE MULTILAYER-COATED GRATINGS

OPERATING NEAR NORMAL INCIDENCE IN THE 136-300 A REGION

J. F. Seelyl m. P. Kowalski} W. R. Hunter? J. C. Rife} T. W. Barbee, Jr.? G. E. Holland? C. N. Boyerf and C. M. Brownl

iNaval Research Laboratory, Washington DC 20375

2SFA Inc, 1401 McCormick Drive, Landover MD 20785

^Lawrence Livermore National Laboratory, Livermore CA 94550.

^USRA, 409 Third Street SW, Washington, DC 20024

Owing to the low reflectance of

materials for wavelengths below 300 A

and near normal incidence, most grating

spectrometers operate at grazing

incidence in the XUV and soft X-ray

regions. These instruments typically

have low throughput because of the small

geometrical collection factor and tend

to be costly and difficult to focus.

Newly-developed multilayer coatings,

that have high reflectance below 300 A,

have opened the possibility of building

high-throughput spectrometers that

operate near normal incidence. The

multilayer coating can be matched to the

blaze angle of the grating substrate so that the grating operates on-blaze in

wavebands of spectroscopic interest with

an efficiency that can be orders of

magnitude higher than that of a similar

gold-coated grating. These are important advantages for instruments

intended to observe weak sources such as EBIT.

Multilayer coatings were applied to

two sister replica grating substrates

that were made from a ruled master by

Hyperfine Inc. The grating substrates

were concave with 2.2 meter radius of

curvature, had 2400 g/mm, and nominal

blaze angle of 2°. The multilayer

coatings were sputter deposited at the

Lawrence Livermore National Laboratory

and consisted of alternating layers of

Mo and Si. Witness optical flats were

coated simultaneously with each grating

substrate. The reflectances of the

witness flats and the efficiencies of

the multilayer-coated gratings were

measured using the NRL ref lectometermonochromator at the National

WAVELENGTH (A)

148
J. F. Seely et al. 149

Synchrotron Light Source. The resolving

powers of the gratings were determined

by mounting the gratings in a 2.2 meter

McPherson normal -incidence spectrograph.

Similar measurements were made using a sister replica grating that had a gold

coating.

Multilayer grating #1 had 30 Mo/Si

periods with a d-spacing of 162.5 A.

The multilayer coating was designed to

have high reflectance in both the first

and second Bragg orders. As shown in

Fig. 1(a), the reflectance of the

witness flat measured at an angle of

incidence of 20° was 24% at a wavelength

of 290 A and in the first multilayer

order (n=l) and 33% at 148 A in the

second multilayer order (n=2) . The

calculated reflectances of the witness

flat at 20° and 4° angles of incidence

are shown by the solid and dashed curves

in Fig. 1(b), respectively, and this

illustrates how the reflectance

wavebands shift with angle of incidence.

For comparison, the normal -incidence

reflectance of a gold coating is shown

by the dot-dashed curved in Fig. 1(b).

The measured efficiencies of the

multilayer and gold gratings are shown

in Fig. 1(c) for an angle of incidence

of 14.5° and in the first outside

grating order. The peak efficiencies

were 2.5% and 1.5% at wavelengths of 290

A and 151 A. These efficiencies were

factors of 4 and 200 greater than the

corresponding efficiencies of the gold

grating.

The multilayer coating for grating #2 was designed so that the grating would

operate on-blaze with high efficiency in

the second grating order and at a wavelength of 140 A at normal incidence.

The multilayer coating was composed of

40 Mo/Si periods with a d-spacing of 73

A. The reflectance of the witness flat was 55% near normal incidence. For an angle of incidence of 14.5°, the grating

efficiency in the second outside order

was highest for a wavelength of 136 A, as shown in Fig. 2, and the efficiency

of the multilayer grating was a factor

or 150 higher than that of the gold

grating. Figure 3 shows ine efficiency

in the outside orders at a wavelength of

136 A and at 14.5° incidence, and the

>-o

-z. UJu

10

1

0.1

o 0.01

<

130 134 138 142

WAVELENGTH (A)

Figure 2

10

IS

>- 1 o

z

UJ 0.1

o

u_

Li_ 0.01

UJo

0.001 1—

<

O

: 1 1 11 -2

1

I 1

^ -1 ^

-3 1

E Mo/Si \*^-4 :

: -2

r . -3 I

r i/ 1 -4 :

1 iro\ 1 1 1 i«

"

10 12 14 16 18 20 22 24

DIFFRACTION ANGLE (deg)

Figure 3

145

140

X

1—

o 135

Ui

_j

UJ> 130 <

125

0 5 10 15 20 25 30

ANGLE (deg)

Figure 4
150

efficiency is highest in the second

order.

Figure 4 illustrates how the

wavelength of peak reflectance of the

witness flat (squares) and peak

efficiency of the grating (diamond and

triangles) vary with angle of incidence.

The McPherson spectrograph operated

with an angle of incidence of 6° and a 20 /im entrance slit. The spectra from a vacuum spark source were recorded on Kodak 101 plates. The higher grating

orders were observed by using a 1 /^m

beryllium filter to attenuate the longer

wavelength radiation. The transmi ttance

of the filter is shown in Fig. 5(a), and

the spectra recorded from a tungsten

electrode without and with the filter

are shown in Figs. 5(b) and (c)

,

respectively. The first, second, and

third grating orders are clearly visible

in Fig. 5(c) at wavelengths near 140 A,

280 A, and 420 A. The periodic

structure on the long wavelength side of

the orders results from the

periodicities in the off-peak

reflectance of the multilayer coating.

The resolving power of nulti layer

grating #1 is illustrated in Fig. 6.

This is the second-Bragg -order spectrum

of a vanadium electrode ir the first,

second, and third grating orders. Using

the V VII transition at lij6.608 A, the

resolving power is 14,000 after removing

the broadening caused by the 20 urn entrance slit. Comparisons between the

multilayer and gold gratings indicated

that the application of the multilayer

coating did not affect resolving power.

100 200 300 400 500

Figure 5 WAVELENGTH (A)

24

CO 'E

o

>-

18 _

12

0

(a)

m=l

A^^^V^^ ..^.|/>^N/V^

(b)

30

+ 20

10

m=2

155 156 157 158

Figure 6

312 314 316

WAVELENGTH (A)

468 471 474 477
New line identifications in XeVIII and XeVII

M. DRUETTA

Laboratoire de Traitement du Signal et Instrumentation

URA CNRS 842

Universite Jean Monnet, 42023 SAINT-ETIENNE Cedex, France

D. HITZ, P. LUDWIG

DRFMC/PSI Centre d'Etudes Nucleaires de Grenoble

85X 38041 GRENOBLE Cedex, FRANCE

ABSTRACT

XeVIII and VU spectra have been observed in the 30 - 90 nnn spectral region by

charge exchange collision. New lines are identified.

Introduction

Charge exchange collision spectroscopy between multicharged ions and

neutrals is a good technique to obtain new spectra ^ of these multicharged

ions. The particularity of this excitation, is suitable for line identification :

- selectivity of the capture and possible prediction of the populated nl

sublevels 2/^'

- possible discrimination between one and two electron capture by the

maximum level n excitated, or with double collision by pressure variation , - variation the selective n level excitated by change of the target (ionisation

potential).

We present here our preliminary results on XeVIII and XeVII obtained by this

method.

Xe 8+/ 7+ ions produced by a 10 GHz E.C.R. ion source at an energy of 160 - 140

kev, are sent after magnetic selection, in a charge exchange chamber filled with

He or H2 . A 3m - VUV grazing incidence spectrometer equipped with a 300

lines/mm grating blazed at 51.2 nm and a channel electron multiplier, analyse

the light emitted at 90° of the incident ion beam.

Results and discussion

For line identification we have used the results obtained in a theta pinch plasma

or by beam foil spectroscopy 6'^. In XeVIII we have observed the already classified 5s - 5p, 5p - 6s, 5p - 5d, 5d -

5f, 4f - 5g transitions. New observed lines (Table I) are identified as the 5d - 6f,

151
152

5f - 5g and 6p - 7s transitions. These measurements permit to deduce the energy

of the 6f and 6g levels in XeVm respectively to 593910 cm'^ and 656850 cm"^.

In XeVII the known 5p-^P°- Sd^D, 5p3p° - 6s^S transitions are observed. We

have also observed the X. 81.6 - 79.8 - 73.7 - 72.3 nm components of the 5s5p3p° - 5p^ multiplet. But we did not observe the X 71 A nm line and a weak line

may be the X 66.0 nn line.The line observed at X 82.8nm6 is the second order of

the X 41.47nm component of the5p 3p° - 6s3s transition.

In the singlet system of XeVII only the X 69.81 nm 5s - 5p transition is known.

The two lines at X 45.77 and 60.80 nm observed both during the collisions of

Xe^+ and Xe''^ with He or H2 are identified as XeVII lines. In the collisions of

XeS+ a two electron capture process is involved with spin conservation.

Predictions with the MCDF code^ show that the X 45.77nm line may be

identified as the 5p^P - 6s^S transition and the X 60.80 nm line may be the 5d^D - 5f transition instead of the 5p - 5d transition which is blend with the 5s - 5p

transition.

XeVIII

Table I New lines in XeVIH and VII

X (nm) ± 0.05 identification

35.21 5d2D5/2-6f 2f°7/2

35.57 5d2D3/2-6f 2F°5/2

62.86 5f V- 6g2G

82.00 6p2P°|/2-7s2Si/2

87.30 6p2P°3/2- 7s2Si/2

XeVII

45.77

60.80

5p IPi - 6s ^So

5d^D2-5f IF3
M. Druetta et al. 153

60.80

56.6

I,

XeVII

45.77

—\—

r

1—

r

53.1

52.2

V

VI

Jl

u

1—i—

r

( I 1 r

Part of the Xe7+ + He spectrum

References

1 M. Druetta, S.. Martin and J. Desesquelles

Nucl. Instrur. Meth B23, (1987), 268

2 A. Niehauss Phys. B 19, (1986), 2929

3 J. Burgdorfer, R. Morgenstern and A. Niehauss Phys B 19, (1986), L507

4 J.R. Roberts, E.J. Knystautas and S. Sugar J. opt. Soc. Am. 69, (1979), 1620

5 E.J. Knystautas, S. Sugar and J.R. Roberts J. opt. Soc. Am. 69, (1979), 1726

6 J.A. Kernahan, E.H. Pinnigton, J.A. O'Neill, J.L. Bahr and K.E. Donnelly

J. opt Soc. Am 70, (1980), 1126

7 S. Bashkin, R. Hallin, J. Leavitt, V. Litzenard and D. Walker

Phys. Scipta 23, (1981), 5

8 J.P. Desclaux Comp. Phys. Comm. 2, (1975), 31
Transition element spectra by high resolution Fourier transform

spectrometry

Jon. E. Murray*, J. Pickering, G. Nave+, R. C. M. Learner & A. P. Thorne

BlackeU Laboratory, Imperial College, London SW7 2BZ

[* now at Harvard-Smithsonian Center for Astrophysics, Cambridge MA 02138)

('^ now at Lund university, Department of Physics, Solvegatan I4, Lund Sweden)

Introduction

The needs of astrophysicists for new and improved atomic data have been emphasised in the

previous meetings in this series and in many published papers. High resolution Fourier transform

spectroscopy (FTS) is making an important contribution to both the accuracy and the completeness

of the spectra of neutral and singly ionised atoms over a wavelength range that has now been

extended from the near infra-red to 180 nm in the VUV.

The FTS advantages of linear (~ 1 : 10^) wavenumber scale, high resolution, and good light

throughput combine to offer accurate wavenumbers (0.001 cm~^ for strong lines), with quantifiable

errors, and the ability to make observations on weak lines and to resolve hyperfine structure. At

Imperial College, in association also with the National Solar Observatory and Lund University,

work has been proceeding on the astrophysically important transition element spectra. This paper

describes the current status of this work.

The existing data base

The need for reliable f- values is well known. What is more surprising is the age and uncertainty

of much of the wavelength data. Many spectra have not been measured since the pubhcation of

the Revised Multiplet Tables [1] in 1952. Moreover, closer examination of these tables reveals that

they are in many cases a republication of very much earlier values, some of them obtained before

1910 - see, e.g., [2]. The uncertainties associated with the published wavelengths are rarely known,

and many weak lines are missing.

The inadequacy of the data base has been highlighted by the results from the Hubble Space

Telescope. In order to model the recorded spectra, data on weak lines of abundant elements and

on isotope shifts and hyperfine structure are aU required, in addition to more accurate wavelengths

and f- values - see, e.g., [3].

Experimental

The spectra have been recorded on a Fourier transform spectrometer covering the range from

about 900 nm to 180 nm, using either the prototype instrument developed at Imperial College [4] or the commercial version of it made by Chelsea Instruments. The maximum spectral resolution,

0.025 cm~^, is sufficient to resolve fully the hues from the hollow cathode lamp used to excite the

spectra. This lamp was run at currents up to 750 mA with carrier gas pressures of a few torr of Ne

or Ar. Fig.l shows examples from the Cr & Co spectra.

Wavenumber accuracy

The transformed and phase-corrected spectra were analysed by the DECOMP program developed by J.W.Brault, which allows a Voigt profile to be least-squares fitted to each line. The

precision with which the centre of a symmetric line can be determined is given by its width divided

by twice its signal-to-noise ratio. The high resolution ensures that the line width is actually the

Doppler width, while the high hght throughput maximises signal- to-noise ratio. The fact that the

noise in our instrument is almost independent of wavenumber allows a quantitative value to be set on precision for each line. Although the FTS wavenumber scale is accurately linear to within the stability of the monitoring

laser (better than 1 : 10^), the absolute scale must be obtained from one or more standards (which

do NOT need to be distributed through the spectral range as in grating spectrometry). A set of blue

Ar II lines measured by Norlen [5] has been used to calibrate strong Fe lines in the same spectral

154
Jon. E. Murray et al. 155

region, and the calibration has then been extended to both longer and shorter wavelengths by means

of overlapping spectral regions. The procedure is fully described in three papers on recommended

iron standards [6,7,8]. The calibration is accurate to a few parts in 10^, corresponding to 0.001

cm~^ in the visible and 0.002 cm~^ in the UV. A stainless steel hollow cathode has been used to put strong lines of Cr and Ni on the same scale as the Fe.

Current state of work

Fe I and Fe II The combination of our measurements with those taken in the IR at NSO with a similar source has resulted in a set of about 29,000 hues over the range 5.5f.im. to 180 nm, some 11,500 of which

are still unassigned transitions. Compared with previous measurements, the number of lines in

increased by a factor of about 5 and the wavenumber accuracy is in general improved by an order

of magnitude. Work on assignment is in progress in collaboration with S.Johansson, and a revised

multiplet table for Fe I is in preparation. The assignment of the high 4/ [9] and 5g (in progress)

states has particular relevance to solar observations. As mentioned above, three subsets of Fe I and

Fe II lines have been selected as recommended wavelength standards for the visible [6], UV [7] and

IR [8] respectively.

Cr I and Cr II About 10,000 Unes have been measured in the visible and UV a significant increase over previous

data (Fig.l). Some 40% of these new observations are unassigned. These measurements have

allowed us to revise over half of the currently known energy levels, 539 [10] , many of them derived

from more than 50 lines, with an uncertainty of 0.001 cm~^. There are significant differences from

the AEL levels [10], in some cases as much as 0.1 cm"-"^ (Fig. 2). A line list will shortly be submitted

for publication, and a revised multiplet table is in preparation.

Co I and Co II The visible and UV spectra have been recorded. Nearly aU lines show hyperfine structure, the

resolution of which is hmited by Doppler rather than instrumental width. The old data, pubHshed

in 1952 [1], are very incomplete and do not include hfs. For example in one 6 nm section centred on 232 nm we have measured 47 lines, of which 15 have resolved hfs and only 19 are included

in previous data. The level analysis will be done in collaboration with colleagues at Lund, and

meanwhile we are determining hfs splitting factors (Fig. 3).

Ti I and Ti II We have started to measure branching ratios in these spectra. These will be combined with

lifetimes measured by Lawler's group by laser techniques to give absolute f-values.

References

1. C. E.Moore, >ln Ultraviolet Multiplet Table, NBS Circular 488, 1952

2. R. CM.Learner, .J.Davies k. A.P.Thorne, Accurate wavelengths for the Th-Nd chronometer,

Mon.Not.R.Astr.Soc.248, 414-418, 1991

3. D.S.Leckrone et al., F^rsf resw/^s/rom /Ae G^i?5, Ap. J. 377, L37-40, 1991

4. A.P.Thorne et al., A Fourier transform spectrometer for the VUV, J.Phys.E 20, 54-60, 1987

5. G.'i^OTlen, Wavelengths and energy levels of Ar I and Ar II, Phys.Scr. 8, 249-268, 1973

6. R. CM.Learner & A.F.Thome, Wavelength calibration of FT emission spectra with applications to Fe I .LOpt.Soc.Am.B5,2045-59, 1988

7. G.Nave, R. CM.Learner, A.P.Thorne & .^&ms, Precision Fe I and Fe II wavelengths in the UV

.J.Opt.Soc.Am.BS, 2028-43, 1991

8. G.Nave, R.C.M. Learner, .J.E.Murray, A.P.Thorne & .J. W.Brault, Preczszon Fe / ari(/ /'e //
156

wavelengths in the IR, J.Phys.II 2, 913-929, 1992

9. S.Johansson & R. C. M.Learner, T/ie lowest 4f subconfiguration of Fe I, Ap.J.354, 755-762, 1990

10. J. Sugar &: C.Corliss, Atomic Energy Levels: K through Ni, J.Phys.Chem.Ref.Data 14, Supp.2, 1985

11. C.C.Kiess, Description and analysis of the first spectrum of chromium, J.Res.NBS.51, 247-305, 1953.

12. C.C.Kiess, Description and analysis of the second spectrum of chromium, J.Res.NBS.47, 385-426, 1951.

Acknowledgements

We would like to take this opportunity to thank the following for their help, advice or funding of this work.

The Science and Engineering Research Council, the National Solar Observatory (J. W. Brault), Mr Geoff

Cox of Imperial College and Dr Peter L. Smith at the Center for Astrophysics.

10»

1

<V2200 42220 42240 iaa

Wavenumber(cm~^ )

h

J-X

Fii

MOOXU t^K*TM ^Js^ -Ms^^ - Wavenuinber(cin~ )

a) 5 A section of chromium spectrum centered on 2367A. X marks those lines not seen in the work of Kiess [11][12]. b) 2. SA section of cobalt spectrum centered on 2206A.

The above intensities are arbitrary and plotted on a linear-log scale.

0.4

0.3

0.2

0.1

0

-0.1

-0.2

-0.3

-0.4 10CXJ0 20000 30000 40000 50000 60000 70000 4531i.59

Lev* energy (an-l

)

Fig. 2 Cr level energy difference between this work and AEL[10]

45312.8822 wavenimber c-l 45314.16

Fig 3. Excimple of fit to a Co D line with hfs.
Atomic Structure-theory

ATOMIC STRUCTURE IN ULTRASTRONG MAGNETIC FIELDS

E. P. LIEF and J. C. WEISHEIT

Space Physics k Astronomy Department, Rice University, Houston, TX 77251-1892, USA

Most previous studies of atoms in strong magnetic fields have been based on the assumption of a

spherically symmetric shape, despite qualitative predictions of more complicated form. This paper

presents equations for an approximate calculation of an axial charge density distribution in the Landau

regime.

1. INTRODUCTION

Discoveries of magnetic white dwarfs and neutron stars in astrophysics, as well as developments in the physics of condensed matter and laser produced plasmas emphasize the issue of atomic behavior in strong magnetic fields.^ Despite two decades' history of extensive work on the problem, most quantitative

approaches in the Landau regime were based either on a spherically symmetrical distribution of the charge

density n, or a complete factorization, n = np{Q)n,{z), in cylindrical coordinates {g,z). In this paper we

instead start with the Kadomtsev equation- and. using the factorization ansaiz

n = n{g, :-) = n^(i))n,{g,z) , (1)

with a parametric dependence of upon g, obtain an analytical solution for n(g,z). We also show that

np{Q) is an almost uniform function of g with a sharp fall at the edge, rather than a discrete set of coaxial

cylinders, as was often a.ssumed before. Our result has several features consistent both with Ruderman's^

semi-quantitative treatment for multi-electron atoms ami with .some explicit computations for hydrogen.*

By using the charge density distribution so obtained, one can calculate a Slater exchange term and then,

after solving Hartree-Fock-Slater equations, derive energy levels and other spectroscopic information.

2. BASIC PRINCIPLES^

We consider a Z-electron atom in a high magnetic field B which is parallel to the z-axis. If 5 >

then the energy of the motion in x - y plane is much greater than the energy of the motion in the z direction. This is the Landau regime, in which the ^-distribution of the charge density can be treated in a

one-dimen.sional Thomas-Fermi model. If, moreover, 5 > there is only one electron in each magnetic

sublevel m. We will consider this particular case. Solving the Kadomt.sev equation" for a one-dimensional, Thomas-Fermi model together with the Poisson

equation, we get for n ^'r = 1^ . (2)

In cylindrical coordinates the non-linear equation for ?)- = n;{g,z) can be written in the form

+ ^rzT- + C{g)—^ = -A{g)n; + D{g)n, , (3) dz- ag-^ ag

where g - \/2/B is the quantum cyclotron radius, which serves as a natural unit of length in the problem,

and where

.= = z/. , ^(J, = ,^!i + iM,/„^ C(^) = i + ^^, D(^) = 2/(.VnJ .(4)

If we neglect the term D[g)n, in Eqn. (3), we will g

et a simple scaling relation: the magnetic field B

determines the dimensions of an atom via g - \/'2/B, hwi the form of the electron density distribution

remains the same.

T W^e use atomic units. In particular, the unit of magnetic field is Bq - 2.35 x 10^ Gauss

159
160

3. SOLUTION OF THE KADOMTSEV EQUATION IN CYLINDRICAL COORDINATES

We assume that the radial wavefunctions are just Landau wavefunctions,

i/'n=o,„,(g) = . (5)

TT m

It has been shown by others that for the case B ^ there is only 1 electron in each magnetic sublevel, m.

This quantum number takes integer values from — (Z — 1) to 0. It therefore follows that

7T0- ^—' 77? ! TTO- m.-0 m. = 0

I I - ~ 0 > yz) .

The Landau wavefunctions Eqn.(5) strongly overlap, a fact that justifies the statistical treatment of the

Thomas-Fermi type.

Complete factorization, n{o,:) = (r) , enables easy analytical solution of Eqn.(3), but such

factorization is formally valid only if A = 0 and D = const.

If we allow a parametric dependence of 77; on g, we obtain a more realistic description of the atom in a strong field. Although we do neglect any explicit dependence on 77^ on g , such dependence is implicit,

because of the forms A{g) and D{g) in the equation that can be obtained from Eqn. (3)

'_^lAll=:_Aig)u',{:) + Dig)nA:) (7) azThis equation also can be solved analitically, and e.xplicit results for n^{g, :) are given in the following table,

where C'j is an arbitrary constant that can be calculated easily from the condition of normalization. The

other integration constant, C'l was chosen to get

^^l--c.(,., -0 (8)

A{g) nr.{gr~) C2{g)

< 0 Computed for the normalization

= 0 ^{~^ + C,(g))-

> 0 3A(e)

[ 4] Computed for the normalization

4. NUMERICAL RESULTS

Some calculations for a carbon atom in a field of 2 x 10^"G' are shown in Fig. 2, which displays 3- dimensional and contour plots of the electron density. The graphs have features consistent with Ruderman's

treatment'^ and with numerical calculations for hydrogen."^

Our next task is to .solve numerically the full Eqn. (3) and to derive effects due to a point nucleus Z. Eqn. (3) also gives an opportunity to study weaker magnetic fields if instead of expresssion Eqn. (6) we

substitute a corresponding form of 77^ in Eqn. (4).
E. P. Lief and J. C. Weisheit 161

FIGURE 1 Electron density n{Q, z) cross section in g - z plane passing through the center of the atom. Left: a

3-dimensional plot, right: a contour plot

5. SUMMARY

To this point our major conclusions are: • For an atom in a strong magnetic field, the Kadomtsev equation can be rewritten in a general form with

partial derivatives, Eqn. (3), using the factorization ansaiz to reflect natural, axial symmetry.

• Under certain assumptions the equation obtained can be solved analytically. The solutions have an

elongated form and are contracted both in length and width, as expected.

• Radial wavefunctions of individual electrons in a high magnetic field strongly overlap and lead to an

almost uniform "radial" electron density that falls sharply at the edge.

• A solution of the simplified Eqn. (7) ha-s features consistent with Ruderman's semi-quantitative predictions,^ and with detailed numerical calculations for hydrogen.^

ACKNOWLEDGEMENTS

We thank the U.S. Department of Energy for supporting this research under grant DE-FG05-91ER14213.

REFERENCES

1) Garstang R. H. 1977, Rep. Progr. Phys. 40, 105.

2) Kadomtsev, B. B. 1970, Soviet Phys. JETP, 31, 94.5.

3) Rau, A. R. P., Mueller, R. O., Spruch, L. 1975, Phys. Rev. A 11, 1865.

4) Neuhauser, D., Koonin, S. E., Langanke, K. 1987, Phys. Rev. A 36, 4163.

5) Spruch, L. 1991, Rev. Mod. Phys. 63, 151.

6) Ruderman, M. 1974, in Physics of Dense Matter, ed. C.J.Hanzen and L.H.Volsky (D.Reidel Publishing

Company: Dodrecht, Holland / Boston, MA), p. 117.

7) Lieb E.H., Solovej J. P., Yngva-son J., Phys. Rev. Lett. 69, 749 (1992).

8) R5sner, W., Wunner, G., Herold, H., Ruder, H. 1984, .J. Phys.B: At. Mol. Phys. 17, 29.
Fine Structure Splittings in the Ground State of

B-Like Ions: Rb32+ -Xe^9+

M. A. Ali

Howard University, Washington, D.C. 20059

and

Y.-K. Kim

NIST, Gaithersburg, MD 20899

Forbidden lines due to transitions between ground levels of the n=2 "complex" in ions are of great interest for plasma diagnostics. Edl6n' fitted the difference between experimental

and multiconfiguration Dirac-Fock (MCDF) fine structure results of Cheng et al.^ to a screening

formula that includes nuclear charge Z and a few fitting parameters to allow for correlation and

relativistic corrections partly missing in the theoretical values, and predicted unknown fine structure splittings of B-like ions up to Kr^'"*". The original multiconfiguration Dirac-Fock level

energies of Cheng et al.- were obtained by optimizing the relativistic radial orbitals and the

configuration mixing coefficients (MCDF-OL) for each level separately. This procedure leads

to a nonrelativistic offset-^, i.e., a nonvanishing (and spurious) fine structure splitting in the

nonrelativistic limit between the levels arising from the same LS term. Edlen used for his fitting

uncorrected fine structure splittings, which contained these spurious nonrelativistic offsets.

Furthermore, Cheng et al." used the <r> method,'* which uses expectation values of r of

MCDF orbitals, in estimating the effect of screening in the self-energy part of the quantum

electrodynamic (QED) corrections.

Since then other methods have been developed to estimate the self-energy screening. One

of them is to use the charge density of MCDF orbitals near the nucleus; we shall refer to this as the p method. The p method leads to results on transition energies that agree better with

experiment than the <r> method, particularly for high-Z ions. Our MCDF codes use these newer methods to yield MCDF-OL energies. Moreover, new experimental results have also

become available since Edlen published his recommended fine structure splittings. Also, Kim

and Weiss^ pointed out that, for the calculation of the fine structure splitting, MCDF calculations

should include all j-j configurations which are degenerate in the limit of infinite Z and thus

belong to the same "relativistic Coulomb complex."^

The difference between experimental and MCDF fine structure splittings may then be

expected to be a smooth and slowly varying function of Z although the functional dependence

may be a complicated polynomial in Z and Z"' over an extended range of Z. This difference can then be used not only for identifying irregularities in experimental data, but also to interpolate and extrapolate to estimate unknown fine structure splittings.

We show the difference, Expt. - MCDF, between experimental and theoretical values

of fine structure splittings corrected for nonrelativistic offsets for Z= 19-36 in Fig. 1 using the

p and <r> methods to estimate QED corrections. We see that the curve with the p method

varies almost linearly with Z while the curve with the <r> methods rises sharply with Z. The

162
M. A. All and Y.-K. Kim 163

fine structure splitting for cobalt (Z=27) does not follow trends of the rest of the curves,

suggesting that the experimental value might be in error. We fitted the p curve to a linear

formula and obtained:

A(p) = 26.444 Z - 479.00 (cm"')

with a standard deviation of 37.08 cm"^

This fitted formula smooths fluctuations in experimental data, and hence fine structure

splittings obtained from the formula should be more reliable than the original experimental data.

We used this fitted formula to obtain predicted fine structure splittings for Rb''^'*' to Xe''^"'" in

Table 1. The table also lists Edl6n's predictions and known experimental values. Our

predictions up to Mo^^"^ are probably accurate within 40 cm'^ In the absence of experimental

data for neighboring ions to define the difference curve, those for Tc^^"^ through Xe^^"^ are

likely to be accurate within 80 cm'^

References

1. B. Edl6n, Phys. Scr. 28, 483 (1983).

2. K. T. Cheng, Y.-K. Kim, and J. P. Desclaux, At. Data and Nucl. Data Tables 24, 111

(1979).

3. Y.-K. Kim and K.-N. Huang, Phys. Rev. A 26, 1984 (1982).

4. Y.-K. Kim, D. H. Baik, P. Indelicate, and J. P. Desclaux, Phys. Rev. A 44, 148

(1991).

5. Y.-K. Kim and A. W. Weiss, Bull. Am. Phys. Soc. 35, 1188 (1990).

Fig. 1. FINE STRUCTURE SPLITTING IN B-LIKE IONS

COMPARISOS' OF DIFFERENT OED CORRECTIONS

NUCLEAR CHARGE Z

EXT - RHO ^ EXT - <R>
164

Table 1. MCDF-OL, fitted and experimental fine structure splittings in the ground state of

boron-like ions (in cm"') using QED corrections for K''*"'' through Xe'*^"'".

Ion xixpi. iixiien 1 neory ion 1 neory

9 soon 9Qf»rLl 98Qil4 Z07'H+ JJJkAJC)

JODl "^^^/^ll 11 DZJ J7

Cpl6 + oC 4jDj / 4JJ77 v34 +

I ^iQRn71

1

'^^=i9An JDZ ^^^9 1 f\ 1

7_35 + yl8 +

V DODiU Doouy \jojyj IN u oD / 7'tD R9Q97 Mn37 +

IVIU yyjjyy I

IVIII QQ419 38 + 11 O^^ROSR UDOUJ 0

rc 1 1 C97n 1 1 oz. /u 1 1 8960 1 1 C9AQ

1 ^10900 1 J7 / UZ 1 jy iij JVIl 1 ^09 1 OQ

INI 1 UJ"DVj 1 1 J 1 DJ700 r U I HjjKjyj

L-U 1 Ql 9Qn l7 i jZo 1 Q 1 "i/l 1 Ag 1 J /H^Kjy'*

Zn^^- 222021 222032 Cd^3+ 1725648

Ga2^+ 256329 256335 In^^+ 1888334

Ge^^+ 294551 294539 294536 2062739

As2«+ 336950 336937 Sb^^+ 2249480

Se29+ 383833 383876 383850 Te^^+ 2449199

435644 435644 435602 j48 + 2662565

Kr3i + 492560 492596 492537 Xe^^+ 2890260
COMPLEX QUANTUM DEFECT AND SCREENING PARAMETERS

FOR AUTOIONIZING STATES OF TWO- AND THREE-ELECTRON ATOMS

FROM LOWEST-ORDER PERTURBATION THEORY

Lonnie W. Manning and Frank C. Sanders

Department of Physics, Southern Ilhnois University- Carbondale

Carbondale, IL 62901-4401

In the usual quantum defect theory, the energies for a Rydberg series of

autoionizing states of an A^-electron atom can be written as a sum of the threshold

energy for the series, Eth plus the energy of the Rydberg electron.

Here a is the screening of the nuclear charge, Z, by the core electrons, n is the

principal quantum number of the Rydberg electron, and /i is the quantum defect.

By making /i (or a) complex one can also include the width of these autoionizing

states in the method. In practice, a and/or fi are generally obtained by fitting

to experimental and theoretical data for a few members of the Rydberg series.

In recent work on autoionizing states of two- and three-electron atoms, we

have found that the lowest-order perturbation expansion coefficients of the energy

and width provide useful information for the classification of such Rydberg states over a broad range of Z and n. These coefficients can also yield reasonably

accurate values of the resonance positions and widths. In the present work,

we make use of these coefficients within the quantum defect method to obtain

quantitatively useful data for such states of two- and three-electron atoms lying

below the n=2 ionization threshold. The parameters of the method, and even the

appropriate choice of approximant for a particular Rydberg series, are entirely

determined by these lowest-order coefficients. Hence, the method is "ab-initio",

requiring no additional input.

In Z-dependent perturbation theory, the Hamiltonian is written as Hq -f \Hi

where

Jf„ = f(-lA.-i); H, = Z-^Ef>.^-

The energy and width are given as expansions in A = 1/Z: E = Y11^=q Z^~'^en;

F — Yl^=2 ^~^^n- can also be expanded in powers of A, cr = Y1V=Q ^k^^ The

coefficients, crjt, can thus be expressed in terms of the conventional perturbation

coefficients of Er and Eth- Hence, cTq = n^(ei — e\^) which, as expected, will

approach A'' — 1 in the limit of infinite n. Similar relations can also be obtained

for the quantimi defect, fi.. The lowest-order contribution is just fii = n[N — 1 —

165
166

There are several alternative approaches that could be attempted at this

point. For those states with ao ^ N — I, a is represented with sufficient accuracy

by its zeroth-order value, ctq, and a good approximant for the energy of such

states is,

Er^Eth-^^- (1)

This expression is equivalent to truncating Er to second-order in A and approximating €2 by e^^ — j^. Thus, for large values of Z, the error in Er is a term

constant in Z and of 0{l/n^). For highly excited states, this difference rapidly

becomes negligible.

Physical considerations tell us that a must be less than or equal to A'' — 1 for all Z and n. Therefore, in those cases where cTq > N — 1, the usual quantum

defect theory with and a = N — 1 is used,

\2 Er ^ - f^^- (2)

In actual practice, it was found that these two approximants could be more

effectively replaced by two alternative formulae which yield improved results over a wide range of n and Z. Replacing the first of the above approximants

(screening), we have utilized

« _ + ilz£±l^-^. (3)

As an alternative to the second of these approximants (quantum defect), we have

utilized

« E,, - (4)

where cr^^ = - 1 + [n'^{ei - ) - + 1]A

To obtain the total width of these states, we let n n — while keeping the

screening parameter a purely real number. The resonance position and width are then given by

Lr-l2- Eth - ^ -fvi- 2(n— )

and the total width is given by F = ^(Z - cr)^ (1 + {^)'^)~'^ 7, the "reduced

width", can also be written as an expansion in A, and relations between these
Lonnie W. Manning and Frank C. Sanders 167

and the r„ yield a simple approximant to the third-order width: Fa « —2(7or2.

Thus, the total width is approximated here by,

r«r2(i-2f), (5)

Results are presented for the 36 lowest ^'^5^ and 48 lowest ^'^P° autoionizing

states for two-electron atoms, and the 36 lowest autoionizing states for threeelectron atoms lying between the first and second ionization thresholds. Exact

values for ei and r2 are presented, together with the corresponding values of

(Jo and fii. Estimates of the resonance positions and widths for these states axe compared with some recent experimental and theoretical values available in

the Uterature. This comparison indicates that these lowest-order values are not

only useful in the high-Z and n limit, but are also capable of giving reasonable

estimates of both the resonance position and width for fairly low values of Z and

n.

The three electron, doublet S-states presented here are all four-fold degenerate. Classification of these states is complicated by the fact that the mixing

coefficients of the individual components of the zero-order wave functions behave

erratically for the first few members of this rydberg sequence. Similarly, the

lowest-order widths also exhibit this erratic behavior. These states can be classified into four unambiguous series, however, based on their first-order energies.

These first-order energy expansion coefficients exhibit very smooth behavior with

increasing degree of excitation. Of particular interest are two of these series of

states, which become nearly degenerate in first-order at n = 6. This near degeneracy is the source of the erratic behavior of the mixing coefficients noted above.

These particular states correspond to autoionizing states of the atom which, for

high n, decay to the (l325)^S and {ls2p)^P states, respectively. At n = 6 each

of these two states shows a significant enhancement of the component of the

other state, so that each state becomes less "pure" and more of a mixture of

the two components. Nevertheless, these states can be unambiguously classified

by their first-order energies. Although this near degeneracy has little apparent

consequence for the resonance position of these states, the effect on the widths

is marked. Note that this irregular behavior of the widths along the Rydberg

series is essentially due to the individual perturbation expansion coefficients, ei and and can therefore be expected to persist over a range of values of Z.

Finally, it should be noted that there is little information available in the

Hterature for the widths of many of these states. Of particiilar interest are those

states where the total widths are extremely small. This is the case for all the

Rydberg series considered here as the level of excitation increases. For such states,

it becomes very difficult to calculate such widths variationally with any precision.

Since the extent to which the r2 accurately represent F improves rapidly as Z

and n increase, the present results can be quantitatively useful, especially in the

absence of other reliable results.
RAIR RUNCXIOM CA l_C U l_ AX Z ON S ROR SCREENED COULOMB ROXENXIALS'

ZHENGMING WANG, YONG YAN , HONGBIN ZHAN and PETER WINKLER

Department of Physics, University of Nevada, Reno.

The results of pair function calculations of ground

and excited state energies of H" and He in various plasma

environments are compared to very accurate calculations. The

stability of the negative hydrogen ion in screened Coulomb

potentials has been studied in particular.

1 INXRODUCXION

Numerical pair functions^ have become an important tool

in the study of atomic structure. For helium-like systems

they offer a rather convenient way to obtain accurate,

numerical bound-state wave functions. For larger systems the

construction of pair functions is a feasible alternative to

the correlation of single particle functions2'3 .While the

ultimate goal of an ab initio theory of general plasmas is

still a development of the future considerable progress has

been made for non-ideal hydrogen plasmas* and to some extent

for helium plasmas^. A welcome alternative is offered by

two-component plasma calculations based on density

functional theory^ . Such calculations determine distribution

functions for ion-ion and ion-electron pairs. Potentials

derived from such quantities allow the inclusion of plasma

effects into atomic structure and scattering calculations in

some average way.

of the negative hydrogen ion in various screening

environments. We proceed from the simple Debye screening

model to mce realistic potentials obtained from pair

distribution tunctions of two-component plasma simulations.

'Work supported by the Division of Chemical Sciences, Office

of Basic Energy Sciences, Office of Energy Research, U.S.

Department of Energy.

Here we have studied, in particular, the stability

168
Zhengming Wang et al. 169

2 THE ATOMIC RA I R FUNCTION

Details of the theory of atomic pair functions can be

found in a publication by Martensson^ . We have developed a modified computer code that allows the inclusion of plasma

screen i ng

.

For two-electron systems the equation for the pair

function Pab is given by

[€.+£b-ho ( 1 )--ho (2)] iPab >= ^ I rsxrsi V| ab+Pab > - rsED

^ Pc d <cd I V I ab+/o a b > (1)

cdGD

Here D is the model space spanned by a subset of

ei genf uncti ons of an approximate Hamiltonian consisting of a sum of single-particle operators ho ( i ) . Starting with an

initial guess for p on the right we use the function

obtained in the (n-1)st step as input for the n-th

iteration. The one-electron problem connected with hg has to

be solved first ( here given for Debye screening ):

hQ(i) = -V^2/2 . 2 exp(-ri /D)/r^ . . (2)

More realistic choices for u(r) have been studied also.

3 R ESU LTS

In Table 1 we present results of the present calculation

for inreasing screening comparing the ground state energy of

H" to the binding energy of H. Both values decrease with D.

We notice that at values of D ~ 34 the two-electron system

ceases to be bound. What happens when we go beyond the bound

regime? Does the system emit the second electron immediately

into the continuum or do features of the bound system

survive ? Our calculations yield electron densities in the

continuum that are not much different from those of bound

states. Similar findings for screened one-electron systems

have been reported previously^. In table 2 we show results

for the 1s3s - states of the helium atom near the critical

screening value for which the system becomes unbound.
170

D H -atom H - i on H -ion H -ion

(N=45) (extrapolated

)

( exact

)

CO -0 . 500000 -0.527613 -0. 527322 -0. 527750

100 -0 .490074 -0.508135 -0. 5081 18 -0.508018

35 -0 .472049 -0.472854 -0 . 472540 -0 .472745

34. 25 -0 ,471430 -0.471 702 -0.471535 -0.471588

34 -0 .471225 -0.471 305 -0.471249 -0.471 1 91

33 . 5 -0 .470848 -0.470543 -0.470343 -0.470343

32 -0 . 469668 -0.468149 -0.467981 -0.468699

XAB l_ E 1 The ground-state energy of the H' -ion for

some values of the Debye parameter D is compared to the

ground state energy of the neutral atom . Columns 3 and 4

show the results of the present calculation obtained on a grid of 45 by 45 points and the values of the Richardson

extrapol at i on

D He-atom He-atom Orbi tal Energies

1 1 s3s ^ S> 1 1s3s -^S) Is 3s

as -2.061907 -2.067574 -2 .000000 -0.222222

1 00 -2.022529 -2.029193 -1 . 980074 -0. 202088

50 -1 . 990510 -1 .998564 -1 .960298 -0. 184795

20 -1 . 899884 -1 . 902935 -

. 9081 84 -0. 137318

"TABLE 2 The energies of the 1s3s - states of

the He-atom for some values of the Debye parameter D are

shown together with the electron energies of the atom.

-4- RERERENCES

1 Lindgren I. and Morrison J. 1986, Atomic Many-Body Theory

(Heidelberg: Springer Verlag, 2nd edition).

2 Morrison J., J. Phys. B.: Atom . Mo 1 ec . Phys . 6,2205 ( 1973 ).

3 Winkler P., Int. J. Quant. Chem. S 19, 201 (1986).

4 Lehmann H. and Ebeling W.,Z. Naturforsch, 46a, 583 (1991).

5 Forster A., Kahlbaum T., and Ebeling W. 1991, in Proc. XX.

Int. Conference on Phenomena in Ionized Gases (in press).

6 Dharma-wardana M. W. C. and Perrot F., Phys . Rev . A26 , 2096

( 1 982 ) . 7 Martensson A., J. Phys. B.: Atom . Mol ec . Phys . 12,3995 (1979).

8 Wang Z., Winkler P., Pickup B. T., and Elander N., Chem.

Phys. 135, 247 (1989).
Atomic properties

from large-scale relativistic calculations

F. A. Parpia and C. F. Fischer

Computer Science Department

Box 1679, Station B

Vanderbilt University

Nashville, Tennessee 37235

The RSCF (relativistic self-consistent-field) and RCI (relativistic configuration interac- tion) programs are derivatives of the GRASP2 multiconfiguration Dirac-Fock package.

RSCF and RCI are expressly designed for the construction of atomic models with large

configuration state function bases [O(IOOO) and up]. In addition to the atomic properties

that can be computed using GRASP2 — level energies using the Dirac-Coulomb operator, corrections due to higher-order relativistic effects, and radiative transitions — nuclear

motional corrections to level energies and diagonal hyperfine constants may be calculated

with RCI. We describe RCI, RSCF, and a set of associated utility packages, and present

examples of atomic properties computed using this approach to atomic structure.

The Multiconfiguration Dirac-Fock approach

The multiconfiguration (MC) Dirac-Fock (DF) method is based on the Dirac-Coulomb Hamiltonian:

i = l » = 1 j=! + l

for an A''-electron atomic system. Here R,j = r,- — rj and we use Hartree atomic units. The natural

generalisation of the nonrelativistic orbital is the four component function,

,

I ,. > f

Pnij{r)xijmii)\

We refer our readers to review articles [1, 2] for the details of the formalism, the trends of relativistic corrections, and an introduction to the literature. For our purposes it will suffice to note that all relativistic

effects to order l/c^ are included if the Dirac-Coulomb Hamiltonian is augmented by the Breit Hamiltonian,

i=i j=i+i '•' \ »j /

The programs described in the remainder of this presentation are based on such a relativistic formalism.

RCI, RSCF, and the utility programs

The GRASP2 MCDF program [3] is a major revision of GRASP [4] , in turn a major revision of MCDF+MCBP/BENA [5]. Extensive testing of GRASP2 has demonstrated that it is appreciably more stable than its predecessors.

We attribute this to the relatively straightforward adaptation to the relativistic problem of the self-consistentfield (SCF) algorithms developed by Fischer and coworkers [6] for the nonrelativistic MC Hartree-Fock (HF)

model, as well as to improved numerical integration, quadrature, and interpolation procedures.

171
172

It is natural to attempt to construct more sophisticated models of atoms as programs become more stable and computers become more powerful. Large-scale MCHF calculations have been carried out by Fischer and

coworkers using the MCHF_ASP suite of programs [7] and derivatives. Here we describe revisions of the

GRASP2 program carried out with the same scope. Extensions to FORTRAN 77 permitting the run time allocation and deallocation of storage to arrays have been implemented in several compilers. Such dynamic memory allocation has been employed in RSCF

[8] and RCI [8]. The elements of the lower triangle of the Hamiltonian matrix are stored in a sparse representation that reduces memory requirements when « 33% or more of the elements are zero.* In contrast

to GRASP2, only the eigenvalues and eigenvectors (together, eigenpairs) of interest are computed and stored

in RSCF and RCI. Eigenpairs are determined using the Davidson procedure [9] as implemented in a package

due to Stathopoulos and Fischer [10]. These modifications have significantly reduced storage requirements

and computational effort. Further improvements in efficiency in RSCF result from the elimination of all modules not required for the MCDF SCF problem. Similarly, in RCI all modules that apply only to the

SCF problem have been eliminated.

The normal and specific mass shifts that result from nuclear translational motion can be estimated

using RCI [11], as can the diagonal hyperfine constants A and B [12]. These capabilities go beyond those

of GRASP2. The properties of radiative transitions could be estimated with GRASP2 and GRASP. This

feature continues to be available in RCI.

Several utility packages are associated with GRASP2: a complete active space (CAS) [13] generator,

JJCAS [14], programs for visualising atomic structure, and programs for computing coefficients for higher

order numerical methods for the GRASP2 family of codes have been prepared. With few exceptions, CAS

calculations are prohibitively expensive. A new package, GENASJJ, generates lists of configuration state functions (CSFs) associated with subspaces — referred to as active spaces (ASs) — of the CASs. Another new utility, MERGEORB, may be used to extract and combine orbital wavefunctions from GRASP2 or RSCF ORBOUT Files into a new ORBOUT File. Finally, MERGEJJAS, in preparation, will permit the

merging of two or more CSF lists from GENASJJ.

Together, RSCF, RCI, GENASJJ, MERGEORB and MERGEJJAS form a fairly complete suite of

programs for the computation of atomic properties using the MCDF formalism.

Large-scale relativistic calculations

With few exceptions, MCDF models of atoms have been constructed with substantially fewer than 1000

CSFs. We shall understand large-scale calculations to be those involving models with several hundred or more CSFs. Computations with a few thousand CSFs are now routinely carried out at Vanderbilt University

using Sun workstations with 64MB or less of memory and 200MB or less of disk storage.

New approaches to the systematic study of atomic structure become possible using large-scale calculations. Different ASs may be used to construct models, the properties of which, in comparison with measurements, may be used to establish trends. This knowledge may then be applied to improve the reliability of

theoretical models in other contexts. An earlier modification of the GRASP2 program along the lines of RSCF was prepared by V. M. Umar,

Z. Cai, and C. F. Fischer, and applied successfully to the prediction of the low-lying spectrum of the Pr IV

ion [15]. This work, involving between 354 and 1708 CSFs in each of the largest calculations, was carried out on a network of Sun workstations.

We are currently studying the hyperfine structure of the 3d^^Pi,2 levels of the Sc II ion using the

programs described in the previous section. As observed first by Young et al. [16], the simplest DF and MCDF

models cannot account for the measured value [17] of the diagonal hyperfine magnetic dipole parameter A. A summary of calculations completed to date appears in Table 1 below. New abbreviations used are: OL —

optimal level calculation; S — single; D — double; R — replacement. The largest of these [a 3487 CSF CI

calculation for the lowest level (1)] required less than 20 MB of storage and less than 12 hours of CPU time on a Sun SPARCstation 2.

* This applies to computers with 32-bit architectures; for 64-bit architectures the sparse representation is more efficient than a packed full representation when « 50% or more of the elements of the Hamiltonian are

zeros.
F. A. Parpia and C. F, Fischer 173

Table 1: Measurement and calculations for the diagonal magnetic dipole hyperfine parameter of the 3d^^Pi

level of Sc II.

Future developments

We are currently revising the RSCF and RCI programs and associated utilities with a view to improving their computational efficiency and user interfaces. Experience gained from the parallelisation of the MCHF_ASP

suite will be brought to bear in the preparation of parallel versions of RCI and RSCF for distributed and

shared-memory parallel processors. Acknowledgments

This work has been supported by the Department of Energy, Office of Basic Energy Sciences; and the

National Science Foundation, under grant ASC-9005687.

References

[1] I. P. Grant, Methods in ComputatiomJ Chemistry 2 (1988) 1

[2] P. Pyykko, Chemical Reviews 88 (1988) 563

[3] F. A. Parpia, I. P. Grant, and C. F. Fischer, 1990, unpublished; most features of GRASP2 have been described

in: F. A. Parpia and I. P. Grant, Journal de Physique IV, Colloque Cl, supplement au Journal de Physique 1 (1991) Cl-33

[4] K. G. Dyall, I. P. Grant, C. T. Johnson, F. A. Parpia, and E. P. Plummer, Computer Physics Communications

55 (1989) 425

[5] I. P. Grant, B. J. McKenzie, P. H. Norrington, D. F. Mayers, and N. C. Pyper, Computer Physics Communications 21 (1980) 207; B. J. McKenzie, I. P. Grant, and P. H. Norrington, Computer Physics Communications 21

(1980) 233

[6] C. F. Fischer, Computer Physics Reports 3 (1986) 273

[7] C. F. Fischer, Computer Physics Communications 64 (1991) 369; ibid. 399; ibid. 431, ibid. 473; C. F. Fischer and B. Liu, ibid. 406; A. Hibbert and C. F. Fischer, ibid. 417; A. Hibbert, R. Glass, and C. F. Fischer, ibid. 455; C. F. Fischer, M. R. Godefroid, and A. Hibbert, ibid. 486; C. F. Fischer and M. R. Godefroid, ibid. 501

[8] F. A. Parpia, I. P. Grant, and C. F. Fischer, 1992, unpublished

[9] E. R. Davidson, Journal of Computational Physics 17 (1975) 87

[10] A. Stathopoulos and C. F. Fischer, in preparation

[11] F. A. Parpia, M. Tong, and C. F. Fischer Physical Review A, in press.

[12] P. O. Jonsson, F. A. Parpia, and C. F. Fischer, 1992, unpublished

[13] This terminology was introduced in quantum chemistry by B. O. Roos, P. R. Taylor, and P. E. M. Siegbahn,

Chemical Physics 48 (1980) 157; the first description of the underlying idea may be found in the article of K. Ruedenberg and K. Sundberg in Quantum Science: Methods and Structure; A tribute to P.-O. Lowdin,

edited by J.-L. Calais, O. Goscinski, J. Linderberg, and Y. Ohrn; Plenum, NY 1976

[14] F. A. Parpia, W. P. Wijesundera, and I. P. Grant, in preparation

[15] Z. Cai, V. M. Umar, and C. F. Fischer, Physical Review Letters 68 (1992) 297

[16] L. Young, W. J. Childs, T. Dinneen, C. Kurtz, H. G. Berry, L. Engstrom, and K.-T. Cheng, Physical Review

37 (1988) 4213

[17] A. Arnesen, R. Hallin, C. Nordlins, 6. Staaf, L. Ward, B. Jelenkovic, M. Kisielinski, L. Lundin, and S. Mannervik,

Astronomy and Astrophysics 106 (1982) 327

Experiment [17]

1 OL 1: Reference CSF: Is22s22p22p^3s23p23p^3a3d J = 1 77 OL 2: Is, ... , 3d from 1 OL 1; 4s, . .

. , 4f from SRAS of 3s, . . . ,4f

3487 CI 1: Is, . .

.

, 4f from 77 OL 2; SDRAS of 3s, ... , 4f 157 OL 2: Is, ... , 4f from 77 OL 2; 5s, ... , 5g from SRAS of 3s, ... , 5g

250 OL 2: Is, ... , 5g from 157 OL 2; 6s, ... , 6h from SRAS of 3s, ... , 6g

148 OL 2: Is, ... , 3d from 1 OL 1; 4s, . .

.

, 4f from SRAS of 2s, ... , 4f

167 OL 2: Is, ... , 3d from 1 OL 1; 4s, . .

. , 4f from SRAS of Is, ... , 4f

343 OL 2: Is, .

.

, 4f from 167 OL 2; 5s, ... , 5g from SRAS of Is, ... , 5g

A = -107.3(6) MHz

-1.8

-7.0

-10.9

-55.1

-56.2

-13.3

-13.3

-83.9
Convergence Studies of Atomic Properties from Variational Methods:

Total Energy, Ionization Energy, Specific Mass Shift,

and Hyperfine Parameters for Li and Be

Ming Tong, Per Jonsson* and Charlotte Froese Fischer

Vanderbilt University

Nashville, TN 37235 USA

* Present address: Depeirtment of Physics, Lund Institute of Technology, P.O. Box 118, S-221 00 Lund, Sweden

In this paper we report on the study of systematic approaches for MCHF wave function calculations for both Li and Be, and the convergence patterns that are observed for a number of atomic

properties. Since the variational procedure is based on the expression for the total energy of the

system, the convergence pattern of the energy is of great importance. Other properties may rely on different parts of the wave function and may converge more rapidly than the total energy. The

ionization energy, E(Li'^) - E{Li), for example, relies more on the outer portion of the wave function as does an oscillator strength (or /-value) for the resonance transition, whereas the hyperfine

contact term depends almost entirely on the wave function near the nucleus. The specific mass

shift (SMS) has not been studied nearly as extensively as some other atomic properties. For some

states of light atoms, the mass polarization correction may be larger than relativistic effects. Its dependence on the wave function is more like that of the energy, except that, being a smaller

effect, it does not need to be computed to as many significant digits.

1 Results for Lithium

The lithium ground state is an excellent test case for our studies. Very accurate non-relativistic

energies are available for comparison obtained from Hylleraas type of calculations which explicitly

include the inter-electronic distance in the series expansion for the wave function (e.g. [1]). Unlike our MCHF approach, the latter cannot readily be extended to many-electron systems.

We use the n-expansion method to compute the wave function along with the other atomic

properties, as shown in Table I. The column denoted "n" indicates the largest n values, in other

words, all of the orbitals with n up to the given value are included in the calculation. The

configuration list is generated from an active set of electrons.

We see in Table I that the computed total energies show convergence, but clearly, the procedure

has not converged to the desired accuracy, although our computed total energy is the lowest among

the known variational calculations so far. Also included in Table I are the ionization energy (IE), specific mass shift (SMS), and Fermi

contact term as a function of n. The former was computed as E{Li'^) — E(Li), using the same

orbital basis for the positive ion as for the neutral atom. This leads to an uneven increase in

IE. The SMS (from the gradient form, in cm~^) shows a generally decreasing trend whereas the

Fermi contact term {uc) is increasing.

174
Ming Tong et al. 175

Table I: The total energy (Etot), the ionization energy (IE), the specific mass shift (SMS) and the

Fermi contact term (cc) from different n sequences for ls^2s ^S in ^Li.

n Etot (a.u.) IE (a.u.) SMS ( Gradient

cm ^)

Slater

Cc (a.u.)

2 -7.454 565 28 0.196 436 28 5.544 94 9.624 35 2.073 08

3 -7.473 184 27 0.196 512 54 5.147 33 10.109 27 2.827 43 — < .4 / 0 zUo Ui fl 1 07 7QO QO c 1 on oo ft 07Q Oft Z.oZD Zo

5 -7.477 159 95 0.197 941 52 5.208 56 5.072 19 2.907 37

6 -7.477 579 74 0.198 078 16 5.205 35 5.303 60 2.888 79

7 -7.477 772 41 0.198 105 70 5.200 00 5.188 70 2.905 66

8 -7.477 874 32 0.198 125 16 5.197 13 5.221 48 2.903 98

9 -7.477 932 61 0.198 131 76 5.195 27 5.195 62 2.904 85

10 -7.477 968 61 0.198 136 79 5.194 15 5.203 60 2.905 13

00 -7.478 060 9 0.198 146 1 5.192 5 2.905 3

other -7.478 060 I'' 0.198 142 7^ 5.192 4-= 2.906 02^^

" Ref. [1]

^ Ref. [2]

" Ref. [3] ^ Ref. [4]

A similar study is carried out for the 15^2^ state. We obtain a value of 0.130 229 2 a.u. for

the ionization energy; 4.2484 cm"^ for the SMS. The convergence is similar to that of Table I. The oscillator strength for the resonance 15^25 ^S — ls'^2p transition is computed with the same n-expansion, as shown in Table II. Our calculated transition energy is 0.067 908 8 a.u. We

obtain an /-value of 0.7472 (length form). This is similar to other recent theoretical predictions,

but, is still larger than the experimental values.

2 Results for Beryllium and Negative Lithium

Similar n-expansion calculations are performed for the ls'^2s'^ ground state of Be and Li".

Now, because of the rapid increase in the number of configuration states with n, rules based on

the observed patterns of significant configuration states are employed to restrict the wave function

expansion. At the same time, small contributors are omitted.

Our extrapolated total energy is -14.667315 hartrees for Be and -7.500758 hartrees for Li".

The former agrees well with the "exact" non-relativistic energy estimated by Lindroth et al. [5]

of -14.667353 hartrees.

The electron affinity for Li is predicted to be 0.61760±0.00004 eV which is identical to the

experimental value of Dellwo et ai. [6], although the latter has larger error bars. The affinity is
176

Table II: The Transition energy (AE) in a.u., the line strength S in a.u., and /-value for the

2s — 2p resonance transition from different n sequences.

n AE (a.u.) S (a.u.) /-value

Length Velocity Length Velocity

2 0.074 442 3 33.788 1 28.694 5 0.838 42 0.712 03

3 0.068 596 6 33.806 8 32.787 0 0.773 01 0.749 70

4 0.068 352 0 33.230 0 33.994 1 0.757 11 0.774 52

5 0.067 992 9 33.029 2 33.017 5 0.749 89 0.749 41

6 0.067 935 3 33.029 2 33.017 5 0.747 95 0.747 68

7 0.067 915 6 33.015 2 33.008 7 0.747 42 0.747 27

8 0.067 908 8 33.008 8 32.998 3 0.747 20 0.746 97

other 0.067 904 7

"

" Obtained by subtracting the total energies (as reported by Pipin and Bishop [1]).

slightly larger than the value reported by Chung and Fullbright [7]. The change in the specific mass shift parameter in going from Be ls^2s^ to Be"^ 15^25 is 0.00723 a.u. in excellent agreement with the experimental value of 0.006741 a.u. reported by

Wen et al [8].

Acknow^ledgments

This research was supported by a grant from the U.S. Department of Energy, Office of Basic

Energy Sciences.

References

1. J. Pipin and D.M. Bishop, Phys. Rev. A 45, 2736 (1992).

2. K.T. Chung, Phys. Rev. A 44, 5421 (1991).

3. F.W. King and M.P. Bergsbaken, J. Chem. Phys. 93, 2570 (1990).

4. A. Beckmann, K.D. Boklen and D. Elke, Z. Phys. 270, 173 (1974).

5. E. Lindroth, H. Persson, S. Salomonson, A-M Martensson-Pendrill, Phys. Rev. A

45, 1493 (1992).

6. J. Dellwo, Y. Liu, D.J. Pegg, and G.D. Alton, Phys. Rev. A 45, 1544 (1992).

7. K.T. Chung and P. Fullbright, Physica Scripta 45, 445 (1992).

8. J. Wen, J.C. Travis, T.B. Lucatorto, C. Johnson, and C.W. Clark, Phys. Rev. A

37, 4207 (1988).
PROSPECTS FOR RELATIVISTIC

MULTICONFIGLRATION DIRAC-FOCK-BREIT

CALCULATION USING GAUSSIAN BASIS SET

METHOD

Farid A. Parpia and Ajaya K. Mohanty

IBM Corporation

Supercomputing Systems, High Performance

Supercomputing Systems Lab.

Kingston, New York 12401

* Present address: Department of Computer Science

Vanderbilt University, Nashville, TN 37235

177
178

Atomic properties

from relativistic basis-set calculations

Two programs from IBM. Based on kinetically-balanced geometric Gaussian basis sets.

GDFB: Dirac-Fock-Breit (DFB) program. Only for closedshell atoms and ions. "Step" or "Fermi" nuclear charge distribution.

• F, A. Parpia, A, K. Mohanty, and E. Clementi, J. Phys,

B: At, MoL Opt. Phys. 25 (1992) 1 • F. A. Parpia and A. K. Mohanty, Phys. Rev, A, in press

• A large DFB calculation for the ground state of Hg has

just been completed.

MCGDFB: Multiconfiguration DFB program. Integral generation packages for one- electron (overlap, kinetic-energy, and

electron-nucleus interaction) integrals and for Coulomb twoelectron integrals completed and tested. These packages were

carefully designed for efficient execution on IBM 3090 and

ES/9000 computers equipped with the Vector Facility. Execution times are roughly 1/20 of comparable modules in GDFB.

• F. A. Parpia and A. K. Mohanty, IBM DSD Technical

Report, 14 August 1991.

The many-body problem of electronic structure physics may

be cast in a form that is "embarassingly parallel" and are ideal

candidates for distributed memory parallel processors.
Farid A. Parpia and Ajaya K. Mohanty 179

Efficient generation of one-electron integrals

The one-electron integrals most difficult to compute are the

electron-nucleus interaction integrals. These involve incompleta Gamma functions,

X

/ X f y ^'^ j{a,x) — at e t 0

All incomplete Gamma functions required in MCGDFB may

be obtained from two sets of Gamma functions using the recurrence relation

7(a, x) = - \j{a -\- l,x) -\- X e

a

which is stable as written. Our procedures for the generation

of the two initial sets of incomplete gamma functions, as well

as our use of the recurrence relation, vectorise.

Databases

\

I

CRITICALLY EVALUATED DATA ON ATOMIC SPECTRA - ENERGY LEVELS, WAVELENGTHS, AND

TRANSITION PROBABILITIES*

W. C. Martin, A. Musgrove, J. Reader, and J. Sugar

Atomic Energy Levels Data Center

W. L. Wiese and J. R. Fuhr

Data Center on Atomic Transition Probabilities and Line Shapes

G. R. Dalton

Standard Reference Data Program

National Institute of Standards and Technology (NIST),

Gaithersburg, MD 20899, USA

and

T. Shirai

JAERI Nuclear Data Center

Japan Atomic Energy Research Institute (JAERI),

Tokai-Mura 319-11, Japan

The Atomic Energy Levels Data Center (NIST), the Data Center on Atomic

Transition Probabilities and Line Shapes (NIST), and the Nuclear Data Center

(JAERI) critically review, compile, and disseminate data on energy levels,

wavelengths, and transition probabilities for the spectra of atoms and atomic ions

in all stages of ionization. The NIST data centers also publish annotated

bibliographies and maintain files on bibliographic references categorized by

element, stage of ionization, and technical content. Energy-level data have been compiled during the past fifteen years for all spectra of the elements Na through S (Z=ll-16) [1-6], the iron-period elements K

through Ni (Z= 19-28) [7], all spectra of Cu, Kr, and Mo (Z=29, 36, 42) [8-10], and 63

spectra of the rare-earth elements La through Lu (Z=57-71) [11]. New energy level compilations are being completed for 0 II (Z=8) and all spectra of CI, Zn, and Ge

(Z= 17, 30, 32).

*Work is supported in part by the Office of Fusion Energy of the U.S. Department of Energy

and the Astrophysics Division of the U.S. National Aeronautics and Space Administration.

183
184

New wavelength compilations based on these energy level data have been

published for all spectra of Mg [12], Al [13], and Sc [14], in all wavelength regions

from x-rays to the far infrared being covered. Work is now in progress on 0 II (Z=8), Na, Si, and S (Z=ll,14,16).

Recent critical compilations of atomic transition probabilities cover the irongroup elements Sc through Ni (Z=21-28) [15,16]. Also, a recent update of the tables

previously published in the CRC Handbook of Chemistry and Physics [17] contains

about 8300 selected lines of all elements for which reliable data are available,

mostly for neutral and singly ionized atoms. A critical compilation of prominent

lines of neutral and singly ionized heavy atoms is now being updated, and work is

also continuing on evaluating data for the light atoms and ions, H through Ne

(Z=l-10). For these spectra, calculations from the "Opacity Project" [18] play a

major role.

In collaboration with JAERI, new compilations containing energy levels,

wavelengths, transition probabilities, and Grotrian diagrams have been published

for the higher spectra of V (V VI-XXIII) [19], Fe (Fe VIII-XXVI) [20], Co

(Co VIII-XXVII) [21], Ni (Ni IX-XXVIII) [22], Cu (Cu X-XXIX) [23] and Uo

(Mo VI-XLII) [24]. Work has been completed on Cr and Mn and will be published

soon.An interactive PC database [25] has been developed by the Standard Reference

Data Program at NIST containing prominent air or vacuum wavelengths and

ionization potentials for neutral through quadruply ionized atoms. The

wavelength data originally appeared in NSRDS-NBS 68 [26] and are reprinted

annually with updates in the "CRC Handbook of Chemistry and Physics" [27].

Also, a PC database containing the NIST transition probability tables for Sc

through Ni [15,16] is available [28]. Work is continuing at NIST on a general

atomic spectroscopic database containing evaluated data on atomic energy levels,

wavelengths, line classifications, and transition probabilities, covering many

atoms and ions of laboratory and astrophysical interest.

References

[1] W. C. Martin and R. Zalubas, J. Phys. Chem. Ref. Data 10, 153-195 (1981).

[2] W. C . Martin and R. Zalubas, J. Phys. Chem. Ref. Data 9, 1-58 (1980).

[3] W. C. Martin and R. Zalubas, J. Phys. Chem. Ref. Data 8, 817-864 (1979).

[4] W. C. Martin and R. Zalubas, J. Phys. Chem. Ref. Data 12, 323-^80 (1983).

[5] W. C. Martin, R. Zalubas, and A. Musgi-ove, J. Phys. Chem. Ref Data 14, 751-802 (1985).

[6] W. C. Martin, R. Zalubas, and A. Musgi-ove, J. Phys. Chem. Ref Data 19, 821-880 (1990).

[7] J. Sugar and C. Corliss, J. Phys. Chem. Ref Data 14, Suppl. No. 2 ( 1985).

[8] J. Sugar and A. Musgrove, J. Phys. Chem. Ref Data 19, 527-616 (1990).

[9] J. Sugar and A Musgrove, J. Phys. Chem. Ref Data 20, 859-915 (1991).
W. C. Martin et al. 185

[10] J. Sugar and A. Musgrove, J. Phys. Chem. Ref. Data 17, 155-239 (1988).

[11] W. C. Martin, R. Zalubas, and L. Hagan, Natl. Stand. Ref. Data Ser., Natl. Bur. Stand. (U.S.)

60, (1978).

[12] V. Kaufman and W. C. Martin, J. Phys. Chem. Ref. Data 20, 83-152 (1991).

[13] V. Kaufman and W. C. Martin, J. Phys. Chem. Ref. Data 20, 775-858 (1991).

[14] V. Kaufman and J. Sugar, J. Phys. Chem. Ref. Data 17, 1679-1789 (1988).

[15] G. A. Martin, J. R. Fuhr, and W. L. Wiese, J. Phys. Chem. Ref. Data 17, Suppl. No. 3 (1988).

[16] J. R. Fuhr, G. A. Martin, and W. L. Wiese, J. Phys. Chem. Ref. Data 17, Suppl. No. 4 (1988).

[17] J. R. Fuhr and W. L. Wiese, Atomic Transition Probabilities, CRC Handbook of

Chemistry and Physics, 72nd Edition (CRC Press, Boca Raton, FL, 1991).

[18] M. J. Seaton, J. Phys. B 20, 6363 (1987) and later Opacity Project papers in that journal.

[19] T. Shirai, T. Nakagaki, J. Sugar, and W. L. Wiese, J. Phys. Chem. Ref. Data 21, 273-390

(1992).

[20] T. Shirai, Y. Funatake, K. Mori, J. Sugar, W. L. Wiese, and Y. Nakai, J. Phys. Chem. Ref.

Data 19, 127-275 (1990).

[21] T. Shirai, A. Mengoni, Y. Nakai, J. Sugar, W. L. Wiese, K. Mori, and H. Sakai, J. Phys.

Chem. Ref. Data 21, 23-122 (1992).

[22] T. Shirai, K. Mori, J. Sugar, W. L. Wiese, Y. Nakai, and K. Ozawa, At. Data Nucl. Data

Tables 37, 235-332 (1987).

[23] T. Shirai, T. Nakagaki, Y. Nakai, J. Sugar, K. Ishii, and K. Mori, J. Phys. Chem. Ref. Data

20, 1-81 (1991).

[24] T. Shirai, Y. Nakai, K. Ozawa, K Ishii, J. Sugar, and K. Mori, J. Phys. Chem. Ref. Data 16,

327-377(1987).

[25] NIST Spectroscopic Properties of Atoms and Atomic Ions, NIST Standard Reference

Database 38.

[26] J. Reader, C. H. Corliss, W. L. Wiese, and G. A. Martin, Natl. Stand. Ref. Data Ser., Natl.

Bur. Stand. (U.S.) 68 (1980).

[27] J. Reader and C. H. Corliss, Line Spectra of the Elements , CRC Handbook of Chemistry

and Physics, 72nd Edition (CRC Press, Boca Raton, FL 1991).

[28] NIST Atomic Transition Probabilities (Scandium through Nickel), NIST Standard

Reference Database 24.
lit Need for Complete Spectroscopic Tables

Vivek Bakshi, Tom D. Boone, Jr., and William C. Nunnally

The Applied Physical Electronics Research Center

The University of Texas at Arlington

Arlington, TX 76019 (817) -- 794- 5100

(1) Abstract

This paper discusses the need for complete spectroscopic tables, i.e., for a given

species, listing of all transition arrays and the

transitions, combined with the values of transition probabilities and the line shape information, if possible. The presently available tables list only

prominent transitions and transition probability values for only some of these transitions. However,

in the case of spectra from some plasma devices one needs to analyze the weaker transitions for the estimation of plasma properties and hence arises the need for complete spectroscopic tables.

(2) Background

(2.1) Need for Atomic Data Base Plasma spectroscopy is a commonly used

and powerful diagnostics tool for the estimation of the plasma properties in various laboratory

plasmas, e.g., plasma jets, low pressure

discharges, plasma armature railguns, and

astrophysical plasmas. We, at The Applied

Physical Electronics Research Center, The

University of Texas at Arlington, have been

interested in the development of spectroscopic

diagnostics of the railgun plasma armatures. The

railgun operates at atmospheric pressure and the plasma emits spectra that are a combination of

optically thin and thick regions. The major

constituents of the plasma have been copper, aluminum, oxygen, and nitrogen in various

ionization stages. In a recent publication[l], we

have shown that prominent transitions are

optically thick in our experiment and the attention must be turned to otherwise weaker transitions,

which are still optically thin. Such transitions allow us to use the relations of emission

spectroscopy for the estimation of the plasma

parameters, which are less involved than the

optically thick plasma calculations. The

importance of weaker transitions can be important

even in the case of optically thin plasmas where

they may distort the line shapes of prominent

transitions being used for the calculation of

electron density, e.g., distortion of line shapes of hydrogen beta transitions by the transitions of 0 II and Si III, which can cause the error in the order

of magnitude in the electron-density

measurements[2]. For the same reasons, the presence of such transitions can also be important

in the choice of transitions in the optically thick

spectra. In short, the presence of such weak

transitions can distort the line shape of the prominent transitions and also introduce error in the measurements of the area under the

transitions. In order to detect the presence of such

weaker transitions and to be able to use them one

needs their listing. Also, in order to obtain plasma

parameters from the spectra the transition probability and line shape information is necessary.

In some experimental situations, where

spectral data must be acquired in a single shot, one tries to cover the wide wavelength region in order to be able to use a Boltzmann plot with reasonable accuracy and may lose the resolution in

this process. For example, in our experiment the wavelength resolution is only 0.6 Angstrom. At

this resolution and in the presence of four or five elements in various ionization stages the acquired

spectra have at least two hundred overlapping

lines in the 40 nm wavelength region and are

quite complex. For such spectra, in order to have

a reliable identification of the weaker transitions it

is quite important to have the complete

spectroscopic information for Cu I and II and Al I and II.

(2.2) Present state of data bases The atomic energy center at NIST

provides, at user's request, a bibliography of all the published work on energy levels, wavelengths,

transitions probability, and line shapes which is

' Paper presented at 4th International Colloquium on Atomic Spectra and Oscillator Strengths for Astrophysical and Laboratory Plasmas, September 14 - 17, 1992, National Institute of Standards and

Technology, Gaithersburg, MD, USA

186
Vlvek Bakshi et al. 187

quite complete and very helpful. Some NIST

publications[3] and CRC handbook [4] give

listings of the prominent transitions of many

elements. MIT press also has an extensive but not complete listing of wavelengths for many atoms and their atomic species which is useful [5]. There

exists in some cases a close to complete listing of

all the transitions in the literature, e.g., Shenstone's work for copper [6]. At present, atomic transition probability values are listed for prominent transitions only in NIST [3] publications or CRC handbook [4] and

NIST may provide more of such tables in the coming years.

transitions. The new wavelengths were also predicted according to the new energy levels. The

forbidden transitions were listed separately. The

transition probability values were then calculated according to Coulomb approximation. Stark widths of the transitions were estimated by using a SE formulation, however, the results are not included in this presentation.

(3.2) Some results Table I gives the typical results for some

transition array of Cu I. Entire table in the wavelength region (300 - 350 nm) will be

published soon.

(3) Complete Spectroscopic Tables

for Cu I and II

(3.1) Procedure for compilation

As explained in the section (2.2), we

needed to have complete spectroscopic tables for Cu I and II in the wavelength region of 300-350

nm. We have compiled such tables. We started with Shenstone's tables[6] and numbered all the multiplets and transition arrays. The next step was

to correct the energy levels by the new level information [7] and then predict the other possible

(4) Conclusions

(4.1) Summary of needs

There exists a need for complete

spectroscopic tables. The best way will be to have

a computerized data base combined with curve

fitting and calibration programs. These data bases will give a definite boost to the application

of plasma spectroscopy in the study of various plasma devices and astrophysical plasmas.

Table 1 : Example d Proposed Tables for Copper I

No. Transition Multiplet X(A) X,(A) Ei(cm)-1 E^(cni)-1 strengths strengths Ak,(s)->

Array

obsen'ed calculated -ii- (multiplet) (line)

1 - 2d 3498.938 3498.99 46598.34 75170.25 6 6 10 0.5600 3.60E+06

3d^4s{3D)6s 3447.59 3447.64 46172.84 75170.25 4 6 10 0.0400 2.50E+05

3362.12 3362.24 46598.34 76332.30 6 4 10 0.0400 4.90E+04

3314.82 3314.81 46172.84 76332.30 4 4 10 0.3600 3.60E+05

2 3d^(2D)4s4p(3p°) - 3498.063 3498.10 43513.95 72093.08 8 8 112 0.0407 7.50E+06

3d^4s(3D)4d 3475.999 3476.04 44544.15 73304.67 4 6 112 0.0029 2.40E+05

3474.578 3474.62 44544.15 73316.46 4 4 112 0.0400 4.80E+06

3459.428 3459.46 44406.27 73304.67 6 6 112 0.0521 4.20E+06

3599.140 3599.17 43513.95 71290.54 8 10 112 0.3571 7.80E+07

3610.809 3610,84 44406.27 72093.08 6 8 112 0.0021 3.90E+05

P 3355.84 43513.95 73304.67 8 6 112 0.2450 1.90E+07

P 3458.05 44406.27 73316.46 6 4 112 0.1607 1.90E+07

3520.031 3520.06 44915.61 73316.46 2 4 112 0.1000 1.20E+07
188

(4.2) Suggestions for Future Work in the Area of Atomic Data-Base

(1) The first step would be the compilation of energy levels for all of the useful atoms and their

ions. The experimental and theoretical studies contributing to this step are very important.

(2) When energy levels are available, one can

proceed to the second step of predicting all of the

transitions in a transition array. Such predictions

for allowed transitions are straightforward in the case of LS coupling but in other cases they are quite complex. There is no reliable technique for the prediction of forbidden transitions that works

for all elements. In our work the compilation of forbidden transitions is restricted to observed

transitions only.

(3) The next step will be the theoretical calculation and experiment measurement of the

transition probabilities and line shape information

for these transitions and critical evaluation of

transition probability and line shape information

(4) The availability of such information for convenient user interaction is also very important.

(5) Acknowledgement

This work is sponsered under SDIO-US ARMYSDC contract No. DASG60-90-C-0133

(6) References

[1] Vivek Bakshi et al, " Spectroscopic

Diagnostics of Railgun Plasma Amiature," To be

published in IEEE Trans. Magnetics, Jan 93.

[2] Vivek Bakshi et al, "Plasma Diagnostics of Railgun Armatures," Resubmitted to IEEE Trans. Plasma Science, August 1992.

[3] (a) Joseph Reader and Charles H. Corliss (Part

I: Wavelength) and W. L. Wiese and G. A. Martin

(Part II Transition Probability), Wavelength and

Transition Probability for Atoms and

Atomic Ions, NSRDS-NBS 68, Institute of Basic

Standards, NBS, Washington, DC, December

1982.

(b) W. L. Wiese, M. W. Smith, and B. M. Miles,

Atomic Transition Probability , Volume I

Hydrogen Through Neon, NSRDS-NBS 4, Institute of Basic Standards, NBS, Washington, D. C, October 1969.

[4]Robert C. Weast and Melvin J, Astle, CRC

Handbook of Chemistry and Physics, CRC

Press Inc., Boca Raton, Florida 1982.

[5]MIT Wavelength Tables, vol. I by George

R. Harrison (1969), vol. II by Federic M. Phelps

(1982), MIT Press, Cambridge Press, Cambridge,

MA.

[6]'The first Spectrum of Copper (Cu I)," A. G.

Shenstone, Phil. Trans. R. Soc. London, Ser. A,

241 37 (1948).

[7]"Energy Levels of Copper, Cu I through XXX,"

J. Sugar and A. Musgrove, J. Phys. Chem. Ref. Data 19, 527-616 (1990).
Spectral Atlas of the Inductively Coupled Plasma

R.K. Winge, D.E. Eckels, and S.J. Weeks

Ames Laboratory, Iowa State University, Ames, lA 50011

and

J.C. Travis and M.L. Salit

National Institute of Standards and Technology, Gaithersburg, MD

ABSTRACT

Introduction - Needs: Analytical atomic

spectrometry and astrophysics share common

needs. Both fields require a means of positive

identification of spectral lines, lines that are

often masked or blended with other lines. Both

fields also require line intensities and often other

analytic information, e.g., temperatures and line

widths that define the excitation characteristics

of the source. Sample elements in the

inductively coupled plasma (ICP) experience

temperatures similar to those existing in the

photospheres of our sun and cool stars, thus

suggesting diagnostic applications for the ICP in

astrophysics.

The ICP is used extensively as a hightemperature atomization-excitation source for

atomic emission spectrometry (AES) and

elemental mass spectrometry (ICP-MS). The

ICP is an efficient source of spectral lines arising

from the singly ionized state (M"^) and this

characteristic provides many strong ion lines

suitable for the measurement of trace

concentrations of the elements in AES [1]. The

enhancement of ion line intensities relative to atom line intensities in the ICP is only one among a number of differences that lead to the

need for a new compilation of spectral data.

Existing spectral line compilations include

deficiencies in one or more of the following

quaUties in relation to the ICP:

1. Spectral line coverage. Gaps exist in

wavelength coverage for many elements

[2]. Deficiencies in weak line coverage

exist throughout the spectrum.

2. Availability in machine readable form.

3. Capability for graphical representation

of spectra.

4. Wavelengths, intensities, and peak

widths relevant to the ICP.

5. Wavelength accuracy sufficient so that specific spectral lines can be located

reliably within a narrow window in

computer controlled routines.

The present work addresses these needs for

>70 elements. The project combines the

wavelength accuracy of Fourier Transform

Spectrometry (FTS) at NIST with the dynamic

range of wavelength dispersive spectrometry at the Ames Laboratory. The latter employs a conventional scanning spectrometer with a photodiode array detector. ICP as an Emission Source: The ICP

employed for analytical emission spectrometry

is typically operated at 27 MHz or 40 MHz at power levels of approximately 1 to 1.2 kW.

Elements of interest are introduced into the axial

channel of the ICP as aerosols of liquid or solid

samples. The aerosols are desolvated (liquids),

vaporized, atomized, and excited, or ionized and

excited as they progress along the axial channel

where gas kinetic temperatures reach 5000 to 7000 K. The degree of ionization of elements in the ICP has been estimated from the Saha

equation by Houk [3]. These calculations

indicate some 54 elements are expected to reach

the first ionization level with efficiencies at 90% or higher. The calculations also indicate

appreciable fractions of doubly ionized species

M^"^ in the ICP for elements with relatively low

second ionization energies. The results of these

calculations coincide closely with experimental

observations, that the most prominent lines for

many elements in the ICP arise from singly

ionized species and that lines from doubly

ionized species are observed for the predicted

elements. The axial sample channel in the ICP

is surrounded by an annular induction region

with a temperature of approximately 10000 K.

Thus, the ICP is an optically thin emission

source exhibiting excellent linearity between

intensity and concentration over approximately

five orders of magnitude.

Experimental Facilities: Spectral data

for each element are collected with aim

scanning spectrometer equipped with a 3600

grooves/mm grating and a 1024 pixel,

photodiode array. The spectrometer is stepped

through a fixed series of computer controlled

189
190

grating angles that allow coverage of the 187 to 434 nm range in 62 overlapping windows (25%

overlap). The wavelength range included in the

window changes with grating angle from -6.4

nm at 189 nm to -3.9 nm at 432 nm. The 1024

pixel array thus samples the spectrum at intervals varying from 6 pm to 4 pm (0.06 to 0.04 A) as the spectrometer progresses through

its stepped sequence of windows. Peak

positions (interpolated diode array pixel

positions), intensities, and widths (FWHM) are obtained from a three-point Gaussian curve

fitting routine. Wavelengths corresponding to peak pixel positions are obtained from the

grating equation, which, in contrast to polynomial curve fitting, requires only one

reference wavelength per diode array window.

Wavelength accuracies on the order of 0.1 pm

are obtained, relative to NIST FTS wavelengths,

after correction for an optical aberration

associated with off-axis rays. Another small but

systematic error (tenths of a picometer), arising

presumably from another optical aberration, occurs at one end of the wavelength range. It is presently under investigation. The dynamic

range of measurable intensities is extended to 5

to 6 orders of magnitude by a combination of

three diode-array measurement conditions

(exposure times of 0.03, 0.3, and 3.0 s; total

integration time of 15 s each) and three

elemental concentrations (10, 100, and 1000

mg/L) for each element.

Summary of Results: Table 1 provides an example of the wavelength accuracy,

expressed as wavelength differences, achieved

with the Ames Laboratory instrumentation with

respect to NIST FTS wavelengths. The 12 iron

lines, measured within one diode array window

with a sample concentration of 1000 mg/L,

yielded an RMS error of 0.08 pm. The RMS

error values for 100 and 10 mg/L iron were 0.09

and 0.12 pm, respectively. Thus, excellent

wavelength accuracy is maintained over a wide

intensity range. A segment of the ICP iron emission

spectrum is compared with an absorption

spectrum of star R 81 [4] in Fig.l. The relative

intensities and positions of the major features in the ICP spectrum correlate closely with the

major absorption peaks in the star spectrum.

The need and usefulness of an ICP atlas is apparent for analysis in astrophysical

measurements, as it is in the field of analytical

chemistry.

References

1. Winge, R.K., Fassel, V.A., Peterson, V.J.,

and Floyd, M.A., "Inductively Coupled

Plasma-Atomic Emission Spectroscopy: An

Atlas of Spectral Information," Elsevier

(1985).

2. Boumans, P.W.J.M., Spectrochim. Acta,

43B,5 (1988)

3. Houk, R.S., Anal. Chem. 58, 97A (1986).

4. Zickgraf, F.-J., "Fe II in Luminous Hot

Stars", p.l25 in "Physics of Formation of Fe

II Lines Outside LTE", Viotti, R., Vittone,

A., and Friedjung, M,, Eds., D. Reidel

PubUshing Company, Dordrecht (1988).

Table 1 . Differences between Ames Laboratory

calculated wavelengths and NIST FTS

wavelengths

NIST?i NIST

(nm) Rel. Int. (pm)

256.69133 41 -.06 257.79225 45 .10

258.25838 65 -.03 258.58762^ 764 0. 259.15435 67 .07 259.83696 876 .15 259.93958 2470 .04

260.70875 727 .14

261.18740 1045 .04 261.38247 432 .07 261.76178 302 .02

262.16695 110 .01 RMS error^ .08

^ AX = X^ - Xffisj

Reference wavelength with inherent zero

error. ^The zero error value for the reference

wavelength is excluded.
R. K. Winge et al. 191

10\

(Aa

© ,

e

>

10^

10^

R 81 lUE. LWR

1982. Feb. 17

B B

B

261?. kiJj 2SS.

261 262

Wavelength (nm)

263

Figure 1 . Comparison of the ICP emission spectrum of iron (bottom) with the

absorption spectrum of R 81 (top). MIT table wavelengths are listed below for

the lines numbered in the ICP spectrum. Upper pan of figure reproduced with

pcmiission of author and publisher [4].

1. 2.3.4.

5.

6.

II 260.9866

II 261.1072

II 261.1872

II 261.3823

II 261.4872

261^422

7.8.

9. 10. II.

12.

II 261.7616

I 261.8017

II 261.9076

II 262.0173

II 262.0407

II 262.0695

13. II 262.1668

14. 262.3123

15. 1 262.3532

16. II 262.3727

17. 262.5490

18. II 262.5666

19. 20.

21. 22.

23.

24. 25.

II 262.6500

II 262.8292

Ml 262.9587

II 263.0066

II 263.1051

II 263.1323

II 263.1609
Atomic Data Center for Astrophysical and Laboratory Plasmas

K. T. Lu, Dennis Baba and Aria Kohshkhou

Atomic Engineering Coi-p., P. O. Box 3342, Gaithersburg, MD. 20885-3342

The astrophysical and laboratory plasmas scientists rely on atomic spectra to determine

temperature, electron density and element abundance. The scientists often spend hours leafing

through pages of wavelengths and energy levels in atomic data books, seeking an unidentified

spectral line. Unfortunately, the usual wavelength tables are not fully adequate . They are too

incomplete compared to the actual spectra. The wavelength lists and intensities available fi*om

different sources are not consistent with each other because they are measured under different

experimental conditions. Furthermore, the tabulated data on wavelength, transition probability

and energy level are not integrated. All these problems make the evaluation and compilation of

data using traditional methods difficult, if not impossible.

This paper describes a software program, Atomic Engineering System ( AESystem)', which can be used as a data center for astrophysical and laboratory plasmas. The AESystem can analyze

and identify spectroscopic data. FurtheiTnore, it can integrate and evaluate atomic/ionic data,

model experiments, and plot a variety of data.

o Automated Spectroscopic Analysis : AESystem can perfomi element identification and analysis of the spectra. The basic idea is to model a complete reference wavelength spectra using Atomic Engineering System. This

complete reference wavelength spectra will be compared with the actual spectra. Atomic

selection rules will be used to control the type of lines generated (e.g., allowed, forbidden,

multiphoton). The user can enter a single line from keyboard or a list of lines from a file. The

software program searches the database which consists of evaluated experimental data and the

complete reference spectra for pairs of energy levels that can produce the frequency within a specified tolerance. This search can be done over many elements or ions at once. It is a useful

feature for astrophysics and plasma spectroscopy where the source may include many

elements/ions. A demonstration will be presented at this conference.

o Computer Modeling of Absorption and Emission Spectra : The AESystem contains an integrated database. The data processed include: energy levels,

ionization limits, oscillator strengths, intensities, Lande-g-factors, photoionization cross sections,

frequencies or wavelengths, life-times. The source of these data are NIST compilations of

atomic data, Kelly's tables on wavelengths, and the open literature. The basic data unit of this

data management is the "channel," which includes a series of related energy levels plus

information common to all members of the channel. The program organizes all channels of a given element or ion into a "super file" for easy access. The mathematical algorithm

characterizes an atom or ion in terms of a small sets of stmctural parameters and a finite number

of channel sets. The structural parameters are detennined either by semi-empirical method

(fitting to the data) or by first principle calculations. Many new data types can be calculated, once the structural parameters are known. Subsequently, only the stmctural parameters of each

atom need to be stored in a modeling experiment. This step makes it unnecessary to use a

192
K. T. Lu et al. 193

mainframe computer in managing and manipulating the vast amounts of data. Thus it is possible

to use PC as data center. A computer modeling of absolution and emission spectrum will be

demonstrated.

0 Evaluation and Integration of Data : The quantitative application of the AESystem in element identification and analysis of the

spectra depends on the reliability and completeness of the database. The data of Fe I from

NIST", Kelly's wavelength table\ and NRL^'as well as the latest data of life-time and transition

probabilities" will be used as a case study to examine the reliability and completeness of various

data. A generic data format has been developed to integrate the non-compatible data foiTnat of

wavelengths vs. transition probabilities with the data format of energy levels vs. life-time. A

user-f.iendly display allows user to select the desired data field to display. The following is the

procedures of evaluation and integration of data:

1. Convert each data files, such as reference 2 to 5, into a generic data file, 2. The algorithm compares each data field in different data files. For example, wavelength

2345.67 A from data file a is checked and compared to the same value within

a certain error with all the other data files, b, c etc. This procedure will be continued until all the data in one file are evaluated.

3. The evaluated wavelength data files are used as input to the automated spectroscopic analysis

module. The "spectra lines" are chemically analyzed and identified according to its element or ion origin, upper/lower energy levels, allowed or forbidden transitions and etc. 4. The data with different data fields are integrated by merging all the evaluated data files under

the generic data format. For example, data of wavelength vs. intensity, oscillator strength and

transition probability from data files a and b are integrated with data of energy levels vs. upper/lower energy levels and upper/lower life-time from files c and d.

Sample data of life-times, transition probabilities, and level energies and wavelength in Fe I are shown in the following tables to demonstrate the evaluation and integration of data. Reference 5

provides the most reliable and consistent data on transition probabilities and life time, because

data was taken under similar experimental conditions.

1 . J. J. Wynne and C. M. Brown, "Atomic Data Center on Your PC", p. 42, Optics and Photonics

News/July (1992).

2. (a) J. R. Fuhr, G. A. Martin, and W. 1. Wiese, "Atomic transition probabilities: Fe through

Ni," J. Phys. Chem. Ref Data 17, Suppl. 4 (1988).

(b) J. Sugar and C. Corliss, "Atomic energy levels of the iron-period elements: K through Ni,"

J. Phys. Chem. Ref Data 14, Suppl. 2 (1985).

3. R. L. Kelly, "Atomic and Ionic Spectrum Lines Below 2000 A: Hydrogen through Krypton,"

J. Phys. and Chem. Ref Data, 17, Suppl. 1, (1987).

4. C. M. Brown, M. L. Ginter, S Johansson and S. G. Tilford, "Absorption spectra of Fe I in the

1550-3215 A region," J. O. S. Am. B 5, (1988).

5. T. R. O'Brian, M. E. Wickliffe, J. E. Lawler, W. Whaling and J. W. Brault, J. 0. S. A. B., V.

8, 1185, (1991).
194

Elm V?l ( air) EUx 10

3 cm- 1 UTerm Trans . Prob

S p e c

1 Wl(air) Ref ELxl0' 3 cm- 1 LTe rm ref

Fe 11689 .973 26479 .3770 z5D* 1 . 00 1 . 39E + 05

(

; 11%)

1 17927 .3770 a5P 1 . 00

Fe 11638 .256 26140 .1777 z5D* 3 . 00 4 . 30E + 04(. 10%)

1 17 5 50 .1758 a5P 3 .00

Fe 11607 .574 26339 .6934 z5D" 2 . 00 9 . 70E + 04(: 11%)

1 17726 . 9863 a5P 2 .00

Fe 11593 . 584 26550 .4746 z5D" 0 .00 1 . 77E + 05

(

15%)

1 17927 .3730 a5P 1 . 00

Fe 11439 .120 31686 .3496 z3D" 2 . 00 1 . 81E + 05([ 9%

)

1 22946 .8105 b3P 1 . 00

Fe 11422 . 322 26479 .3770 z 5 D ' 1 . 00 3 . 40E + 04(.11%)

1 17726 . 9844 a5P 2 .00

Fe 11374 .079 26339 .6934 z 5 D

" 2 . 00 6 . 00E + 03(, 13% ) 1 17 5 50 .1797 a5P 3 . 00

Fe 11298 . 854 31686 .3496 z3D" 2 . 00 2 . 70E + 04(; 10%)

1 22838 .3164 b3P 2 . 00

Fe 11251 .111 31937 .322 3 z 3D* 1 . 00 1 . 1 3E + 05

; 10%)

1 23051 . 7441 b3P 0 . 00

Fe 11119 .789 31937 .3223 z 3 D 1 . 00 1 . 1 3E + 05

; 11%)

1 22946 .8086 b3P 1 .00

Fe 9889 . 042 50703 .8633 e5G 5 . 00 2 . 22E + 06(; 26%)

1 40257 . 3086 x5 F

" 4 .00

Fe 9861 .735 50979 .5742 e5G 4 .00 5 . 49E + 06

; 2 6%)

1 40842 . 1484 x5F" 3 . 00

Fe 9763 . 380 51370 . 1406 e5G 2 .00 5 . 42E + 06

; 21%)

1 275 59 .5801 z5F" 2 .00

Fe 9738 .573 50522 . 9414 e5G 6 . 00 7 . 65E + 06

; 30%)

1 40257 . 3086 x5F" 5 . 00

Fe 9626 .494 50979 .5742 e5G 4 . 00 4 . 51E + 06(; 26%)

1 40594 .4258 x5F " 4 . 00

* Fe 9569 . 909 50703 .8633 e5G 5 . 00 2 . 50E + 06

(

21%)

1 40594 .4258 x5F* 5 . 00

Fe 9443 . 803 51604 .1016 f 5F 3 . 00 6 . 39E + 06

(

;2i%)

1 41018 .0469 x5F" 2 . 00

Fe 9414 . 041 514 61 .6680 f 5F 4 . 00 3 . 98E + 06

(

35%)

1 40842 . 1484 x5F* 3 .00

* Fe 9401 .112 51228 . 5469 e7G 5 . 00 2 . 64E + 06(.21%)

1 34039 .5117 y5F" 4 .00

Fe 9372 .897 31307 .2422 z3F" 4 .00 2 . 05E + 04(.13%)

1 20641 . 1094 b3F 4 .00

Fe 9362 . 360 29056 . 3203 z5P* 3 . 00 7 . 66E + 03( 31%)

1 18378 . 1836 a3P 2 . 00

tu ( n s

)

tl(ns)

I 86 . 300

81 . 100

84 .500

88 . 500

245 .000

86 . 300

84 .500

245 .000

237 . 000

237 .000

11 . 500

2 .000

12 . 800

2 . 000

10 . 300

2 .000

13 .000

2 . 000

12 . 800

2 .000

11 . 500

2 .000

14 . 800

2 . 000

12 . 700

2 . 000

7 . 800

7 . 700

Revi sed Data

Transition Probabilities and Life-Ti:;:es are from reference 5
Author Index

A

Adelman, S. J., 99

Ali, M. A., 162

Artru, M.-C, 93

Azarov, V., 119

B

Baba, D., 192

Bakshi, V., 186

Baliyan, K. S., 4, 31

Barbee, Jr., T. W., 148

Bastert, A., 122

Beideck, D. J., 47

Bhatia, A. K., 4

Biemont, E., 3, 26

Bieron, J. R., 29

Boduch, P, 136, 139

Boone, Jr., T. D., 186

Bowyer, S., 96

Boyer, C. N., 148

Brault, J. W., 40, 71

Brekke, P., 83, 111

Brown, C. M, 145, 148

Bukow, H. H., 122

Bye, C. A., 37

C

Calamai, A. G., 59

Carlsson, M., 114

Chantepie, M., 136, 139

Chantler, C. T., 23

Chen, X., 37

Church, D. A., 44

Cremer, G., 139

D

Dalton, G. R., 183

Doerfert, J., 50

Druetta, M., 136, 139, 151

Duffer, T., 37

E

Eckels, D. E., 189

Ekberg, J. O., 13

EUis, D. G., 47

Engleman, R., 40

Escalante, V., 62

F

Federman, S. R., 47

Feldman, U., 91, 145

Fischer, C. F., 171, 174

Fremont, F., 139

Fuhr, J. R., 183

G

Gillaspy, J. D., 145

Glass, G. A., 142

Godefroid, M. R., 26

Goldbach, C, 77

Gongora, A., 62

Granzow, J., 50

Guardala, N. A., 142

Gulliver, A. F., 99
H

Hammel, B. A., 134

Hansen, J. E., 3

Harra, L. K., 68

Hauschildt, P. H., 108

Heckmann, P. H., 50

Helbig, v., 65

Hennecart, D., 136, 139

Hibbert, A., 16, 26

Hicham, S., 139

Hitz, D., 151

Holland, G. E, 148

Honda, Y., 19

Hubeny, I., 93

Hunter, W. R., 148

Husson, X., 136, 139

J

Jacobs, V. L., 22

Jacquet, E., 136, 139

Jin, J., 44

Johansson, S., 13, 56, 86, 88,

102, 128, 131

Jonsson, P., 174

Joshi, Y. N., 125

Joueizadeh, A. A., 13, 86, 131

Judge, P, 111, 114

K

Kagawa, T., 19

Kania, D. R., 134

Keane, C. J., 134

Keenan, F. P., 68

Kelleher, D. E., 65

Kim, Y.-K., 162

Kiyokawa, S., 19

Klose, J. Z., 41

Kohshkhou, A., 192

Kowalski, M. P., 148

Krenzer, M., 122

Krier, H., 37

Kushner, M. J., 37

Kwong, V. H. S., 59

L

Lakshmi, P. A., 31

Laming, J. M., 91

Land, D. J., 142

Lanz, T., 93

Larsson, J., 86

Lawler, J. E., 71

Learner, R. C. M., 154

Le Dourneuf, M., 93

Leckrone, D. S., 86, 88

Lecler, D., 136, 139

Lief, E. P., 159

Litzen, U., 56, 86, 102

Lu, K. T, 192

Lu, R., Ill

Liidtke, T., 77

Ludwig, P., 151

M

Msmning, L. W., 165

Martin, M., 77

Martin, W. C, 183

Mazumder, J., 37

McCann, S. M., 68

Migdalek, J., 29

Moller, G., 50

Mohanty, A. K., 177

Murray, J. E., 154

Musgrove, A., 183

N

Nahar, S. N., 7, 10

Nave, G., 128, 154

Nollez, G., 77

Nunnally, W. C, 186

O

O'Brian, T. R., 71

Osterheld, A. L., 134
p T

Parkinson, W. H., 59

Parpia, F. A., 171, 177

Persson, A., 86

Pickering, J., 154

Phillips, K. J. H., 68

Podobedova, L. I., 119

Pradhan, A. K., 7, 10, 111

Price, J. L., 142

Q

Quinet, P., 3

R

Raassen, A. J. J., 13

Rachlew-Kallne, E., 68

Radziemski, L. J., 40

Reader, J., 105, 183

Rice, J. E., 68

Rief, J. C, 148

Rieger, G., 122

Roberts, J. R., 145

Robinson, D. J. R., 16

Rosberg, M., 102

Ryabtsev, A. N., 119

S

Salit, M. L., 189

Sanders, F. C, 165

Sansonetti, C. J., 105

Schectman, R. M., 47

Scheeline, A., 37

Seely, J. F., 148

Shirai, T., 183

Simons, D. G., 142

Smith, P. L., 59

Srivastava, S. K., 74

Starrfield, S., 108

Stolterfoht, N., 136, 139

Stumborg, M. F., 142

Sugar, J., 183

Svanberg, S., 86

Tauheed, A., 125

Tchang-Brillet, W.-U. L., 119

Tewari, S., 37

Thorne, A. P., 154

Tong, M., 174

Trabert, E., 50, 53

Travis, J. C, 189

U

Uylings, P. H. M., 13

V

Vaeck, N., 26

Vennes, S., 96

Victor, G. A., 62

W

Wagner, C., 50

Wahlgren, G. M., 86, 88

Wang, Z., 168

Weeks, S. J., 189

Weisheit, J. C., 159

Whaling, W., 71

Wickliffe, M. E., 71

Wiese, W. L., 41, 65, 183

Wilson, M., 68, 136, 139

Winge, R. K., 189

Winkler, P., 168

Wyart, J.-F., 13, 119

Y

Yan, Y., 168

Z

Zeippen, C. J., 3

Zerkle, D., 37

Zhan, H., 168

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