Experimental Stark widths and shifts for spectral lines of neutral and ionized atoms A critical review of selected data for the period 2001–2007

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New Astronomy Reviews 52 (2009) 471–535 www.elsevier.com/locate/newastrev

Experimental Stark widths and shifts for spectral lines of neutral and ionized atoms A critical review of selected data for the period 2001–2007 q A. Lesage GEPI/UMR 8111, Observatoire de Paris, 92195 Meudon Cedex, France Accepted 7 January 2008 Available online 2 March 2008

Abstract A critical review of the available experimental data on Stark widths and shifts for spectral lines of non-hydrogenic neutral atoms and positive ions has been carried out. The review covers the period from 2001 through the end of 2007 and represents a continuation of earlier critical reviews up to 2000. Data tables containing the selected experimental Stark broadening parameters are presented with estimated accuracy. Guidelines for the accuracy estimates, developed during the previous reviews, are summarized again. The data are arranged according to elements and spectra, and these are presented in alphabetical and numerical order, respectively. A total of 41 spectra are covered. Comparisons with comprehensive calculations based on semi-classical theory or on semi-empirical method are made whenever possible, since the comparison with theory has often been a principal motivation for the experiments. Ó 2008 Elsevier B.V. All rights reserved. Keywords: Critically evaluated data; Full-width-at-half-maximum intensity; Neutral atoms; Positive ions; Stark broadening parameters; Stark shifts; Stark widths

Contents PART I. INTRODUCTION . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 1. Introductory remarks . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 2. General discussion of our evaluation procedure . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 3. Comparisons with theory . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 4. Arrangement of the tables . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 5. Summary and conclusions . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 6. Appendix: Plasma sources . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 6.1. Stationary plasma sources . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 6.2. Pulsed discharges. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 6.3. Shock tubes . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 6.4. Laser-produced plasmas . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 6.5. Sources used since 24761, and not during the 1990–2000 period of time . . . . . . . . . . . . . . . . . . . . . .

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The present edition of ‘‘A Critical Review of Selected Data” continues the material already published in the Journal of Physical and Chemical Reference Data in 2002 (Konjevic´ et al., 2002). The data collected for the period from 2001 through end of 2007, has been evaluated and included in the present edition. The source of literature references has been the Atomic Spectral Line Broadening Bibliographic Database (Fuhr et al., 1998) and the data bases ‘‘BiblioPl@nets ERL WebSPIRS5” of ‘‘l’Institut de l’Information Scientifique et Technique” (INIST). E-mail address: [email protected] 1387-6473/$ - see front matter Ó 2008 Elsevier B.V. All rights reserved. doi:10.1016/j.newar.2008.01.001

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Appendix: Advanced procedures for the deconvolution of line profiles . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . Part II. DATA TABLES . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . Argon, Ar I . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . Argon, Ar II . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . Argon, Ar IV. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . Carbon, C I . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . Fluorine, F II . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . Fluorine, F III . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . Gold, Au II . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . Gold, Au III . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . Helium, He I . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . Indium, In III . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . Iron, Fe I . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . Krypton, Kr I . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . Krypton, Kr II. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . Lead, Pb II . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . Lead, Pb III. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . Magnesium, Mg I. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . Magnesium, Mg II . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . Manganese, Mn I . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . Manganese, Mn II . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . Manganese, Mn III . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . Neon, Ne I . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . Neon, Ne II . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . Neon, Ne III . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . Neon, Ne IV . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . Neon, Ne VIII . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . Oxygen, O II . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . Oxygen, O III . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . Oxygen, O IV . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . Silicon, Si II. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . Silicon, Si III . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . Silicon, Si IV . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . Silver, Ag I . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . Silver, Ag II. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . Silver, Ag III . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . Sodium, Na I. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . Sulfur, S III . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . Sulfur, S IV . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . Tin, Sn I . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . Tin, Sn II . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . Tin, Sn III . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . Xenon, Xe II . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . Xenon, Xe III . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . Note added in proof: neon, Ne II, and nitrogen, N II, data . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . Neon, Ne II . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . Nitrogen, N II . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . Acknowledgements . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . References . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

476 477 477 479 480 482 482 483 484 485 486 490 491 492 493 494 495 496 497 498 499 499 500 502 505 506 506 507 508 511 511 513 514 514 515 515 516 517 518 519 520 520 521 527 529 529 530 530 531

PART I. INTRODUCTION 1. Introductory remarks This tabulation is a continuation of a series of critical reviews and tables on experimental Stark broadening data for spectral lines of non-hydrogenic atoms and ions which started in 1976 (Konjevic´ and Roberts, 1976; Konjevic´ and Wiese, 1976) and continued in 1984 (Konjevic´ et al., 1984a,b), 1990 (Konjevic´ and Wiese, 1990), 2002 (Konjevic´ et al., 2002). Generally, we have adhered to the format of the previous reviews, and we have subjected the data again to the same evaluation criteria as established earlier.

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Our main source of literature references has been the master file (Fuhr et al., 1998) of the Data Center on Atomic Line Shapes and Shifts at the National Institute of Standards and Technology (formerly the National Bureau of Standards), the ‘‘Bibliography on Atomic Line Shapes and Shifts (Fuhr et al., 1972)” and the Digital Library for Physics and Astronomy (ADS). A principal reason for many Stark-broadening experiments is to provide comparisons for theoretical Stark width and shift data. We have therefore also presented comparisons with the generally successful and widely applied semi-classical theory or with the semi-empirical method. Another reason for such experiments is (especially for heavier and higher ionized elements) the importance of Stark broadening parameters in stellar atmosphere opacity calculations (Lesage, 1994; Dimitrijevic´ et al., 2007), and in the analysis of dense laboratory plasmas. 2. General discussion of our evaluation procedure We have evaluated and tabulated the two principal Stark broadening parameters obtained from the experiments: the full width of a spectral line at half maximum intensity (FWHM) and the shift of a line, usually determined at peak intensity. But in several cases the shifts are reported for the position of the halfwidth, and this is noted in the tables for these spectra. The shifts are listed as positive when they occur toward longer wavelengths (red shift), and as negative when they occur toward shorter wavelengths (blue shift). Detailed discussions of our evaluation procedure and of the adopted criteria have been provided in the earlier reviews (Konjevic´ et al., 2002; Konjevic´ and Roberts, 1976; Konjevic´ and Wiese, 1976, 1990; Konjevic´ et al., 1984a,b) and extensive literature references have been given there. Therefore, we only summarize below our principal criteria for the selection of the experimental results and for the estimates of the uncertainties: (a) The plasma source must be well characterized, i.e., it must be homogeneous in the observation region, be quasi steadystate during the observation time and must be highly reproducible. The last requirement is especially important for shotto-shot line scanning techniques with pulsed plasmas. A detailed listing of the applied plasma sources, their range of applications, power requirements, etc. is given in Appendix A of the 2002 issue introduction (Konjevic´ et al., 2002). Three properties of the plasma sources principally affect the accuracy of the Stark broadening data: the geometry of the source (especially its homogeneity or inhomogeneity and the presence or absence of boundary layers); its stability during the observation time; and its reproducibility (this is especially important for pulsed sources, when shot-to-shot scanning techniques are used). These features are discussed in some detail in the references of Appendix 6. (b) The electron density in the observed plasma region must have been determined accurately by an independent method (i.e., a method other than utilizing the Stark broadening of the investigated lines). (c) A temperature determination with an accuracy similar to that for the electron density must have been carried out. (d) Competing line broadening and shift mechanisms must have been considered, such as Doppler, van der Waals, and instrumental broadening and their contributions must have been estimated and subtracted. A discussion of recent line shape deconvolution techniques, especially for the slightly asymmetric profiles of neutral atoms, is given in Appendix 7. (e) Optically thin conditions must prevail at the line centers, or appropriate corrections must be made. Also, inhomogeneous plasma boundary layers must be either eliminated by appropriate experimental arrangements or must be taken into account in the uncertainty estimates. We have generally found that in the large majority of the experiments, the above listed critical factors (a)–(e) have been addressed. Occasionally, one of the factors, like the measurements of the plasma temperature or the effects of plasma endlayers has not been discussed and we have either noted this in the tables which list ‘‘Key data on experiments,” or have commented on this in the introduction to the pertinent spectrum. In the present review, contrary to what has been done in the previous ones, there are data which are included in the present issue, even if the published results do not fulfill all the above mentioned criteria. Such results are clearly identified and commented. Two reasons explain why they are not rejected: first because they are published in refereed journals considered by the majority of the scientists as being of high level and second because of the astrophysical interest of the studied elements. 3. Comparisons with theory Whenever theoretical data are available, we have provided comparisons with the semi-classical theory developed by Griem et al. (1962) in 1962 or with semi-empirical method. For neutral atoms and singly-charged ions, the semi-classical results by Griem (1974) are normally used. For a few exceptions the source of the theoretical data is clearly noted. For multiply charged ions the results of another semi-classical perturbation mechanism (Sahal-Bre´chot, 1969a,b) are used. This

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approach was then modified and extended, especially by Sahal-Bre´chot, and Dimitrijevic´, and a large number of additional numerical results were provided by these authors (see the NBS/NIST bibliographies on spectral line broadening (Fuhr et al., 1998; Fuhr et al., 1972) for numerous references). The ratios of measured-to-calculated widths and shifts tabulated by us for the various spectra provide guidance on the degree of agreement between the experiments and theory, and thus provide a valuable indication of the quality of the calculated as well as measured data. It is seen that for most transitions, the semi-classical calculations compare well with the experimental data, which was also observed in the earlier reviews. We should note that the theoretical width data for ionic radiators are for the electron width only, and the usually very small additional width caused by ion broadening is neglected. Also, small shifts contributed by ions are neglected in the theoretical shift data for ionic radiators. 4. Arrangement of the tables The data are presented in separate tables for each spectrum (or stage of ionization) and the spectra are arranged according to chemical elements, which are given in alphabetical order. Each data table is preceded by short comments providing important information on the selected literature and by a short tabular overview providing some key points on each selected experiment, such as the type of plasma source employed. For spectra containing more than 20 transitions, we provide a finding list where the selected lines are given in order of increasing wavelength. The data tables are subdivided into four principal parts. In the first part, which comprises three columns, each spectral ˚ ngstrom units). line is identified by transition array, multiplet designation (wherever available), and wavelength (given in A The wavelengths are usually taken from the ‘‘Atomic Spectra Database (ASD)” by NIST or, in a few cases, from more recent NIST compilations (Musgrove et al., private communications) or the earlier data tables of Striganov et al. (1966). In the second part of the table, the principal plasma data are listed. Normally, these are the ranges of temperatures and electron densities at which the width and shift data have been measured. However, in a number of papers the authors have not listed the actual electron densities at which the measurements were made, but have presented their data scaled to nominal electron densities of 1016 cm3 (mainly for neutrals) or 1017 cm3 in order to facilitate comparisons with theory. We have always listed the electron densities in units of 1017 cm3. In the third part of the table, we present the measured Stark broadening data, specifically the full width at half maximum intensity (FWHM), i.e., the Stark width, ‘‘wm”, and the Stark shift, ‘‘dm”. We also present the ratios of measured to theoretical, i.e., semiclassically or semiempirically calculated, widths and shifts, wm/wth and dm/dth, when available. In the fourth part of the table, we provide estimates of the uncertainties of the data and we also identify the literature references. As in the 2002 edition, the new values added in the present issue have been evaluated with the same criteria as before. Accuracy A = uncertainties within 15% B+ = uncertainties within 23% B = uncertainties within 30% C+ = uncertainties within 40% C = uncertainties within 50% D = uncertainties larger than 50% But it should be mentioned that due to the progress in the experimental methods, the quality of the results is most of the time better than before. Therefore, the letter B+ has been used very frequently, even when the accuracy was very close to the A limit (15%). Furthermore in several cases, the authors calculate their own detailed estimation of the accuracy for each measured value. In such cases, the author’s value has been retained and the numerical value written in the accuracy column. D is used very sparingly, i.e., for important transitions only when no other data are available, and for uncertainties estimated not to exceed factors of three. In this critical review we have expressed the relative uncertainties as ‘‘combined standard uncertainties” according to the recommendations by Taylor et al. (1994) This means that the overall uncertainties of the measurements are given as the root of the sum of the squares (rss) of the individual contributions. All reported, or otherwise estimated-individual standard uncertainties, that are contributing have been combined to the ‘‘rss” relative error. This new procedure differs from the preceding reviews (Konjevic´ and Roberts, 1976; Konjevic´ and Wiese, 1976, 1990; Konjevic´ et al., 1984a,b) where the straight sum of individual uncertainties was taken as the overall uncertainty. For example, in Konjevic´ and Roberts (1976) and Konjevic´ and Wiese (1990) the total error in the Stark width from uncertainties of ±10% in the electron density and ± 15% in the half-width measured was ± 25%, while the rss estimate used here yields ±18%. In many experiments, the two dominant contributions are the uncertainties in the electron density and line width, or shift, measurement. Smaller

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contributions arise usually from the deconvolution process, from plasma inhomogeneities such as cooler, lower electrondensity end-layers, from optical depth problems and corrections, and from plasma temperature measurements. In arriving at our uncertainty estimates, we have also taken into account occasional disagreements between authors outside their mutual error estimates. Furthermore, whenever possible, we have tested the adherence of the data to regularities and similarities predicted on the basis of atomic structure considerations (Wiese and Konjevic´, 1982, 1992; Konjevic´, 1999). For example, Stark half-widths should be normally nearly the same for all lines within multiplets, and we commented on cases where significant departures from this rule occurred. Studies of iso-electronic ions of the Li-sequence have shown clear systematic trends of the Stark widths with nuclear charge. 5. Summary and conclusions We have critically evaluated and compiled experimental Stark broadening data for isolated spectral lines of neutral and ionized atoms published since our last compilation in 2001, that is, for the 7 years period 2001 through June 2007. The growth of experimental data has been especially pronounced for multiply-charged ions due to the development and applications of new plasma sources, see also Konjevic´ (1999). We have found that the new experimental data are generally very consistent with the earlier material, as well as with the results of the semi-classical theory. But most of the new data are not significantly better than those in the last 2001 review, indicating that improvements in the experimental techniques have not advanced significantly in recent years. For lines of neutral atoms we observe that for Stark widths the agreement between different experiments, as well as experiment and theory, is usually within ± 20%, and often within 10%. Stark width data of especially good quality and mutual consistency are found for several lines, of Ar IV, He I, O III, Si II and Xe III (Pelaez et al., 2006b). So that these Stark widths can compete with other techniques as a high-accuracy plasma diagnostic approach for the determination of electron densities. Stark widths have been measured over a large electron density and temperature range and the agreement between experiments and theory is usually good. 6. Appendix: Plasma sources Three properties of the plasma sources principally affect the accuracy of the Stark broadening data: the geometry of the source (including presence or absence of boundary layers), its stability during observation time, and the reproducibility of pulsed sources, especially for shot-to-shot scanning techniques. 6.1. Stationary plasma sources For the wall-stabilized arc, it has been already mentioned (Konjevic´ and Wiese, 1976) that a stationary source induces boundary layers. Accordingly they necessitate either side-on observation, with Abel inversion of the profiles, or end-on observation. The problem of the de-mixing effect makes difficult the observation of the elements that have to be added in the carrier gas. The limited access to the arc channel and its small radial extension make applications of laser techniques for electron density measurements impractical. 6.2. Pulsed discharges In the condenser discharge created plasma case, the boundary layer thickness is a function of the duration of the plasma and of the time of observation. Its effect on the observed spectral profile depends on the side the observation is done and on the ratio of this layer to the length of the homogenous part of the plasma. That is why the column of plasma should be linear and observed end on. It is recommended to situate the electrodes along the axis of the plasma column and to observe though them. The possibility of varying the length of the plasma facilitates optical depth checks (Radtke and Gu¨nther, 1986; Uzelac et al., 1991). Techniques as pre-ionization of the plasma are prone to improve homogeneity. When the studied element cannot be supplied under gaseous or vapor phase, the way it is introduced could induce in-homogeneity. 6.3. Shock tubes The shock-wave-generated plasma has to be observed side on, due to the fact that the electron density can be considered as constant in thin slices perpendicular to the direction of propagation of the wave. Their interest is due to the large volume of plasma with negligible boundary layers (Truong-Bach and Drawin, 1979), to the possibility to introduce controlled quantities of the elements under studies though gaseous or volatile compounds. The range of temperature covered by such a device is exactly the same as those where the Stark parameter exhibits large variations and where theories disagree.

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6.4. Laser-produced plasmas For laser-created plasmas, three cases have to be considered. The first one is when the laser is fired in a vessel containing gas, then the plasma column resembles the one that is driven by a discharge. The second is when the laser is fired onto a solid surface, the properties of the plasma vary greatly from the surface to the top of the plasma column generated by the laser beam (plasma plume). The source has to be observed side-on in sections perpendicular to the beam. The boundary layer can be thinner than in the case of a discharge, when the pulse duration is shorter. In the third case when the laser is stationary, the plasma has thick boundary layers similar to those in arcs. Two sources have been especially designed to try to avoid boundary layers: it is the gas liner pinch of Kunze (Finken and Ackermann, 1982; Glenzer et al., 1994; Bu¨sher et al., 1996; Glenzer et al., 1996) and the two perpendicular laser beams of the Naval Research Laboratory, by Martinez and Bianco (Martinez et al., 1996; Chan et al., 1996; Mayer and Bush, 1985; Kearney et al., 1990; Mostovych et al., 1991, 1995). Whatever is the source, a characterization of the plasma is highly desirable prior to measurements. The principal properties and specifications of the plasma sources used from 1990 to 2000, most of them being still used up to now, are listed in the 2002 Critical Review (Konjevic´ et al., 2002). 6.5. Sources used since 2001, and not during the 1990–2000 period of time For Ar I, Dzierzega et al. (2003) have used an arc described in Pokrzywka et al. (1996) and Cadwell and Hu¨wel (2004) a pulsed Nd:YAG laser described in Nassif and Hu¨wel (2000). For Ar II, Iglesias et al. (2006) have used a laser heated gaspuff described in Elton et al. (2004b). For Au II, Ortiz and Mayo (2005) have used a Nd:YAG laser described in Xu et al. (2004). For Na I, Miokovic´ et al. (2005) have used an AC-high pressure discharge described in de Groot et al. (1986). For Sn III, Kieft et al. (2004c) have used a pinched arc discharge described in Kieft et al. (2004d). A special mention has to be done for a modified version of the linear, low pressure, pulsed arc used as plasma source in many experiments: Djenizˇe and Srec´kovic´ (2007) for Au III; Djenizˇe et al. (2001, 2002a,b,c, 2003, 2004a,b,c, 2005a,b,c, 2006a,b,c,d,e) for Ar IV, Ne II, Si III, Si IV, S III, S IV, O III, O IV, Mg I, Mg II, He I, Ag I; Milosavljevic´ and Djenizˇe (2001, 2003b,c) for He I, for Ar I and He I; Milosavljevic´ et al. (2001, 2003a,b, 2004a,b, 2006) for Ne II, III, IV, Kr I, Ar I, Ne I; Sreckovic´ et al. (2000, 2001a,b, 2003, 2004a,b, 2005, 2007) for Sn II, O II, III, S III, F II, III, He I, Mn I. That source has been described by Labat (1978) and by Djenizˇe and Labat (1979) and has been tested for its homogeneity along the line of sight by Labat et al. (1991) in the only case of ionized bromine spectral lines, by driving the discharge in tubes of various lengths, the bromine vapor being diluted (5–30%) in a nitrogen driving gas but such test has never been repeated later. The length variation permit to correct from self absorption in the linear part of the discharge, but not from the distortion of the line profile due to the curved part of the plasma between the linear part and the electrode which is in the observation line. A more complete description of the source can be found in Milosavljevic´ et al. (2007). A doubt concerning the homogeneity (boundary layer) of the source, especially when it has been used with pure gas, has been raised by several authors: Ivkovic´ et al. (2006), Jovic´evic´ et al. (2005) and Dzierzˇega et al. (2006) in the case of the Stark parameters measurements of Ne I spectral lines. In addition to the effect on the observed line profile, such inhomogeneity should also affect the accuracy of the electronic value measured by laser interferometry. In the conclusion of Milosavljevic´ et al. (2007) article ‘‘characterization of the pulsed plasma source” the authors consider that: the plasma density along the optical axis exceed the minimum threshold for LTE between 3 and 60 ls and that no low-density boundary layer was observed. 7. Appendix: Advanced procedures for the deconvolution of line profiles In most Stark broadening experiments dealing with symmetric line profiles, a standard line shape deconvolution technique is used which is, for example, well described by Davies and Vaughan (1963) These authors supply convenient correction tables for the width of the Lorentzian components and are therefore widely cited. However, most lines of neutral atoms are slightly asymmetric since their Stark profiles contain a usually small asymmetric ion broadening component (which becomes negligible for ion lines). Thus, the above cited standard method to deconvolute Voigt profiles developed by Davies and Vaughan (1963) is not strictly applicable, and two methods, generalized to include the deconvolution of asymmetric profiles, were developed. An approximate graphical deconvolution procedure for asymmetrical line profiles was described by Mijatovic´ et al. (1993). Then, in order to determine simultaneously the electron impact width, shift and ion broadening-parameter, a fitting method was developed by Nikolic´ et al. (1999) for the asymmetric Stark profiles of isolated and overlapping neutral atom lines. This paper follows to a certain extent the earlier work by Goly and Weniger (1986) who determined widths, shifts, and ion broadening parameters for several C I and N I lines (for the latter, widths only) by a convolution procedure (Doppler and best fit Stark profile). Generally speaking, this fitting method involves the computation of convolution integrals of Gaussian and of asymmetric Stark broadening profiles for a wide range of ion broadening and Debye shielding parameters. These have been tabu-

A. Lesage / New Astronomy Reviews 52 (2009) 471–535

477

lated, and the Stark widths may be derived from the known parameters. Applications were performed by Nikolic´ et al. (1999) and Schinko¨th et al. (2000). An iterative non-linear deconvolution method was developed by Biraud (1969) and Depiesse et al. (1995) and its description is quite complex Jansson (1997). An application for the deconvolution of Si II lines was performed by Wollschla¨ger et al. (1997). Milosavljevic´ (2001), Milosavljevic´ and Poparic´ (2001) and Milosavljevic´ and Djenizˇe (2003a), have shown that a numerical integration of the integral included in the equation providing the various line shapes in the case of neutral atom broadening by electron and ions, allows the simultaneous determination of the basic physical properties that characterize the line profile and of the plasma parameters. They mention that such a method could be of great interest for plasma modeling and diagnostics, especially for remote sources as it is the case in astrophysics. But the Milosavljevic´ et al. (2001) ‘‘atomic spectral line-free parameter deconvolution procedure” has been commented by Nikolic´ et al. (2003) who suggest to use another method for the deconvolution of plasma broadened non-hydrogenic neutral atom lines using Marquardt–Levenberg algo˚ isolated, and 4333, 4335A ˚ blended lines. A reply to rithm, presented in Nikolic´ et al. (2001) and tested with the Ar I 4259A that comment has been published by Milosavljevic´ and Poparic´ (2003). An evaluation of Milosavljevic´ et al. (2001) procedure for the ‘‘simultaneous determination of electron impact width, ion and ion-dynamic parameter from the shape ˚ of plasma broadened non-hydrogenic atom line” has been presented by Ivkovic´ et al. (2006) taking the Kr I k 8104.4 A as an example. Ivkovic´ et al. (2006) have shown that Milosavljevic´ et al. (2001) procedure is inappropriate for line shape parameters determination in the case of small differences due to the ionic contribution. Furthermore Jovic´evic´ et al. (2005) and Dzierzˇega et al. (2006) have shown that the line asymmetry detected when the linear low pressure pulsed arc is used as plasma source is due to boundary effect, especially when pure gas are used. PART II. DATA TABLES Argon, Ar I Ground state: 1s22s22p63s23p61S0. Ionization energy: 15.7596 eV = 127,109.80 cm1. Dimitrijevic´ et al. (2002), Milosavljevic´ and Djenizˇe (2003b) and Milosavljevic´ et al. (2003b) used a low-pressure pulsed discharge to measure three and five Ar I lines respectively, end-on, along the axis of a pyrex discharge tube of 5 mm inner diameter and 8 cm plasma length, by a step-by-step technique. The working gases are mixtures of argon and helium 72%, 28%, except for two experiments of Milosavljevic´ et al. (2003b) where it is 97% and 3%. Self-absorption was checked by comparison of the measured intensities ratio of lines of the 4s–4p0 transition to the calculated value. The purposes of the two studies are different: in the first article, the Stark width of three lines are measured including the ion contribution and compared to previous measurements and with semi-classical calculations. In the second and third articles, the purpose is to test a new deconvolution procedure Milosavljevic´ and Poparic´ (2001), on five Ar I lines observed in three different plasmas sources for plasma diagnostics. Such procedure is of great interest in astrophysics, where direct measurements of the plasma parameters (T and Ne) are not possible. Comparison with Griem (1974) theoretical data are done for the k ˚ and k 4200.68 A ˚ multiplets. Milosavljevic´ and Djenizˇe (2003b) and Milosavljevic´ et al. (2003b) experimental data 4198.32 A are about 50% and 20% smaller, respectively, than Griem (1974) predictions. They are in agreement with those of Bues et al. (1969) and Gericke (1961) for the Ar I k 4198.32 multiplet and with theoretical values of Griem (1962), and with the experimental values of Gericke (1961), Musielok (1994), Chapelle et al. (1967) and Bues et al. (1969) for the Ar I k ˚ multiplet, but not with those of Kusz et al. (1996) in the two cases. Direct comparison of Milosavljevic´ and 4200.68 A ˚ lines with Djenizˇe (2003b) and Milosavljevic´ et al. (2003b) experimental data for the Ar I k 4158.6, 4164.2 and 4266.3 A previous measurements is impossible, because of the various plasma conditions in the experiments. Instead of the classical optical emission spectroscopy almost exclusively used to measure Stark parameters, Dzierzega et al. (2003) used a Doppler-free method called ‘‘degenerate four-wave mixing spectroscopy” in an electric argon arc. ˚ line width and shift is compared with previous measurements. The agreement with the results The Ar I k 6965.43 A obtained with the classical method lead the authors to the conclusion that the new one is particularly recommended in the case of elements with large Doppler broadening. Their tabulated width and shift values are normalized to a specific value of the electron density, but the corresponding temperature is not provided. Cadwell and Hu¨wel (2004) measured 12 Ar I lines in a pulsed laser-generated argon plasma at atmospheric pressure and made comparisons with previous measurements and with Griem (1974) calculations. But as published values are obtained for ranges of temperature and electron density, they cannot be introduced in the present tabulation. Milosavljevic´ et al. (2004b) measured separately the ion and electron contributions to the Stark width and shift of the k ˚ Ar I line. The experimental set up and procedure are as in Milosavljevic´ et al. (2003b) except that the temper4259.36 A ature and electron density have been, in addition, determined by the line deconvolution method described in Milosavljevic´

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and Poparic´ (2001) The measured electron contributions to the width and shift values are approximately 1.5 times lower than Griem (1974) predictions. As in (Milosavljevic´ et al., 2004b), Milosavljevic´ et al. (2006) measured seven Ar I lines from 4s–4p and 4s–4p0 transitions. Self absorption is carefully checked by doubling the optical path length with a mirror and taken in account for each of the measured lines, when necessary. For lines belonging to the 4p–4s transition, comparison with available experimental values is impossible because of large differences in plasma parameters especially in electron temperature. For the 4s–4p0 ˚ line, comparison with Vitel and Skowronek (1987b), Siyacoun et al. (1992), Valognes et al. array Ar I k 6965.43 A (2004) at similar electron temperature shows that Milosavljevic´ et al. (2004b) values are 38% and 15% larger for the widths and the shifts, respectively, than theirs. For the three other lines belonging to the same transition, direct comparison is difficult due to the different plasma conditions. There are no theoretical predictions for the present measured lines. Neverthe˚ total (electron + ion) lines widths and shifts with less, a comparison is made for the measured Ar I k 7635.11 and 7723.76 A ˚ Griem (1974) calculated Ar I k 8103.69 A line parameter. This comparison suggests that the contribution of the quasi-static ion, and ion dynamic effects is more important than what semi-classical theory predicts. Ref.

Plasma source

Dimitrijevic´ et al. (2002) Milosavljevic´ and Djenizˇe (2003b), Milosavljevic´ et al. (2003b, 2004b, 2006) Dzierzega et al. (2003)

Low-pressure pulsed arc Modified linear low pressure pulsed arc Electric arc

Cadwell and Hu¨wel (2004)

Laser plasma

Method of measurement

Remarks

Electron density

Temperature

Single wavelength laser ˚ interferometer at 6328 A Single wavelength laser ˚ and Ar I interferometer at 6328 A line deconvolution procedure Degenerate four-wave mixing spectroscopy Saha equation and Stark width of ˚ line Ar I 7030.25 A

˚ Ratio of Ar II 5009 to Ar I 6965 A lines From ratio of seven Ar I spectral lines to five Ar II lines and Ar I line deconvolution procedure Degenerate four-wave mixing spectroscopy Boltzmann plot of 17 Ar I lines

Shot-to-shot scanning Shot-to-shot scanning

Doppler-free method Published experimental widths including ion contribution

Numerical results for Ar I No. Transition Multiplet array 1.

4s–4p

2

[3/2]0–2[3/2]

Wavelength Temperature ˚) (A (K)

Electron density (1017 cm3)

˚) wm (A

7723.76

0.67 0.70 0.71 0.38 0.67 0.70 0.71 0.67 0.70 0.71 0.33 0.67 0.70 0.71 0.67 0.70 0.71 0.67 0.70 0.71 0.38 0.8 0.67 0.70 0.71

.774 .844 .855 0.28 .763 .830 .849 .796 .852 .905 0.25 .638 .692 .714 .529 .563 .583 .726 .785 .802 0.33 66 GHz .519 .580 .570

7635.11

2.

3.

4s–4p0

2

[3/2]0–2[1/2]

7514.65

2

[3/2]0–2[3/2]

7383.98

7067.22

4.

2

[3/2]0–2[1/2]

7272.94

6965.43

15,600 16,000 16,200 13,000 15,600 16,000 16,200 15,600 16,000 16,200 13,000 15,600 16,000 16,200 15,600 16,000 16,200 15,600 16,000 16,200 13,000 12,760–18,560 15,600 16,000 16,200

wm/wth

˚) dm (A

.390 .432 .445 .378 .420 .433 .411 .448 .490 .216 .226 .228 .187 .197 .220 .189 .204 .208 22 GHz .175 .210 .199

dm/dth

Acc. Ref.

B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+

Milosavljevic´ et al. (2006) Milosavljevic´ et al. (2006) Milosavljevic´ et al. (2006) Dimitrijevic´ et al. (2002) Milosavljevic´ et al. (2006) Milosavljevic´ et al. (2006) Milosavljevic´ et al. (2006) Milosavljevic´ et al. (2006) Milosavljevic´ et al. (2006) Milosavljevic´ et al. (2006) Dimitrijevic´ et al. (2002) Milosavljevic´ et al. (2006) Milosavljevic´ et al. (2006) Milosavljevic´ et al. (2006) Milosavljevic´ et al. (2006) Milosavljevic´ et al. (2006) Milosavljevic´ et al. (2006) Milosavljevic´ et al. (2006) Milosavljevic´ et al. (2006) Milosavljevic´ et al. (2006) Dimitrijevic´ et al. (2002) Dzierzega et al. (2003) Milosavljevic´ et al. (2006) Milosavljevic´ et al. (2006) Milosavljevic´ et al. (2006)

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479

Table (continued) No. Transition Multiplet array 2

2

5.

[3/2]0–2[5/2]

[3/2]0–2[3/2]

wm Wavelength Temperature Electron ˚) ˚) (A (A (K) density (1017 cm3)

wm/wth

4200.67

4266.29

4164.18

4158.59

2

2

6.

a

[3/2]0–2[1/2]

[1/2]0–2[1/2]

4198.32

4259.36

15,600

˚) dm (A

dm/dth

Acc. Ref.

B+

0.67

1.19

0.77

16,000

0.70

1.23

0.76

B+

16,200

0.71

1.26

0.76

B+

15,600

0.67

1.10

B+

16,000

0.70

1.13

B+

16,200

0.71

1.18

B+

15,600

0.67

1.09

B+

16,000

0.70

1.15

B+

16,200

0.71

1.15

B+

15,600

0.67

1.14

B+

16,000

0.70

1.19

B+

16,200

0.71

1.22

B+

15,600

0.67

1.12

0.50

16,000

0.70

1.17

0.49

B+

16,200

0.71

1.19

0.49

B+

0.67 0.70 0.71

1.584a 1.670a 1.638a

1.138 1.094 1.134

B+ B+ B+

15,600 16,000 16,200

B+

Milosavljevic´ Milosavljevic´ Milosavljevic´ Milosavljevic´ Milosavljevic´ Milosavljevic´

and Djenizˇe (2003b), et al. (2003b) and Djenizˇe (2003b), et al. (2003b) and Djenizˇe (2003b), et al. (2003b)

Milosavljevic´ Milosavljevic´ Milosavljevic´ Milosavljevic´ Milosavljevic´ Milosavljevic´ Milosavljevic´ Milosavljevic´ Milosavljevic´ Milosavljevic´ Milosavljevic´ Milosavljevic´ Milosavljevic´ Milosavljevic´ Milosavljevic´ Milosavljevic´ Milosavljevic´ Milosavljevic´ Milosavljevic´ Milosavljevic´ Milosavljevic´ Milosavljevic´ Milosavljevic´ Milosavljevic´

and Djenizˇe (2003b), et al. (2003b) and Djenizˇe (2003b), et al. (2003b) and Djenizˇe (2003b), et al. (2003b) and Djenizˇe (2003b), et al. (2003b) and Djenizˇe (2003b), et al. (2003b) and Djenizˇe (2003b), et al. (2003b) and Djenizˇe (2003b), et al. (2003b) and Djenizˇe (2003b), et al. (2003b) and Djenizˇe (2003b), et al. (2003b) and Djenizˇe (2003b), et al. (2003b) and Djenizˇe (2003b), et al. (2003b) and Djenizˇe (2003b), et al. (2003b)

Milosavljevic´ et al. (2004b) Milosavljevic´ et al. (2004b) Milosavljevic´ et al. (2004b)

Milosavljevic´ et al. (2004b). The width value is the total width.

Djurovic´ et al. (2002) measurements of 9 neutral argon line widths and shifts are not presented here, because they are provided for ranges of electron density and temperature and measured over calculated ratio, and consequently cannot be introduced in the numerical result table. For the Milosavljevic´ and Djenizˇe (2003b) measurement, as the ion contribution only of 19 prominent Ar I spectral lines have been reported they are not introduced in the table. Determination of ion-broadening parameters of ten Ar I spectral lines has been presented in Nikolic´ et al. (2004). From the analysis of theirs and others results they conclude that Griem’s (1974) theory gives underestimated values for the ion˚ , N I k 4151.5 A ˚ and Ar I k 7030.3 A ˚ line cases. Further improvements broadening parameter, except in the C I k 5380.3 A of the theory are needed to discriminate between divergent experimental results. Argon, Ar II Ground state: 1s2 2s2 2p6 3s2 3p52 P03=2 . Ionization energy: 27.630 eV = 222,848.2 cm1. Key data on experiments Ref.

Plasma source

Method of measurement

Remarks

Electron density

Temperature

Iglesias et al. (2006)

Plasma laser

He I, He II Stark width

Ratio of He II/He I integrated-line-intensity ratios

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A. Lesage / New Astronomy Reviews 52 (2009) 471–535

Numerical results for Ar II (averaged temperature along line of sight 43,000 K) No.

Transition array

Multiplet

Wavelength ˚) (A

Electron density (1017 cm3)

wm ˚) (A

wm/wth

1.

3d–4p

4

3968.4

9.0

1.6

7.2

D–4D0

4013.9

2.

3.

4s–4p

4s–4p

4

4

P–4P0

P–4D0

4847.8

4331.2

4348.1

4.

a

4s–4p

2

P–2P0

4764.9

dm ˚) (A

dm/dth

Acc.

Ref.

1.1

B

1.0

0.82

B

4.5

0.8

1.1

B

9.0

1.6

1.1

B

7.2

1.6

1.3

B

4.5

1.0

1.3

B

9.0

2.9

1.2

B

7.2

1.7

1.0

B

4.5

1.1

0.90

B

9.0

3.0

1.3

B

7.2

2.2

1.2

B

4.5

1.8

1.5

B

9.0

3.5

1.5

B

7.2

2.6

1.4

B

4.5

1.9

1.6

B

9.0

2.4

1.0a

B

7.2

2.0

1.1a

B

4.5

1.6

1.4a

B

Iglesias et al. (2006) Iglesias et al. (2006) Iglesias et al. (2006) Iglesias et al. (2006) Iglesias et al. (2006) Iglesias et al. (2006) Iglesias et al. (2006) Iglesias et al. (2006) Iglesias et al. (2006) Aparicio et al. (1998) Iglesias et al. (2006) Iglesias et al. (2006) Iglesias et al. (2006) Iglesias et al. (2006) Iglesias et al. (2006) Iglesias et al. (2006) Iglesias et al. (2006) Iglesias et al. (2006)

Using wth from Wm/Wth in Konjevic´ (1999) as derived from Dimitrijevic´ and Konjevic´ (1980).

Iglesias et al. (2006) measured Stark profiles of non-blended Ar II spectral lines in a plasma created by the laser heating ˚ , output energy 5J, pulse width 22 ns) of a puff of gas (Ar + 30% He, at pressure 7 atm., description (ruby laser at 6943 A in Elton et al. (2004b)). Observation with a 0.75 m focal length Czerny–Turner spectrograph was done along an axis orthogonal to that of the horizontal laser and the vertical axis of the gas expansion. An intensified CCD detector, coupled ˚ . Lorentz profiles with an optical system, is enable to space and time resolve the plasma. The spectral resolution was 1.8 A convoluted with the apparatus function were compared, through a computerized procedure, to the measured spectral profile, until a best fit profile was obtained. Authors estimated the precision, for their Stark broadening parameter obtained (full-width at half-maximum of the best fit profile), as being ± 23%. Iglesias et al. (2006) measured values (of average ± 30% accuracy according to the authors), agree with all previously published Ar II values: Dzierzega and Musiol (1994), Pellerin et al. (1997), Aparicio et al. (1998) (of average ± 25% accuracy). Griem (1974) calculated values for the 4 D–4D0, 4P–4P0 and 4P–4D0 multiplets and Dimitrijevic´ and Konjevic´ (1980) for the 2P–2P0 agree with Iglesias et al. (2006) measured values and previous ones within ± 40% uncertainty. Argon, Ar IV Ground state: 1s2 2s2 2p6 3s2 3p34 S03=2 . Ionization energy: 59.81 eV = 482,400 cm1.

A. Lesage / New Astronomy Reviews 52 (2009) 471–535

481

Djenizˇe et al. (2001) have measured widths and shifts of 18 Ar IV lines in a modified version of a low-pressure pulsed arc, end-on, on a shot-to-shot basis. The plasma was assumed to be homogeneous, but the effects of the inhomogeneous end-layers were not discussed. Due to the very low concentration of emitting atoms, self-absorption is negligible and the measure of relative line intensity ratios within multiplet 4UV in Ar IV confirms that assumption. The line profiles were corrected for Doppler and apparatus contributions. Measured widths and shifts were compared with previous measured values and those calculated with Griem’s semi-empirical formula (Griem, 1974) and with the modified semi-empirical formula by Dimitrijevic´ and Konjevic´ (1981). Comparison includes the theoretical Stark width values calculated by Hey et al. (1990) on the basis of the impact and classical-path approximation of Hey and Breger (1982). ˚ spectral lines between previous measured as with calculated and reported The agreement for Ar IV 2640.3 and 2757.4 A values leads the authors to recommend them for diagnostic purpose.

Key data on experiments Ref.

Plasma source

Method of measurement

Remarks

Electron density

Temperature

Djenizˇe et al. (2001)

Modified linear low pressure pulsed arc

Laser interferometer at k ˚ 6328 A

Boltzmann plot of seven Ar III lines

Shot-by-shot profile recording

Numerical results for Ar IV ˚ )a dm/dth Acc. wm/wth dm (A

No.

Transition array

Multiplet

Wavelength ˚) (A

Temperature (K)

Electron density (1017 cm3)

wm ˚) (A

1.

4s–4p

4

2830.25

22,500

1.9

0.18

0.0

B+

2809.44

22,500

1.9

0.21

0.0

B+

2788.96

22,500

1.9

0.19

0.033

B+

2776.26

22,500

1.9

0.18

0.032

B+

2640.34

22,500

1.9

0.16

0.028

B+

2615.68

22,500

1.9

0.165

0.0

B+

2608.06

22,500

1.9

0.185

0.036

B+

4

2.

3. a

4s0 –4p0

P–4D0

P–4P0

4

P–4S0

2513.28

22,500

1.9

0.165

0.0

B+

2

P–2D0

2926.33

22,500

1.9

0.21

0.024

B+

2

P–2P0

2608.44

22,500

1.9

0.215

0.0

B+

2599.47

22,500

1.9

0.165

0.0

B+

2525.69

22,500

1.9

0.175

0.0

B+

0.018

B+

2

D–2F0

2284.47

22,500

1.9

0.19

2

D–2D0

2757.42 2624.92

22,500 22,500

1.9 1.9

0.200 0.16

0.025 0.013

B+

2621.36

22,500

1.9

0.19

0.03

B+

2619.98

22,500

1.9

0.16

0.03

B+

Unidentif.

4005.1

22,500

1.9

˚. Djenizˇe et al. (2001) mentioned a shift measurement accuracy of ± 0.008 A

0.26

B+

Ref. Djenizˇe (2001) Djenizˇe (2001) Djenizˇe (2001) Djenizˇe (2001) Djenizˇe (2001) Djenizˇe (2001) Djenizˇe (2001) Djenizˇe (2001) Djenizˇe (2001) Djenizˇe (2001) Djenizˇe (2001) Djenizˇe (2001) Djenizˇe (2001)

et al.

Djenizˇe (2001) Djenizˇe (2001) Djenizˇe (2001) Djenizˇe (2001) Djenizˇe (2001)

et al.

et al. et al. et al. et al. et al. et al. et al. et al. et al. et al. et al. et al.

et al. et al. et al. et al.

482

A. Lesage / New Astronomy Reviews 52 (2009) 471–535

Carbon, C I Ground state: 1s22s22p23P0. Ionization energy: 11.260 eV = 90,820.42 cm1. ˚ line profile in a linear low-pressure pulsed arc on a step-by-step Djenizˇe et al. (2006e) measured the C I k 2478.561 A recording technique. The plasma (length 14 cm, diameter 5 mm) is observed end-on. The working gas was CO2 at 67 Pa filling pressure in flowing regime. The authors have chosen the discharge conditions to minimize the self-absorption, but did not mention any check. van der Waals and resonance broadening were neglected. The ion contribution to the total Stark width is also neglected according to Griem’s (1974) published ion broadening parameters (less than 3% of the estimated electron contribution at Ne = 1017 cm3). The standard (Davies and Vaughan (1963)) deconvolution procedure has been applied using the least squares algorithm. The Djenizˇe et al. (2006e) measured Stark width is in agreement with the Mu¨ller et al. (1973) experimental value within the error bar and is 18% below Griem’s (1974) semi-classical calculated value. The Nubbemeyer and Wende (1977) value is 12% higher than Griem’s (1974) predictions. The Djenizˇe et al. (2006e) measured Stark shift agrees within 7% with Griem’s (1974) calculated value and the Nubbemeyer and Wende (1977) experimental value is 22% greater than the predicted.

Key data on experiments Ref.

Plasma source

Djenizˇe et al. (2006e)

Low-pressure pulsed arc

Method of measurement

Remarks

Electron density

Temperature

Stark widths of six O II lines: 3954.36, 3973.26, ˚ 4072.15, 4075.86, 4185.44 and 4189.79 A

Boltzmann plot of relative intensities of OIII ˚ ) to OII (3954.36 and 3973.26 A ˚ ) lines (3961.57 A

Numerical results for C I No.

Transition array

Multiplet

1.

2p2–2p3s

1

S0 –1 P01

Wavelength ˚) (A

Temperature (K)

Electron density (1017 cm3)

wm ˚) (A

˚ ) dm/dth Acc. wm/wth dm (A

Ref.

2478.561

17,600

1.08

0.0740

0.84

Djenizˇe et al. (2006e)

0.047

0.93

B

Fluorine, F II Ground state: 1s22s22p43P2. Ionization energy: 34.971 eV = 282,058.6 cm1. Srec´kovic´ et al., 2004a measured Stark widths and shifts of five F II lines with a linear low-pressure pulsed arc. The working gas was SF6 at 130 Pa filling pressure in a flowing regime. The line profiles were recorded by a step-by step technique. Absence of self absorption was checked by the technique described by Djenizˇe and Bukvic´ (2001). van der Waals and resonance broadening were neglected. A standard Davies and Vaughan (1963) deconvolution procedure has been applied using the least-squares algorithm. For Mults. 1 and 7, the F II line widths of Srec´kovic´ et al. (2004a) closely agree with the previous measurements of Platisˇa et al. (1977), Djenizˇe et al. (1991b) and in the case of Mult. 5, with the results of Djenizˇe et al. (1991b). The agreement of the values of Srec´kovic´ et al. (2004a) with their own semi-classical calculations is within the experimental error limit for all their measured lines except for those of Mult. 8 and 1, where they are within the mutual error limit. For the F II line shift, the values measured by Djenizˇe et al. (1991b) are the only ones available for comparison for four of the five multiplets, and the agreement is within the error bar for the lines of Mults. 1, 5, and 7. Again, the agreement of the values measured by Srec´kovic´ et al. (2004a) with their own semi-classical calculations is within the experimental error bar for all their measured lines except for those of Mults. 8 and 9, where they are within the mutual error bar.

A. Lesage / New Astronomy Reviews 52 (2009) 471–535

483

Key data on experiments Ref.

Plasma source

Method of measurement

Remarks

Electron density

Temperature

Srec´kovic´ et al. (2004a)

Low-pressure pulsed arc

˚ Laser interferometer at 6328 A

Boltzmann plot of six F II lines

Numerical results for F II ˚) wm/wth dm (A

No.

Transition array

Multiplet

Wavelength ˚) (A

Temperature (K)

Electron density (1017 cm3)

wm ˚) (A

1.

2p33s– 2p3(4S0)3p 2p33s0 – 2p3(2D0)3p0

5 0 5

S–P

3851.67

33,600

2.80

0.648

0.034

B+

3

D0–3D

4109.16

30,400

2.75

0.610

0.018

B+

33,600

2.80

0.548

B+

30,400

2.75

0.744

B+

33,600

2.80

0.718

30,400

2.75

0.610

33,600

2.80

0.578

2.

1

3.

1

4.

2p33d– 2p3(4S0)4f

5.

5

D0–1F

4299.17

D0–1D

D0–5F

3202.76

4246.66

0.006

dm/dth Acc.

B+ B+

0.050

B+

30,400

2.75

3.81

0.018

B+

33,600

2.80

3.55

0.04

B+

Ref. Srec´kovic´ (2004a) Srec´kovic´ (2004a) Srec´kovic´ (2004a) Srec´kovic´ (2004a) Srec´kovic´ (2004a) Srec´kovic´ (2004a) Srec´kovic´ (2004a) Srec´kovic´ (2004a) Srec´kovic´ (2004a) Srec´kovic´ (2004a)

et al. et al. et al. et al. et al. et al. et al. et al. et al. et al.

Fluorine, F III Ground state: 1s2 2s2 2p34 S03=2 : Ionization energy: 62.708 eV = 505,777 cm1. Srec´kovic´ et al. (2004a) measured Stark widths and shifts of five F III lines with a linear low-pressure pulsed arc (Skuljan, 1993). The working gas was SF6 at 130 Pa filling pressure in a flowing regime. The line profiles were recorded by a step-by step technique. The absence of self absorption was checked by the technique described by Djenizˇe and Bukvic´ (2001). van der Waals and resonance broadening were neglected. The standard Davies and Vaughan (1963) deconvolution procedure has been applied using the least squares algorithm. For F III Mult. 1, the line widths measured and calculated (semi-classical perturbation formalism) by Srec´kovic´ et al. (2004a) agree mutually within 5%, and both lie above the previously measured Puric´ et al. (1988d) and calculated (Dimitrijevic´ and Konjevic´ (1981), Dimitrijevic´ and Konjevic´ (1980), Griem (1968b)) values. For the line shifts, measured ‘‘d” values show evident scatter and within the experimental accuracy are near to zero, and are very close to the values ˚. calculated by the authors. Srec´kovic´ et al. (2004a) mentioned a shift measurement accuracy of ± .008 A

Key data on experiments Ref.

Srec´kovic´ et al. (2004a)

Plasma source

Low-pressure pulsed arc

Method of measurement

Remarks

Electron density

Temperature

˚ Laser interferometer at 6328 A

Boltzmann plot of six F II lines

484

A. Lesage / New Astronomy Reviews 52 (2009) 471–535

Numerical results for F III ˚) wm/wth dm (A

No.

Transition array

Multiplet

Wavelength ˚) (A

Temperature (K)

Electron density (1017 cm3)

wm ˚) (A

1.

2p23s– 2p2(3P)3p

4

3113.61

30,400

2.75

0.359

0.028

B+

3115.69

30,400

2.75

0.327

0.014

B+

33,600

2.80

0.311

30,400

2.75

0.397

33,600

2.80

0.377

30,400

2.75

0.387

33,600

2.80

0.396

30,400

2.75

0.406

33,600

2.80

0.396

P–4D0

3121.54

3124.78

3134.22

dm/dth Acc.

B+ 0.019

B+ B+

0.003

B+ B+

0.028

B+ B+

Ref. Srec´kovic´ (2004a) Srec´kovic´ (2004a) Srec´kovic´ (2004a) Srec´kovic´ (2004a) Srec´kovic´ (2004a) Srec´kovic´ (2004a) Srec´kovic´ (2004a) Srec´kovic´ (2004a) Srec´kovic´ (2004a)

et al. et al. et al. et al. et al. et al. et al. et al. et al.

Gold, Au II Ground state: 1s22s22p63s23p63d104s24p64d104f145s25p65d101S0. Ionization energy: 20.20 eV = 162,950 cm1. Ortiz and Mayo (2005) measured the Stark parameters of 26 Au II lines in a plasma produced by ablation of gold, placed in molecular argon at 6.5 Torr, with a 160 mJ, pulsed (7 ns) Nd:YAG laser at 20 Hz. Description of the source ˚ ) observed the plasma perpendicular to the laser beam. is in Xu et al. (2004). A 1 m Czerny–Turner (resolution 0.3 A ˚ at 2800 A ˚ . The resolution was 0.30 A ˚ . Spectra were The instrumental line width, known with a 3% accuracy, was 0.32 A recorded on a time resolved multichannel analyzer (OMA III, EG&G). The 1 cm vertical entrance slit of the detector allowed storage of spectrum sections at preset delay from the laser pulse and during a selected time length. Detection was made in synchronism with the laser trigger. Background accumulation and subtraction was made. An Abel inversion of the spectra showed that Au I emission spectra came from the outer part of the plasma, whereas the Au II emission arises from the internal one. Ortiz and Mayo (2005) considered the plasmas as homogeneous and stable. Comparison of the observed intensity of the line with the one emitted by an optically thin plasma showed that in the worse ˚ ) the self-absorption was lower than 3% and consequently neglected. case (Au II, k 1921.00 A The Au II Stark line parameters were obtained from a computerized fit of the Voigt profile obtained by convolution of Lorezian profile due to the Stark broadening, with the Gaussian profile due to Doppler and instrumental broadening. Other broadening mechanisms were considered as negligible. Ortiz and Mayo (2005) estimated the line width error for most of the studied transitions was 18%. As the 26 values of the Au II Stark parameters are the first ever measured, there are no possible comparisons. Theoretical values are published in Popovic´ et al. (1999), but for lower temperatures. The D accuracy (larger than 50%) attributed to Ortiz and Mayo (2005) values is justified by the adopted spectrograph resolution, unable to measure such narrow width values. In a contribution to the VI SCSLSA Mayo et al. (2007) implicitly recognize that new measurements have to be done at higher resolution using the second order of the spectrograph.

Key data on experiments Ref.

Plasma source

Method of measurement

Remarks

Electron density

Temperature

Ortiz and Mayo (2005)

Plasma laser

˚ lines Saha equation with six Au II and the Au III 1917.64 A

Boltzmann plot of the Au II lines

Abel inversion

A. Lesage / New Astronomy Reviews 52 (2009) 471–535

485

Numerical results for Au II No.

Transition array

Multiplet

6s–6p 6s–6p 6s–6p 6p–7s 6p–6d 6s–6p 6p–7s 6p–6d 6p–6d 6p–7s 6p–6d 6p–7s 6s2–6s6p 6s2–6p 6s2–6p 6p–7s 6p–7s 6s–6p 6p–7s 6s2–6p 6s2–6p 6p–7s 6s2–6p 6s–6p 6p–7s 6s2–6p

Wavelength ˚) (A

Temperature (K)

Electron density (1017 cm3)

˚) wm (A (HWHM)

1921.64 2044.54 2213.16 2215.63 2231.18 2283.30 2291.40 2304.69 2314.55 2315.75 2340.06 2552.67 2565.70 2687.63 2688.16 2802.04 2819.79 2825.44 2837.85 2907.04 2913.52 2954.22 2982.10 2990.27 2994.80 3015.81

16,200 16,200 16,200 16,200 16,200 16,200 16,200 16,200 16,200 16,200 16,200 16,200 16,200 16,200 16,200 16,200 16,200 16,200 16,200 16,200 16,200 16,200 16,200 16,200 16,200 16,200

1.45 1.45 1.45 1.45 1.45 1.45 1.45 1.45 1.45 1.45 1.45 1.45 1.45 1.45 1.45 1.45 1.45 1.45 1.45 1.45 1.45 1.45 1.45 1.45 1.45 1.45

0.0169 0.0186 0.0180 0.0212 0.0230 0.0186 0.0204 0.0218 0.0189 0.0199 0.0206 0.0164 0.0196 0.0187 0.0170 0.0219 0.0226 0.0187 0.0227 0.0189 0.0179 0.0217 0.0199 0.0169 0.0221 0.0197

˚ ) dm/dth Acc. wm/wth dm (A D D D D D D D D D D D D D D D D D D D D D D D D D D

Ref. Ortiz Ortiz Ortiz Ortiz Ortiz Ortiz Ortiz Ortiz Ortiz Ortiz Ortiz Ortiz Ortiz Ortiz Ortiz Ortiz Ortiz Ortiz Ortiz Ortiz Ortiz Ortiz Ortiz Ortiz Ortiz Ortiz

and and and and and and and and and and and and and and and and and and and and and and and and and and

Mayo Mayo Mayo Mayo Mayo Mayo Mayo Mayo Mayo Mayo Mayo Mayo Mayo Mayo Mayo Mayo Mayo Mayo Mayo Mayo Mayo Mayo Mayo Mayo Mayo Mayo

(2005) (2005) (2005) (2005) (2005) (2005) (2005) (2005) (2005) (2005) (2005) (2005) (2005) (2005) (2005) (2005) (2005) (2005) (2005) (2005) (2005) (2005) (2005) (2005) (2005) (2005)

Gold, Au III Ground state: [Xe]4f145d92D5/2. Ionization energy: 33 eV = 270,000 cm1. Djenizˇe and Srec´kovic´ (2007) measured 12 doubly-ionized gold spectral lines in a modified version (Djenizˇe et al., 2004c) of a low-pressure pulsed Pyrex discharge (5 mm inner diameter and 14 cm plasma length) on a shot to shot basis. Observations were made end-on. Gold was introduced in a helium plasma by eroding thin (150 lm) gold cylindrical plates (l = 20 mm) posted inside the cylindrical part of the discharge tube on its ends. The working gas was an admixture of helium, nitrogen, and oxygen (90% He + 7% N + 3% O) flowing at 665 Pa. The plasma reproducibility was controlled by monitoring the He I, He II and O II line intensities. Self absorption was checked by using the method described in Djenizˇe et al. (2004c). The authors did not mention any correction. van der Waals and resonance broadening were neglected.

Key data on experiments Ref.

Djenizˇe and Srec´kovic´ (2007)

Plasma source

Method of measurement

Low-pressure pulsed arc

Electron density ˚ Stark He II Pa 4686 A width

Remarks Temperature ˚ /He I 5876 A ˚ Relative intensity ratio of He II 4686 A lines

486

A. Lesage / New Astronomy Reviews 52 (2009) 471–535

Numerical results for Au III ˚ ) dm/dth Acc. wm/wth dm (A

No.

Multiplet

Wavelength ˚) (A

Temperature (K)

Electron density (1017 cm3)

wm ˚) (A

1.

a4P–z4D0

2159.08

16,800

.78

.068

B+

2184.11

16,600

.74

.130

B+

a2F– z4D0 a2F– z4G0 ?

2322.27

16,400

.71

.080

B+

2188.97

16,800

.78

.062

B+

2167.33

16,600

.73

.066

B+

b2D– z4D0 b2D– z4G0 b2D– z4F0 a2G– z4D0

2402.71

16,600

.74

.070

B+

2382.40

16,600

.74

.130

B+

2405.12

16,600

.74

.050

B+

3227.99

19,600

.92

.180

B+

3309.86

19600

.92

.146

B+

2083.09

16,600

.76

.112

B+

2172.20

16,600

.74

.100

B+

2. 3. 4. 5. 6. 7. 8.

9. 10.

a2G– z4F0 a2P–90

Ref. Djenizˇe (2007) Djenizˇe (2007) Djenizˇe (2007) Djenizˇe (2007) Djenizˇe (2007) Djenizˇe (2007) Djenizˇe (2007) Djenizˇe (2007) Djenizˇe (2007) Djenizˇe (2007) Djenizˇe (2007) Djenizˇe (2007)

and Srec´kovic´ and Srec´kovic´ and Srec´kovic´ and Srec´kovic´ and Srec´kovic´ and Srec´kovic´ and Srec´kovic´ and Srec´kovic´ and Srec´kovic´ and Srec´kovic´ and Srec´kovic´ and Srec´kovic´

Helium, He I Ground state: 1s21S0. Ionization energy: 24.5874 eV = 198,310.68 cm1. Milosavljevic´ and Djenizˇe (2001, 2002a,b, 2003c) and Sreckovic´ et al. (2004b) used the modified low-pressure pulsed dis˚ line and its forbidden component (Milosavljevic´ and Djenizˇe, 2001); the charge to measure: the overlapping He I k 4470 A ˚ lines (Milosavljevic´ and Djenizˇe, 2002a); the He I k 3888.6, astrophysically important He I k 4471.5, 5875.6, 6678.2 A ˚ ˚ line (Milosavljevic´ and Djenizˇe, 2003c) 4713.2, 5015.6 A lines (Milosavljevic´ and Djenizˇe, 2002b); the He I k 7065.2 A ˚ and the He I k 3819.6 A (Sreckovic´ et al., 2004b) line profiles. Various dimensions of the discharge tube offer the possibility to vary the electron temperature in a wide range (see description of the sources in Djenizˇe et al., 1991c; Djenizˇe et al., 1998). They use a new deconvolution method, described in Milosavljevic´ and Poparic´ (2001), Milosavljevic´ and Djenizˇe (2003a). It includes a new numerical procedure to unfold the theoretical asymmetric convolution integrals of a Gaussian and a plasma-broadened spectral line profile jA,R(k) for spectral lines. The method determines all broadening contributions and plasma parameters, directly from the shape of the experimental spectral line. This is a characteristic which is of great interest in the field of astrophysics. The working gas is a helium (90%), nitrogen (8%) and oxygen mixture at filling pressure from 267 to 133 Pa. Observations were made end-on and profiles recorded step-by-step. Plasma reproducibility (±5%) was ˚ line profiles have been corrected for monitored by radiation from three helium lines. The He I k 3888.6, 5015.7 and 4771 A ´ self-absorption by using the double plasma length method described in Konjevic (1999). At high temperature (18,000–33,000K) Milosavljevic´ and Djenizˇe (2001) graphically compare the total line width of the overlapping components Dk1/2 and the wavelength distance between peaks DkAF with the predicted values by Griem (1968a) and Barnard et al. (1969), their measured values lie slightly below the calculated ones but still within error bar. The agreement is closer with the Valogne and Bardet (1996) more recently calculated values, even if that last ones are provided at higher temperature. Similar agreement is also graphically shown with the previous measured values by Haw´ ircovic´ (1984), Uzelac and Konjevic´ (1986), Perez et al. (1996), ryluk et al. (1974), Bavarian et al. (1975), Vujicic´ and C ˚ Wulff (1958), Nelson and Barnard (1971) and Berg et al. (1962). At lower temperature (T = 6000 K) the He I k 4471 A line is separated from the forbidden component and Milosavljevic´ and Djenizˇe (2001) compare their measured total width ‘‘wt” and electronic contribution ‘‘we” to the calculated values by Griem (1974), Bassalo et al. (1982) and Dimitrijevic´ and Sahal-Bre´chot (1990). The ratio of that measured line to the three above mentioned calculated values is Wexp/Wth = 0.78, 0.80 and 0.89, respectively. Previous measured values by Keller (1981) provide line widths 10% narrower.

A. Lesage / New Astronomy Reviews 52 (2009) 471–535

487

˚ Milosavljevic´ and Djenizˇe (2002a) measured values agree better with BasFor the He I, k 4471.5, 5875.6 and 6678.2 A salo et al. (1982) calculated values than with those of Griem (1974) and Dimitrijevic´ and Sahal-Bre´chot (1990) and in the ˚ line it is Dimitrijevic´ and Sahal-Bre´chot (1990) results which are the closest. Comparison is done for case of the k 4471.5 A the three lines with all previous measured values: Berg et al. (1962), Keller (1981), Roder and Stampa (1964), Puric et al. (1970), Gauthier et al. (1981), Vujic´ic´ and Kobilarov (1988), Kobilarov et al. (1989), Pe´rez et al. (1991), Bu¨cher et al. (1995) ˚ , with Berg et al. (1962) for the and Mijatovic´ et al. (1995). The best agreement is found with Keller (1981) for the k 4471.5 A ˚ ˚ 5875.6 A and Pe´rez et al. (1991) for the 6678.2 A lines measured values. ˚ lines Milosavljevic´ and Djenizˇe (2002b) measured values are compared to For the He I, k 3888.6, 4713.2, and 5015.6 A ˚ the best the Griem (1974), Bassalo et al. (1982), Dimitrijevic´ and Sahal-Bre´chot (1990) calculated ones. For k 3888.6 A ˚ agreement is found with Dimitrijevic´ and Sahal-Bre´chot (1990) values, for k 4713.2 A their measured values fall between ˚ Dimitrijevic´ and Sahal-Bre´chot those of Bassalo et al. (1982), Dimitrijevic´ and Sahal-Bre´chot (1990) and for k 5015.6 A (1990) values are those that fit experimental values the best. But nevertheless Griem (1974), Bassalo et al. (1982) calculations provide values of almost equal agreement. Milosavljevic´ and Djenizˇe (2002b) measured values are also compared with Berg et al. (1962), Griem et al. (1962), Bo¨tticher et al. (1963), Lincke (1964), Roder and Stampa (1964), Wulff (1958), Greig and Jones (1970), Kusch (1971), Einfeld and Sauerbrey (1976), Chaing et al. (1977), Soltwisch and Kusch (1979), Mazing and Slemzin (1973), Keller (1981), Kobi˚ Kobilarov et al. (1989) larov et al. (1989), Pe´rez et al. (1991) and Mijatovic´ et al. (1995) experimental values. For k 3888.6 A ´ measured values perfectly fit those of Milosavljevic and Djenizˇe (2002b) and for the others, the agreement is within error ˚ excellent agreement is found with bar except for those measured by Kusch (1971) which are much larger. For k 4713.2 A ´ ´ Lincke (1964), Wulff (1958), Perez et al. (1991) values. Mijatovic et al. (1995), Berg et al. (1962), Griem et al. (1962) values ˚ line Dimitrijevic´ and Sahal-Bre´chot (1990) provides the best are larger but still within mutual error bar. For the k 5015.6 A agreement between experimental and theoretical values but the two other theories also provide a very good agreement. ˚ line agree with those of Keller (1981) as well Milosavljevic´ and Djenizˇe (2003c) measured values for the He I k 7065.2 A as with those of Mazing and Slemzin (1973), while Mijatovic´ et al. (1995) values are15% larger. Milosavljevic´ and Djenizˇe (2003c) similarly compare their measured values with the three above mentioned theories. They fall between Bassalo et al. (1982) and Dimitrijevic´ and Sahal-Bre´chot (1990) calculated values, these last ones being closer to theirs. Griem (1974) calculated values are 20% larger. On the basis of the observed asymmetry of the profile, the ion broadening parameter and ion dynamic effect were obtained. A stronger influence of the ion contribution than existing theoretical approximation estimate, was found. ˚ line are the first ever done and as the only existing As the Sreckovic´ et al. (2004b) measured values for the He I k 3819 A theoretical calculations (Dimitrijevic´ and Sahal-Bre´chot, 1990) have been done at electron density much lower (1013 cm3) than the experimental one, no comparison is possible. In their articles Milosavljevic´ and Djenizˇe (2002a,b, 2003c) have obtained, on the basis of the observed asymmetry, the ion broadening parameters (A) caused by influence of the ion microfield on the line broadening mechanism and also the influence of the ion dynamic effect (D) on the line shape. They have found that the ion contribution to the line profiles plays a more important role than the semiclassical approximation (Griem, 1974; Bassalo et al., 1982) provides. That has to be taken into account when these He I lines are used for plasma diagnostic or astrophysical plasma modeling purposes. Similar behavior have been predicted by the semiclassical perturbation formalism (Dimitrijevic´ and Sahal-Bre´chot, 1990). The ion parameters Wi, and the A and D values measured by Milosavljevic´ and Djenizˇe (2002a,b, 2003c) are shown in the numerical result table despite the restrictions raised by Ivkovic´ et al. (2006), but they are not evaluated. The accuracy estimations in the corresponding column are for the electronic contribution to Stark width, which is then compared to Griem’s (1974) calculated value. (Values in the Wi and We colums, with one or two stars (* or **) do not seem to follow the regular rules.) Pe´rez et al. (2003) used a pulsed discharge, observed end-on, to measure line widths and shifts of the k 7065.19 and ˚ He I lines. Profiles were corrected from self-absorption with the help of a mirror. Contribution of instrumental 3888.65 A ˚ and and Doppler broadening to the measured line profiles are found to be negligible. Stark widths and shifts of k 7065 A ˚ He I lines are provided graphically. The value derived from these graphs are introduced in the table for a specific 3889 A value of the electron density. At these temperatures, the measured values are in close agreement with Griem (1974) predictions and previous experimental values: Milosavljevic´ and Djenizˇe (2003c), Mazing and Slemzin (1973), Mijatovic´ et al. ˚ line is prone (1995), Wulff (1958), Berg et al. (1962), Kusch (1971) and Kobilarov et al. (1989). As the strong k 3888.65 A to self-absorption, authors suspect that large line width measured in their experiment may be the consequence of small uncorrected self-absorption and could explain that their data are, for that line, slightly higher than the previous ones. ˚ astrophysically important line Djenizˇe et al. (2005a) measured for the first time the high lying 2p–5d, He Ik 4026.186 A profile, in a linear low pressure pulsed arc, end-on, on a step-by-step technique. Working gas was 95% He, 4% N, 1% O at 53 Pa. Authors assume that for such a high lying transition the helium plasma is optically thin. The line shape is approximated by a pure Lorentz profile. Comparison with semi-classical calculation Griem (1974) is not possible due to the fact

488

A. Lesage / New Astronomy Reviews 52 (2009) 471–535

that they are calculated for much lower electron density. At the high electron density of the experiment the lowering of the effective ionization energy has influence on the number and contribution of the perturbing levels. ˚ (2s3S–4p3P0) line were measured by Pela´ez et al. (2006a) to calStark parameters (width and shift) of the He I k 3188 A ibrate Stark width and shift dependencis as a function of the electron density. A spectroscopic and interferometric analysis of a pulsed plasma was achieved. The electron temperature (from 19,000 to 23,000 K) was obtained with the intensity ratio of He II lines. The electron density (in the range from 1.25  1016 to 6.22  1016 cm3) was measured by a two wavelengths ˚ lines. These experimental results are graphinterferometer and by measuring the Stark width of He II k 3203 and 4686 A ically and mathematically presented in the Pela´ez et al. (2006a) article, the formula is: 5 1=6 23 ; w ¼ N e ½A þ BN1=4 e ð1  4:81  10 N e Þ  10 23 d ¼ N e ½C þ DN1=4 ð1  4:81  105 N 1=6 ; e Þ  10

where width ‘‘w” and shift ‘‘d” are in nanometers and Ne in m23. The parameters A, B, C, D are given in the table. Parameters

Value

Statistical error

Comparison

wm/wth

dm/dth

A B C D

6.7  101 4.95  107 1.33  101 2.83  107

2.7  102 2.2  108 9.7  103 2.1  108

G BCW DSB

0.89 0.97 1.12

0.95 1.17 1.03

[G] Griem et al. (1962), Griem (1974); [BCW] Bassalo et al. (1982); [DSB] Dimitrijevic´ and Sahal-Bre´chot (1990).

A comparison with theoretical models is provided as well as with previous experimental results. Pela´ez et al. (2006a) data were obtained with very controlled features concerning its reproducibility between discharges and non-detectable boundary layers effects, they agree very well with theoretical predictions and previous experimental results. Their calibration equations may be used with confidence for plasma diagnostics of astronomical objects in the UV range.

Key data on experiments Ref.

Plasma source

Milosavljevic´ and Djenizˇe (2001, 2002a, 2003c, 2004b) Pe´rez et al. (2003)

Modified low-pressure pulsed arc Linear pulsed discharge Modified low-pressure pulsed arc

Djenizˇe et al. (2005a)

Method of measurement

Remarks

Electron density

Temperature

Laser interferometer ˚ at 6328 A Line width of three He I lines Laser interferometer ˚ at 6328 A

Ratio of the relative intensities of four N III spectral lines Boltzmann plot of five He I lines

Shot-by-shot profile recording

˚ /He I 5876 A ˚ line He II Pa 4686 A intensity ratio

Numerical results for He I (Milosavljevic´ and Djenizˇe, 2002a,b, 2003c) No.

Transition array

Multiplet

Wavelength ˚) (A

Temperature (K)

Electron density (1017cm3)

We ˚) (A

we/ wth

Acc.

Wt ˚) (A

Wi ˚) (A

A

D

Ref.

1.

2s–3p

3

3888.65

33,000

0.61

1.10

0.97

B+

1.39

.29

.196

1.26

31,500

0.82

1.45

0.96

B+

1.85

.40

.212

1.19

30,000

0.67

1.18

0.94

B+

1.49

.31

.202

1.25

28,000

0.44

0.78

0.93

B+

.96

.18

.181

1.37

18,000

0.50

0.83

0.88

B+

1.03

.20

.190

1.37

Milosavljevic´ and Djenizˇe (2002b) Milosavljevic´ and Djenizˇe (2002b) Milosavljevic´ and Djenizˇe (2002b) Milosavljevic´ and Djenizˇe (2002b) Milosavljevic´ and Djenizˇe (2002b)

S-3Po

A. Lesage / New Astronomy Reviews 52 (2009) 471–535

489

No.

Transition array

Multiplet

Wavelength ˚) (A

Temperature (K)

Electron density (1017 cm3)

We ˚) (A

wm/ wth

Wt ˚) (A

Wi ˚) (A

A

D

Acc.

Ref.

2.

1s2s–1s3p

1

5015.68

33,000

0.61

2.79

0.72

B+

4.52

1.73

.46

1.0

31,500

0.82

3.65

0.70

B+

6.02

2.37

.496

1.0

30,000

0.67

2.74

0.68

B+

4.81

1.87

.486

1.0

28,000

0.44

1.98

0.70

B+

3.12

1.14

.433

1.08

18,000

0.50

2.18

0.64

B+

3.32

1.14

.427

1.07

Milosavljevic´ and Djenizˇe (2002b) Milosavljevic´ and Djenizˇe (2002b) Milosavljevic´ and Djenizˇe (2002b) Milosavljevic´ and Djenizˇe (2002b) Milosavljevic´ and Djenizˇe (2002b)

33,000

0.61

2.34

0.76

B+

2.81

.47

.148

1.51

0.82

3.07

0.74

B+

3.72

.65

.160

1.42

0.67

2.50

0.75

B+

3.00

.50

.142

1.49

0.44

1.61

0.74

B+

1.90

.29

.136

1.65

0.5

1.79

0.77

B+

2.11

.32

.145

1.62

33,000

0.61

1.72

0.80

B+

2.10

.38

.163

1.46

31,500

0.82

2.18

0.75

B+

2.68

.50

.176

1.40

30,000

0.67

1.79

0.75

B+

2.18

.39

.167

1.46

28,000

0.44

1.26

0.81

B+

1.51

.25

.150

1.57

18,000

0.50

1.26

0.71

B+

1.50

.24

.156

1.60

33,000

0.61

3.71

0.66

B+

5.42

1.71

.342

1.0

0.82

4.81

0.66

B+

7.13

2.32

.368

1.0

0.67

4.07

0.67

B+

5.95

1.88

.352

1.0

0.44

2.61

0.66

B+

3.72

1.11

.317

1.0

0.5

2.86

0.66

B+

4.03

1.17

.335

1.0

16,000

0.07

1.06

0.65

B+

2.37

1.31

.917

1.0

14,500

0.09

1.45

0.68

B+

3.16

1.71

.911

1.0

14,000

0.08

1.20**

0.63

B+

2.58

1.38**

.883

1.0

12,500

0.03

0.48

0.69

B+

1.01

.53

.806

1.03

80,000

0.06

1.03

0.66

B+

2.03

1.00

.825

1.0

33,000

0.61

2.98

0.75

B+

4.81

1.83

.459

1.18

31,500

0.82

3.70

0.69

B+

6.28

2.58

.498

1.12

+

5.12

1.97*

.474

1.17

3.

4.

5.

6.

7.

2p–3s

2p–3d

1s2p–1s4s

2p–4d

2p–3d

S-1Po

3 o 3

P -S

3 o 3

P –D

3 o 3

P –S

3 o 3

P -D

1 o 1

P -D

7065.19

5875.7

4713.15

4471.5

6678.15

30,000

0.67

3.15

0.71

B

28,000

0.44

2.16

0.74

B+

3.37

1.21

.420

1.27

0.67

+

3.61

1.21

.413

1.26

18,000

0.5

2.40

B

Milosavljevic´ and Djenizˇe (2003c) Milosavljevic´ and Djenizˇe (2003c) Milosavljevic´ and Djenizˇe (2003c) Milosavljevic´ and Djenizˇe (2003c) Milosavljevic´ and Djenizˇe (2003c) Milosavljevic´ and Djenizˇe (2002a) Milosavljevic´ and Djenizˇe (2002a) Milosavljevic´ and Djenizˇe (2002a) Milosavljevic´ and Djenizˇe (2002a) Milosavljevic´ and Djenizˇe (2002a) Milosavljevic´ and Djenizˇe (2002b) Milosavljevic´ and Djenizˇe (2002b) Milosavljevic´ and Djenizˇe (2002b) Milosavljevic´ and Djenizˇe (2002b) Milosavljevic´ and Djenizˇe (2002b) Milosavljevic´ and Djenizˇe (2002a) Milosavljevic´ and Djenizˇe (2002a) Milosavljevic´ and Djenizˇe (2002a) Milosavljevic´ and Djenizˇe (2002a) Milosavljevic´ and Djenizˇe (2002a) Milosavljevic´ and Djenizˇe (2002a) Milosavljevic´ and Djenizˇe (2002a) Milosavljevic´ and Djenizˇe (2002a) Milosavljevic´ and Djenizˇe (2002a) Milosavljevic´ and Djenizˇe (2002a)

490

A. Lesage / New Astronomy Reviews 52 (2009) 471–535

Numerical results for He I (Milosavljevic´ and Djenizˇe, 2001) ID/ IA

Acc.

Ref.

7.2

.86

.55

B+

19

8.4

.85

.61

B+

0.67

15

6.9

.84

.57

B+

28,000

0.44

13

6.5

.80

.51

B+

18,000

0.50

14

6.2

.82

.54

B+

Milosavljevic´ and Djenizˇe (2001) Milosavljevic´ and Djenizˇe (2001) Milosavljevic´ and Djenizˇe (2001) Milosavljevic´ and Djenizˇe (2001) Milosavljevic´ and Djenizˇe (2001)

we

wt

a (Ne = 1016)

.06

1.02

We/ wth 2.03

Transition array

Multiple

Wavelength ˚) (A

Temperature (K)

Electron Density (1017 cm3)

Dk1/ ˚ 2(A)

DkAF ˚) (A

5.

2p–2d

3 0 3

4471.5

33,000

0.61

16

31,500

0.82

30,000

P–D

4471.0

wm/ wth

IF/IA

No.

6000

0.78

Milosavljevic´ and Djenizˇe (2001)

.937

Numerical results for He I (Pe´rez et al., 2003; Sreckovic´ et al., 2004b; Djenizˇe et al., 2005a) No.

Transition array

Multiple

Wavelength ˚) (A

Temperature (K)

Electron Density (1017 cm3)

wm ˚) (A

wm/ wth

˚) dm (A

dm/ dth

Acc.

Ref.

2.

2p–2d

3

S–3P0 P–S 3 0 3 P–D

3888.65 7065.19 3819.6028

17,000a 9000a 50,000

0.40 0.2 0.61

1.15a 1.1a 12.8

1.05 1.05

0.33a 0.65a 0.31 ± 0.05

1.18 1.18

B B+ B+

3 0 3

4026.186

52,000

1.3

6.4

Pe´rez et al. (2003) Pe´rez et al. (2003) Sreckovic´ et al. (2004b) Djenizˇe et al. (2005a)

3 0 3

6.

2p–6d

7.

2p–5d

a

P–D

1.24

B+

Estimated values from published graph.

Indium, In III Ground state: 1s22s22p63s23p63d104s24p64d105s2S1/2. Ionization energy: 28.03 eV = 226,077.11 cm1. Djenizˇe et al. (2006a) measured 16 doubly ionized indium spectral lines in a modified version of a linear low-pressure pulsed arc. Working gas was 90% helium plus small admixture of nitrogen and oxygen (7% and 3%, respectively). Spectroscopic observations were made end-on along the axis of the discharge tube. Indium atoms were evaporated from indium cylindrical plates located in the homogenous part of the discharge. Self-absorption was checked by comparison of the measured relative line intensity ratios with the calculated ones. Experimental values are higher than the tabulated ones, especially in the case of the In4032.32/In4062.30 ratio. In III line profiles were of the Voigt type, according to the authors this mean that the expected hyperfine structure splitting in the investigated In III has been overpowered by Stark and Doppler broadening. The Gaussian components due to Doppler effect and instrumental function were extracted from the Voigt observed profile by a computerized deconvolution technique based on the standard Davies and Vaughan (1963) deconvolution procedure using the least squares algorithm. Authors estimate an electron density accuracy of ±9% and of ±13% for the temperature, and they estimate the resulting error for the Lorentz fraction as being ±12%. As Djenizˇe et al. (2006a) In III line width measurement are the first ever done there is no possible comparison. Theoretical calculations for such heavy and doubly ionized ion are not yet available. Key data on experiments Ref.

Djenizˇe et al. (2006a)

Plasma source

Method of measurement

Modified low-pressure pulsed arc

Electron density ˚ line He II Pak 4686 A width

Remarks Temperature ˚ and In I k Relative intensity ratio between In II k 2941.04 A ˚ lines 2932.63 A

A. Lesage / New Astronomy Reviews 52 (2009) 471–535

491

Numerical results for In III No.

Transition

Wavelength ˚) (A

Temperature (K)

Electron density (1017 cm3)

wm ˚) (A

5s22 D5=2 –4f 2 F07=2

2154.08

13,000

1.48

5s22 D3=2 –4f 2 F05=2

2227.41

13,000

5d2 2 D3=2 –4f 2 F05=2

2982.80

5d22D5/2–4f2D3/2

wm/ wth

dm/ dth

dm ˚) (A

Acc.

Ref.

.175

B+

1.48

.140

B+

13,000

1.48

.240

B+

3008.08

13,000

1.48

.250

B+

5d2 2 D5=2 –4f 2 F07=2

3008.82

13,000

1.48

.210

B+

6p2 P01=2 –6dD 3=2

3852.82

13,000

1.48

.450

B+

6p2 P01=2 –7sS 1=2

4023.77

13,000

1.48

.545

B+

6p2 P03=2 –6dD 5=2

4032.32

13,000

1.48

.515

B+

6p2 P03=2 –6dD 3=2

4062.30

13,000

1.48

.555

B+

6p2 P03=2 –7s2 S1=2

4252.68

13,000

1.48

.480

B+

5s22 D3=2 –6p2 P01=2

4509.58

13,000

1.48

.490

B+

6s2 S1=2 –6p2 P03=2

5248.77

13,000

1.48

.717

B+

6s2 S1=2 –6p2 P01=2

5645.15

13,000

1.48

.520

B+

5d2 D3=2 –6p2 P03=2

5723.17

13,000

1.48

.450

B+

5d2D5/2–6p2P3/2

5819.50

13,000

1.48

.520

B+

5d2 D3=2 –6p2 P01=2

6197.72

13,000

1.48

.800

B+

Djenizˇe (2006a) Djenizˇe (2006a) Djenizˇe (2006a) Djenizˇe (2006a) Djenizˇe (2006a) Djenizˇe (2006a) Djenizˇe (2006a) Djenizˇe (2006a) Djenizˇe (2006a) Djenizˇe (2006a) Djenizˇe (2006a) Djenizˇe (2006a) Djenizˇe (2006a) Djenizˇe (2006a) Djenizˇe (2006a) Djenizˇe (2006a)

et al. et al. et al. et al. et al. et al. et al. et al. et al. et al. et al. et al. et al. et al. et al. et al.

Iron, Fe I Ground state: 1s22s22p63s23p63d64s25D4. Ionization energy: 7.9024 eV = 63,737.1 cm1.

Key data on experiments Ref.

Plasma source

Method of measurement

Remarks

Electron density

Temperature

Aragon et al. (2004)

Laser induced plasma

˚ and Fe I k Stark width of Al II k 2816.18 A ˚ lines 5383.37 A

Boltzmann slope of line intensity ratio

Temperature provided by a two dimensional picture

Numerical results for Fe I No.

Transition array

Multiplet

Wavelength ˚) (A

Temperature (K)

Electron density (1017 cm3)

wm ˚) (A

1.

(4F)4s–(4F)4p

a3F– y3D0

3827.82

12,000

1.0

0.13

wm/ wth

dm ˚) (A

dm/ dth

Acc.

Ref.

B

Aragon et al. (2004)

˚ Fe I line in a laser-induced plasma. The plasma was generated in air Aragon et al. (2004) have measured the k 3827.83 A at atmospheric pressure by focusing a 4.5 ns, 100 mJ laser pulse on a Fe–Ni–Al alloy. Fifty laser shots were accumulated for each measurement. The spectra were time and space resolved. Vertical and horizontal resolutions were obtained with a spectrometer coupled with a CCD intensified detector. The plasma emission was integrated along the line of sight. Special

492

A. Lesage / New Astronomy Reviews 52 (2009) 471–535

care was taken to check optical thinness by measuring line intensities at different concentrations of iron. An Abel inversion procedure described in Aguilera et al. (2003) was used to transform the intensity distributions integrated along the line of sight into emissivity distributions. The authors do not ascribe a particular temperature to their Fe I line width measurement, a two dimensional figure shows the emissivity and temperature distribution in the plasma. A detailed electronic temperature determination is provided by Aguilera and Aragon (2004). Bengoechea et al. (2005) have experimentally shown that the static Stark ion effect has to be taken into account for the k ˚ line width and shift. For electron density 4–15  1016 cm3, the ion’s influence on the total broadening was 15– 5383.4 A 20%. As the electronic density, in their experiment, is obtained by using the Stark parameter of the line under investigation, Bengoechea et al. (2005) results are not reported here. Krypton, Kr I Ground state: 1s22s22p63s23p63d104s24p61S0. Ionization energy: 13.9996 eV = 112,914.35 cm1.

Key data on experiments Ref.

Plasma source

Milosavljevic´ et al. (2003a)

Linear lowpressure pulsed arc Linear flash-tube

Valognes et al. (2005) Ivkovic´ et al. (2006)

Method of measurement

Linear lowpressure pulsed arc

Remarks

Electron density

Temperature

˚ Single wavelength laser interferometer at 6328 A

Saha equation applied to KrII/KrI intensity ratio and special line deconvolution procedure

Radial profile of particle densities deduced from measurement of the optically thick lines ˚ line and Separation of maxima of the He I 4471 A its forbidden component

Radial profile of temperature deduced from measurement of the optically thick lines Boltzmann plot and transition probabilities of seven Kr II lines

Numerical results for Kr I (wm for Milosavljevic´ et al. (2003a) is the electronic component only) Transition array

Multiplet

Wavelength ˚) (A

Temperature (K)

1.

5s–5p

[3/2]o–[1/2] [3/2]o–[3/2]

7587.41 7601.54 7694.54 8190.05 8298.11 8104.36

17,000 17,000 17,000 17,000 17,000 17,000 21,000 17,000

1.65 1.65 1.65 1.65 1.65 1.65 0.83 1.65

1.644 1.464 1.218 1.607 1.542 1.752 1.30 1.576

17,000 17,000 17,000 16,100 16,950 17,550

1.65 1.65 1.65 13.3 17.7 22.8

1.458 1.276 1.30 7.80 9.90 12.15

8281.05 7685.24 7854.82 8263.24 8059.50

17,000 17,000 17,000 17,000 17,000

1.65 1.65 1.65 1.65 1.65

1.585 1.431 1.498 1.579 1.391

[3/2]o–[5/2]

8112.90 2.

3.

0

5s–5p

5s0 -5p0

o

[3/2] –[1/2] [3/2]o–[3/2] [3/2]o–[3/2]

[1/2]o–[1/2]

o

[1/2] –[3/2]

5570.29 5562.22 5870.91

Electron density (1017 cm3)

wm ˚) (A

No.

4.

5s-6p

[3/2]o–[1/2] [3/2]o–[3/2] [3/2]o–[3/2] [3/2]o–[5/2]

4362.64 4273.97 4463.69 4319.58

17,000 17,000 17,000 17,000

1.65 1.65 1.65 1.65

3.252 4.237 3.483 3.280

5.

5s0 -6p0

[1/2]o–[1/2]

4351.36

17,000

1.65

4.699

wm/ wth

˚) dm (A

0.64 0.80 0.64 0.71 0.71 0.90 1.00 0.82

2.65 ± 0.15 3.50 ± 0.20 4.35 ± 0.30

0.84 1.08 0.84 0.86

dm/ dth

Acc.

Ref.

B+ B+ B+ B+ B+ B+ A B+

Milosavljevic´ et al. (2003a) Milosavljevic´ et al. (2003a) Milosavljevic´ et al. (2003a) Milosavljevic´ et al. (2003a) Milosavljevic´ et al. (2003a) Milosavljevic´ et al. (2003a) Ivkovic´ et al. (2006) Milosavljevic´ et al. (2003a)

B+ B+ B+ B+ B+ B+

Milosavljevic´ et al. (2003a) Milosavljevic´ et al. (2003a) Milosavljevic´ et al. (2003a) Valognes et al. (2005) Valognes et al. (2005) Valognes et al. (2005)

B+ B+ B+ B+

Milosavljevic´ et al. (2003a) Milosavljevic´ et al. (2003a) Milosavljevic´ et al. (2003a) Milosavljevic´ et al. (2003a) Milosavljevic´ et al. (2003a)

B+ B+ B+ B+

Milosavljevic´ et al. (2003a) Milosavljevic´ et al. (2003a) Milosavljevic´ et al. (2003a) Milosavljevic´ et al. (2003a)

B+

Milosavljevic´ et al. (2003a)

A. Lesage / New Astronomy Reviews 52 (2009) 471–535

493

Milosavljevic´ et al. (2003a) have measured, end-on, 20 Kr I Stark widths in a modified linear pulsed arc (Djenizˇe et al., 1991c; Djenizˇe et al., 1998). Self-absorption is checked using the intensity ration method described in Djenizˇe and Bukvic´ (2001) A new deconvolution method (Milosavljevic´ and Poparic´, 2001) allows direct determining of electron density and temperature and of the electronic and ionic component of the line profiles. The Ne and T values obtained with a laser interferometer and with Saha equation applied to KrI/KrII lines intensity ratio are in close agreement with those obtained with their above mentioned method. Comparison of the measured electronic and ionic contribution to the total line widths of Kr I lines, with those calculated with the semi-classical perturbation formalism (Dimitrijevic´ et al., 1991) shows the influence of the quasi-static ion and ion-dynamic effects on the investigated KrI line shapes. The separate electron and ion contributions to the total Stark width are provided for the first time by the authors, but the electron one only is reported in the present table. For comparison with previous measurements and calculated values the reader is reported to the original article (Milosavljevic´ et al., 2003a). Nevertheless, the data published by Schinko¨th et al. (1999) for 11 Kr I lines are in close agreement with those of Milosavljevic´ et al. (2003a). ˚ Kr I lineshape in a linear flash-tube (l = 100 mm, d = 5 mm) created Valognes et al. (2005) measured the 5870.90 A plasma, in pure krypton at initial pressure of 200 Torr. Observations are done side-on during a period of time of 1 ls at the current maximum, considered as being the quasi-stationary phase of the plasma. A high resolution spectrograph records the continuum and the Kr I line profiles on an optical multichanel analyser. Absolute calibration is performed with ˚ and a tungsten ribbon lamp for k < 3800A ˚ . Radial profiles of temperature and particles a deuterium lamp for k < 3800 A densities measurements are based on optically thick line intensities and on the transverse distribution of continuum intensities. Abel inversion provides the radial functions of the emission coefficient. The Saha equation and Dalton law are then applied for each radial position. Radial profiles deduced are, according to the authors, practically flat over one half of the diameter. Profiles are corrected from optical thickness by using a concave mirror. The observed profile is corrected from the apparatus contribution. Doppler and van der Waals profiles are neglected. A profile is calculated by taking into account the radial profiles of particles and temperature on the basis of a linear variation of the Stark parameters versus electron densities. The authors consider that a good fit of the experimental Lorentzian profile to the calculated one proves that the measured width and shift are mainly due to the part of the plasma where the radial profile of electron density and temperature is flat and the contributions from the cold layers are weak. Valognes et al. (2005) present calculations done with a method using the N-N approximation for many electron atoms and the possibility to estimate the contribution of interacting levels of like and unlike parentage. The comparison between their measured and calculated values is within mutual error bar. ˚ line in similar experimental conditions as Milosavljevic´ et al. (2003a) Ivkovic´ et al. (2006) have measured the k 8104.36 A but the krypton is gradually diluted with helium and hydrogen (5% Kr + 8% He + 87% H2, total pressure 8 mb) until optically thin conditions prevails. The line profile (close to the symmetric one) was corrected for Doppler and apparatus ˚ ) contributions. The Davies and Vaughan (1963) deconvolution procedure was applied to obtain the Lorenzian (wi = 0.17 A component. The measured value (at 21000 K) is 57% larger than in Milosavljevic´ et al. (2003a) (at 17000 K). Ivkovic´ et al. (2006) ‘‘reference experiment” confirm the doubt about possible boundary effect due to the geometry of the plasma and the way it is observed. Krypton, Kr II Ground state: 1s22s22p63s23p63d104s24p5 2P03/2 Ionization energy: 24.360 eV = 196 474.8 cm1 de Castro et al. (2001) have measured 25 Kr II lines in a pulsed discharge lamp end-on with an optical multichannel analyzer (OMA). Self-absorption was checked with and without mirrors and was found to be negligible. Their values are compared with previous ones obtained at a lower temperature and are found to be in agreement with most of them within the error bars. Their calculated statistical error is lower than any of the indicated previous ones. As the accuracy is calculated by the authors for each line width and shift value, their values are reported in the accuracy column in percent instead of the conventional letter. As can be noted they are all (except some for the shift accuracy) lower than or equal to 15%; then the A letter would have been used instead of the authors’ numbers. Key data on experiments Ref. de Castro et al. (2001)

Plasma source Pulsed discharge lamp

Method of measurement Electron density

Temperature

Remarks

Two wavelengths interferometer and Stark width of He I ˚ 3886.5 A

Slope of Boltzman plot of Kr II lines

494

A. Lesage / New Astronomy Reviews 52 (2009) 471–535

Numerical results for Kr II No.

Transition array

Multiplet

Wavelength ˚) (A

Temperature (K)

Electron density (1017 cm3)

wm ˚) (A

1.

5s–5p

4

4739.00 4658.88 4832.08 5208.32 5308.66 5992.22

16,000-24,500 16,000-24,500 16,000-24,500 16,000-24,500 16,000-24,500 16,000-24,500

1.0 1.0 1.0 1.0 1.0 1.0

0.341 0.32 0.378 0.394 0.508 0.518

2.

4

4355.48 4765.74 4292.92 4811.76 4431.69

16,000-24,500 16,000-24,500 16,000-24,500 16,000-24,500 16,000-24,500

1.0 1.0 1.0 1.0 1.0

3.

4

4436.81 4145.12

16,000-24,500 16,000-24,500

P–4Po

P–4Do

P–2Po P–4So

4

wm/ wth

˚) dm (A

dm/ dth

Acc. %

Ref.

0.054 0.06 0.056 0.090 0.078 0.076

10-4 6-5 5-18 10-4 6-7 10-13

de de de de de de

Castro Castro Castro Castro Castro Castro

et et et et et et

al. al. al. al. al. al.

(2001) (2001) (2001) (2001) (2001) (2001)

0.291 0.415 0.336 0.442 0.306

0.038 0.039 0.039 0.032 0.056

6-66 7-8 5-8 11-32 4-18

de de de de de

Castro Castro Castro Castro Castro

et et et et et

al. al. al. al. al.

(2001) (2001) (2001) (2001) (2001)

1.0 1.0

0.381 0.320

0.083 0.013

7-7 11-35

de Castro et al. (2001) de Castro et al. (2001)

3754.24

16,000-24,500

1.0

0.224

0.054

9-6

de Castro et al. (2001)

5.

2

4846.61 4615.29

16,000-24,500 16,000-24,500

1.0 1.0

0.371 0.365

0.055 0.028

5-4 4-13

de Castro et al. (2001) de Castro et al. (2001)

6.

2

4762.44 4619.17

16,000-24,500 16,000-24,500

1.0 1.0

0.406 0.352

0.024 0.038

5-33 5-5

de Castro et al. (2001) de Castro et al. (2001)

7.

2

4300.49 4825.18

16,000-24,500 16,000-24,500

1.0 1.0

0.327 0.424

0.051 0.056

8-38 6-22

de Castro et al. (2001) de Castro et al. (2001)

4857.20

16,000-24,500

1.0

0.531

0.105

8-15

de Castro et al. (2001)

3783.09 3778.05

16,000-24,500 16,000-24,500

1.0 1.0

0.964 0.966

0.325 0.314

6-4 5-5

de Castro et al. (2001) de Castro et al. (2001)

0.106

8-23

de Castro et al. (2001)

6-5

de Castro et al. (2001)

4. P–2Po P–2Do P–4So

4d-5p

4

9.

5p–5d

4

10.

5p-4d0

4 o 2

3771.34

16,000-24,500

1.0

0.366

11.

0

2 o 2

3718.02

16,000-24,500

1.0

1.093

8.

D–2So o 4

D –F P –S

0

5p –5d

F –G

0.3137

Lead, Pb II Ground state: 1s2 2s2 2p6 3s2 3p6 3d10 4s2 4p6 4d10 4f 14 5s2 5p6 5d10 6s2 6p2 P01=2 . Ionization energy: 15.0322 eV = 121,243 cm1. Colon and Alonso-Medina (2006) measured 31 Pb II lines in a laser produced plasma, at 1.4  1010 W cm2, on lead targets, in argon atmosphere. A Czerny–Turner spectrograph observed, side-on, the plasma plume. Resolution of the spec˚ . The instrumental contribution was included in the unfolding process. The spectra were troscopic system was 0.3 A recorded by a time-resolved optical multichannel analyzer (OMA III, EG&G). The analysis of the spectral lines (obtained after Abel inversion of the integrated intensity) was made by fitting the observed line shapes to numerically generated Voigt profiles. No mention is made of the van der Waals and Doppler effects. Self absorption was checked. The optical depth ˚ line for which lower concentrations of lead were used. For the electron dendoes not exceed 0.02, except for the 2203.53 A sity measurement, Miller et al. (1979a) and Puric´ et al. (1985) values were used, while the later ones by Djenizˇe et al. (1992a) and Fishman et al. (1994) were ignored. McWhite’s criterion has been used to support the LTE hypothesis. Colon and Alonso-Medina (2006) measured values agree with the experimental trend, versus temperature obtained with Djenizˇe ˚ line, where et al. (1992a), Miller et al. (1979a), Fishman et al. (1994), Salakov et al. (1985) values, except for the 2203.5 A Djenizˇe et al. (1992a) value is much less. Comparison is made with Colon and Alonso-Medina (2002) calculated values which are in good agreement with their measured ones, with the exception of the lines that involve the 5f configuration. ˚ line. Note that according to the authors: ‘‘The possible error Nevertheless a remarkable discrepancy exists for the 2203.5 A Key data on experiments Ref.

Colon and AlonsoMedina (2006)

Plasma source

Pulsed Nd-YAG laser, 10 ns, 20 Hz, 275 mJ

Method of measurement

Remarks

Electron density

Temperature

Known Stark parameters of Pb II: 5042.6, ˚ 5372.3 A ˚ lines 5544.3, 4386.5, 4244.9 A

Boltzman plot of five Pb II: 3455.1, 4152.8, ˚ 4386.5, 5608.9 A ˚ lines 5024.6 A

A. Lesage / New Astronomy Reviews 52 (2009) 471–535

495

Numerical results for Pb II No.

Transition array

Multiplet

Wavelength ˚) (A

Temperature (K)

Electron density (1017 cm3)

wm ˚) (A

wm =wth a

1. 2. 3.

6p–7s 7p–8s 7p–9s

4.

7p–10s

5.

7s–7p

2 0 P3=2 –2 S1=2 2 0 P1=2 –S1=2 2 0 P1=2 –2 S1=2 2 0 P3=2 –S1=2 2 0 P1=2 –2 S1=2 2 0 P3=2 –2 S1=2 2 S1=2 –2 P01=2

6p2–7p

11,300 11,300 11,300 11,300 11,300 11,300 11,300 11,300 11,300 11,300 11,300 11,300 11,300 11,300 11,300 11,300 11,300 11,300 11,300 11,300 11,300 11,300 11,300 11,300 11,300 11,300 11,300 11,300 11,300 11,300 11,300

0.1 0.1 0.1 0.1 0.1 0.1 0.1 0.1 0.1 0.1 0.1 0.1 0.1 0.1 0.1 0.1 0.1 0.1 0.1 0.1 0.1 0.1 0.1 0.1 0.1 0.1 0.1 0.1 0.1 0.1 0.1

0.11 0.22 .33 0.32 0.21 0.17 0.12 0.14 0.16 0.19 0.076 0.20 0.19 0.17 0.39 0.36 0.34 0.35 0.25 0.41 0.13 0.19 0.19 0.18 0.22 0.20 0.28 0.32 0.24 0.11 0.30

8.8 0.6 1.2 0.8 0.4 .27 .70 .71

6.

2203.534 6791.2 3718.3 4152.82 2986.87 3260.9 6660.0 5608.85 6041.17 5163.3 2805.9 2717.4 3945.7 3665.5 5042.6 5876.6 5544.3 3455.1 3827.2 3713.9 4386.5 4242.14 4244.92 3785.9 5367.64 5372.099 3016.39 2947.43 2948.53 2719.8 3451.7

P1=2 –2 P01=2 P1=2 –2 P03=2 2 S1=2 –2 P01=2 2 S1=2 –2 P03=2 4 P1=2 –2 P01=2 4 P1=2 –2 P03=2 2 0 P1=2 –2 D3=2 2 0 P3=2 –2 D3=2 2 0 P3=2 –2 D5=2 2 D3=2 –2 P01=2 2 D3=2 –2 P03=2 2 D5=2 –2 P03=2 2 D3=2 –2 F05=2 2 D3=2 –2 F05=2 2 D3=2 –2 F05=2 4 P1=2 –2 F05=2 4 P5=2 –2 F05=2 4 P5=2 –2 F07=2 2 D3=2 –2 F05=2 2 D5=2 –2 F05=2 2 D5=2 –2 F07=2 4 P3=2 –2 F05=2 4 P5=2 –2 F07=2 4 4

7.

7s–8p

8.

6p2–8p

9.

7p–7d

10.

7d–8p

11.

6d–5f

12.

6p2–5f

13.

6d–6f

14.

6p2–6f

a

.61 .96

.93 .72

.48 .81 .66 .56 .42

dm ˚) (A

dm/ dth

Acc.

Ref.

D D D D D D D D D D D D D D D D D D D D D D D D D D D D D D D

Colon Colon Colon Colon Colon Colon Colon Colon Colon Colon Colon Colon Colon Colon Colon Colon Colon Colon Colon Colon Colon Colon Colon Colon Colon Colon Colon Colon Colon Colon Colon

and and and and and and and and and and and and and and and and and and and and and and and and and and and and and and and

Alonso-Medina Alonso-Medina Alonso-Medina Alonso-Medina Alonso-Medina Alonso-Medina Alonso-Medina Alonso-Medina Alonso-Medina Alonso-Medina Alonso-Medina Alonso-Medina Alonso-Medina Alonso-Medina Alonso-Medina Alonso-Medina Alonso-Medina Alonso-Medina Alonso-Medina Alonso-Medina Alonso-Medina Alonso-Medina Alonso-Medina Alonso-Medina Alonso-Medina Alonso-Medina Alonso-Medina Alonso-Medina Alonso-Medina Alonso-Medina Alonso-Medina

(2006) (2006) (2006) (2006) (2006) (2006) (2006) (2006) (2006) (2006) (2006) (2006) (2006) (2006) (2006) (2006) (2006) (2006) (2006) (2006) (2006) (2006) (2006) (2006) (2006) (2006) (2006) (2006) (2006) (2006) (2006)

wm/wth according to Colon and Alonso-Medina (2002).

due the experimental uncertainty in the density of electrons in this study is not included”. As in the 1984 and 1990 issues of Konjevic´ et al. (1984a,b) and Konjevic´ and Wiese (1990) critical reviews, the estimated Stark parameter uncertainty was C, that explains why we put the D one in. Lead, Pb III Ground state: 1s22s22p63s23p63d104s24p64d104f145s25p65d106s21S0. Ionization energy:31.9373 eV = 257,591.607 cm1. Alonso-Medina and Colon (2007) observed the emission lines from a laser induced plasma Alonso-Medina (1997), Alonso-Medina and Herran-Martinez (2001), Colon and Alonso-Medina (2006) and Colon et al. (1999). Stark widths of ten Pb III lines have been measured. The plasma was generated by a Q-switched Nd:YAG laser (290 Mj pulses of ˚ ) focused on the lead sample in an argon atmosphere at 12 Torr. A Czerny–Turner spectrom7 ns at 20 Hz and k 10640 A ˚ eter (0.3 A resolution) equipped with a time-resolved multichannel analyzer allows the recording of the spectra at preset delays from the laser pulse, with a selected time length. The analysis of the spectral lines (obtained after Abel inversion of the integrated intensity) was made by fitting the observed line shapes to numerically generated Voigt profiles. No Key data on experiments Ref.

Plasma source

AlonsoMedina and Colon (2007)

Pulsed Nd-YAG laser, 10 ns, 20 Hz, 275 mJ

Method of measurement

Remarks

Electron density

Temperature

Known Stark parameters of Pb II: ˚ and Ar II 5608.9, 5544.3, 4244.9 A ˚ lines 4806.0 A

˚ , Pb Boltzman plot of Pb II: 5042.6, 5372.3, 5608.9, 6660.0 A ˚ , Ar II 3841.5, 4131.7, 3850.6, III 3854.1, 4761.1, 4798.6 A ˚ lines 4847.8 A

496

A. Lesage / New Astronomy Reviews 52 (2009) 471–535

Numerical results for Pb III No.

Transition array

Multiplet

Wavelength ˚) (A

Temperature (K)

Electron density (1017 cm3)

wm ˚) (A

1.

7s–7p

3

S1–3P0

4798.59

25,200

1

3

S1–3P1

4761.12

25,200

3

S1–3P2

3854.08

3

S0–3P1

1

2.

6d–7p

6p2–7p

3.

wm/ wth

dm ˚) (A

dm/ dth

Acc.

Ref.

1.0

B

1

1.0

B

25,200

1

0.75

B

5779.41

25,200

1

2.9

B

D2–3P1

5207.10

25,200

1

2.2

B

1

D2–3P2

4141.59

25,200

1

2.7

B

3

D1–3P2

5280.12

25,200

1

2.7

B

3

D2–3P2

5523.97

25,200

1

2.4

B

1

D3–3P2

5857.96

25,200

1

1.1

B

1

D1–3P2

4855.06

25,200

1

1.4

B

Alonso-Medina Colon (2007) Alonso-Medina Colon (2007) Alonso-Medina Colon (2007) Alonso-Medina Colon (2007) Alonso-Medina Colon (2007) Alonso-Medina Colon (2007) Alonso-Medina Colon (2007) Alonso-Medina Colon (2007) Alonso-Medina Colon (2007) Alonso-Medina Colon (2007)

and and and and and and and and and and

mention is made of the van der Waals and Doppler effects, but it seems that the first is considered as being negligible and the second taken in account for the Gaussian contribution. Self absorption was checked. Authors calculated that, according to their experimental conditions, the optical depth is negligible. No comparison is made with previous measurement and theoretical prediction. Magnesium Mg I Ground state: 1s22s22p63s21S0. Ionization energy: 7.6462 eV = 61,671.02 cm1. Djenizˇe et al. (2004a) used a linear low-pressure arc to measure, end-on, six astrophysically important Mg I lines. Magnesium was introduced through erosion of magnesium metal bands fixed on the discharge electrodes. The working gas was helium at 532 Pa in a flowing regime. The line profiles were recorded by a step-by-step technique. The absence of self absorption was checked by the technique described in Djenizˇe and Bukvic´ (2001). The standard Davies and Vaughan (1963) deconvolution procedure was applied using the least square algorithm. The ion broadening contribution as well Key data on experiments Ref.

Plasma source

Method of measurement

Remarks

Electron density

Temperature

Djenizˇe et al. (2004a)

Low-pressure pulsed arc

Single wavelength laser interferometer

He II/He I intensity ratio

Numerical results for Mg I No.

Transition array

Multiplet

Wavelength ˚) (A

Temperature (K)

Electron density (1017 cm3)

wm ˚) (A

1.

3s3p–3s4s

3 0 3

5183.6043

49,500

1.0

0.350

5172.6844

49,500

1.0

5167.3213

49,500

3838.2919

2.

3.

3s3p–3s3d

2p63s2–3s3p

P–S

3 0 3

P–D

wm/ wth

˚) dm (A

dm/ dth

Acc.

Ref.

0.074

B+

0.353

0.084

B+

1.0

0.330

0.090

B+

59,460

1.0

1.10

0.020

B+

3832.3039

59,460

1.0

0.92

0.035

B+

2852.1261

43,460

1.0

.

0.018

B+

Djenizˇe (2004a) Djenizˇe (2004a) Djenizˇe (2004a) Djenizˇe (2004a) Djenizˇe (2004a) Djenizˇe (2004a)

et al. et al. et al. et al. et al. et al.

A. Lesage / New Astronomy Reviews 52 (2009) 471–535

497

as the van der Waals and resonance broadening were neglected. The calculated width values by Griem (1974) and by Dimitrijevic´ and Sahal-Bre´chot (1994, 1995a, 1996a) are in good agreement with measurements by Djenizˇe et al. (2004a) for the 3p–3d transition lines and lie far below the theoretical values for the 2p63s2–3s3p and 3s3p–3s4s transition lines. Magnesium, Mg II Ground state: 1s22s22p63s2S1/2. Ionization energy: 15.04 eV = 121,267.61 cm1. Djenizˇe et al. (2004b) used a linear low-pressure arc to measure, end-on, Mg II UV multiplet lines. Magnesium was introduced through erosion of magnesium metal bands fixed on the discharge electrodes. The working gases were helium at 532 Pa or a mixture of 72% argon and 28% helium or oxygen at 133 Pa, in flowing regime. Line profiles were recorded by a step-bystep technique. Absence of self absorption was checked by the technique described by Djenizˇe and Bukvic´ (2001) for the 2 and 3 UV multiplet lines. Presence of self-absorption for the multiplet 1 UV prevent the authors to provide width measurement for these lines. The standard Davies and Vaughan (1963) deconvolution procedure was applied using the least squares algorithm. van der Waals and resonance broadening were neglected. Calculated width values by Griem (1974) and by Dimitrijevic´ and Sahal-Bre´chot (1995b) are in agreement with Djenizˇe et al. (2004b) measurements. The measured shift values are in better agreement with those calculated by Dimitrijevic´ and Sahal-Bre´chot (1995b) than with those of Griem (1974). Bukvic´ et al. (2004a) used the same source as Djenizˇe et al. (2004b); the working gas was a helium–oxygen (1/1.1) mixture in flowing regime at 266 Pa pressure. Good agreement is found with results of the semi-classical theory as calculated by Key data on experiments Ref.

Plasma source

Djenizˇe et al. (2004b) Bukvic´ et al. (2004a) Djenizˇe et al. (2005b)

Low-pressure pulsed arc Low-pressure pulsed arc Low-pressure pulsed arc

Method of measurement

Remarks

Electron density

Temperature

Single wavelength laser ˚ interferometer at k 6328 A ˚ O III Stark width of k 2983.8 A spectral line Single wavelength laser interferometer

He II/He I intensity ratios for helium plasma Saha equations applied to O III, O II, Ar III, Ar II lines Saha equations applied to O III, O II, spectral lines Boltzmann plot of relative intensities of six N II lines: k 4035, 4041, ˚ 4044, 3956, 3995 and 3919 A

Numerical results for Mg II No.

Transition array

Multiplet

Wavelength ˚) (A

Temperature (K)

Electron density (1017 cm3)

1.

3s–3p

2

2795.528

30,000 42,000 52,000 26,000 30,000 42,000 52,000 26,000 30,000 42,000 52,000 30,000 42,000 52,000 30,000 42,000 52,000 26,000 30,000 42,000 52,000 26,000 16,900 – –

1.0 1.0 1.0 1.1 1.0 1.0 1.0 1.1 1.0 1.0 1.0 1.0 1.0 1.0 1.0 1.0 1.0 1.1 1.0 1.0 1.0 1.1 1.35 – –

S–2P0

2802.705

2.

3p–4s

2 0 2

P–S

2928.633

2936.510

3.

3p–3d

2 0 2

P–D

2790.777

2797.998

4.

3d–4f

2

D–2F0

4481.126 4481.150 4481.325

wm ˚) (A

0.096

0.104 .29 .206 .197 .30 .206 .197 .166 .137 .153 .178 .166 .137 .153 .158 2.95 – –

wm/ wth

˚) dm (A .01 .005 .015 0.0072 .002 .004 .005 0.0066 .057 .039 .096 .068 .037 .125 .020 .030 .026 .024 .013 .017 .019 .021 .085 – –

dm/ dth

Acc.

Ref.

B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+

Djenizˇe et al. (2004b) Djenizˇe et al. (2004b) Djenizˇe et al. (2004b) Bukvic´ et al. (2004a) Djenizˇe et al. (2004b) Djenizˇe et al. (2004b) Djenizˇe et al. (2004b) Bukvic´ et al. (2004a) Djenizˇe et al. (2004b) Djenizˇe et al. (2004b) Djenizˇe et al. (2004b) Djenizˇe et al. (2004b) Djenizˇe et al. (2004b) Djenizˇe et al. (2004b) Djenizˇe et al. (2004b) Djenizˇe et al. (2004b) Djenizˇe et al. (2004b) Bukvic´ et al. (2004a) Djenizˇe et al. (2004b) Djenizˇe et al. (2004b) Djenizˇe et al. (2004b) Bukvic´ et al. (2004a) Djenizˇe et al. (2005b) – –

498

A. Lesage / New Astronomy Reviews 52 (2009) 471–535

Griem (1974), Chapelle and Sahal-Bre´chot (1970) and Dimitrijevic´ and Sahal-Bre´chot (1998). Apart from those of Roberts and Barnard (1972) and those of Goldbach et al. (1982), the previous measured values by Chapelle and Sahal-Bre´chot (1970), Jones et al. (1972) and Hadziomerspahic et al. (1973) are within the error limits. The authors estimate their Stark ˚. shifts error bar as being ±0.008 A Djenizˇe et al. (2005b) measured the Stark width and shift of three Mg II lines in a linear low pressure pulsed arc. Magnesium was introduced through erosion of magnesium metal bands fixed on the discharge electrodes. The working gas was nitrogen at 133 Pa in flowing regime. No measure of the optical depth of the plasma for the lines has been done, the authors refer to previous publications Djenizˇe et al. (2004a,b), Bukvic´ et al. (2004a), to state that the low density of Mg II ions due to the method of introduction provided conditions free of self-absorption. Spectroscopic observation was made end-on and line profiles were recorded by a step-by-step technique. The standard Davies and Vaughan (1963) deconvolution procedure was applied using the least squares algorithm. van der Waals and resonance broadening were neglected. Djenizˇe et al. (2005b) measured width values are in agreement with those of Chapelle and Sahal-Bre´chot (1970) and disagree with those of Helbig and Kusch (1972). Agreement is within error bar with Griem (1974), Dimitrijevic´ and Sahal-Bre´chot (1995b) cal˚ (0.108 A ˚ at T = 10,000 K) is much higher than preculated values. Kusch and Scweicker (1976) width value for k 4481.2 A vious results, and the shift is negative as predicted by Griem (1974), while Djenizˇe et al. (2005b) value is in good agreement with Dimitrijevic´ and Sahal-Bre´chot (1995b) calculated value. Manganese, Mn I Ground state: 1s22s22p63s23p63d54s26S5/2. Ionization energy: 7.43402 eV = 59,959.4 cm1. Srec´kovic´ et al. (2007) measured 12 neutral manganese spectral lines in a low pressure pulsed discharge (inner diameter 5 mm and plasma length 14 cm) on a shot to shot basis. Observations were made end-on. Manganese was introduced in a helium plasma by eroding of manganese metal bands fixed on discharge electrodes. The working gas was helium flowing at 665 Pa. Self absorption was checked using the method described in Djenizˇe and Bukvic´ (2001), authors did not mention any correction. van der Waals and resonance broadening were neglected. The standard (Davies and Vaughan, 1963) deconvolution procedure was applied using the least squares algorithm. The hyperfine structure splitting in Mn I contributes sig˚ for the experimental temperature. Despite the nificantly to the Doppler broadening and is estimated to be about 0.084 A high resolving power of their spectrograph, the authors are unable to monitor the Stark effect of a particular hyperfine structure splitting component. Consequently their measured Stark widths are associated with this ‘‘averaged” spectral line. Authors expect a Mn II ion contribution to the Stark width of the order of 5%, hardly distinguishable from the noise, giving symmetrical Mn I line profiles. This approximation results in measured Stark width accuracy values of ±22% according to the authors. The measured Stark parameter values are 1.7–3.0 times larger than the hyperfine structure splitting. Key data on experiments Ref.

Plasma source

Method of measurement

Srec´kovic´ et al. (2007)

Low-pressure pulsed arc

Electron density ˚ Stark width He II Pa 4686 A

Remarks Temperature ˚ /He I 5876 A ˚ lines Relative intensity ratio of He II 4686 A

Numerical results for Mn I No.

Multiplet

Wavelength ˚) (A

Temperature (K)

Electron density (1017 cm3)

wm ˚) (A

1

a6S–z6P0

2.

a6S–y6P0

3.

a6D– z6D0

4.

a6D– x6P0 z8P0–e8S

4030.753 4033.062 4034.483 2794.817 2798.269 2801.081 4041.355 4048.743 4055.544 3577.868

47,000 47,000 47,000 47,000 47,000 47,000 47,000 47,000 47,000 47,000

.66 .66 .66 .66 .66 .66 .66 .66 .66 .66

4783.427 4823.524

47,000 47,000

.66 .66

5.

wm/wth (Konjevic´ and Roberts, 1976)

dm ˚) (A

dm/dth (Konjevic´ and Roberts, 1976)

Acc.

Ref.

.148 .160 .120 .040 <.030 <.030 .132 .148 .124 .040

B B B B B B B B B B

Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´

.126 .160

B B

Srec´kovic´ et al. (2007) Srec´kovic´ et al. (2007)

et et et et et et et et et et

al. al. al. al. al. al. al. al. al. al.

(2007) (2007) (2007) (2007) (2007) (2007) (2007) (2007) (2007) (2007)

A. Lesage / New Astronomy Reviews 52 (2009) 471–535

499

Manganese, Mn II Ground state: 1s22s22p63s23p63d54s7S3. Ionization energy: 15.6400 eV = 126,145.0 cm1. Djenizˇe et al. (2006b) measured 11 singly-ionized manganese spectral lines in a low pressure pulsed discharge on a shot to shot basis. Observations were made end-on. Manganese was introduced in an helium plasma by eroding of manganese metal bands fixed on discharge electrodes. The working gas was helium flowing at 66 Pa. Self absorption was checked using the method described in Djenizˇe and Bukvic´ (2001), authors did not mention any correction. The standard Davies and Vaughan (1963) deconvolution procedure was applied using the least squares algorithm. van der Waals and resonance Key data on experiments Ref.

Plasma source

Djenizˇe et al. (2006b)

Method of measurement

Low-pressure pulsed arc

Remarks

Electron density

Temperature

˚ Stark width He II Pa k 4686 A

˚ lines Relative intensity ratio of He II k 4686/He I 5876 A

II wth and dth as in Popovic´ and Dimitrijevic´ (1997) No.

Transition array

Multiplet

Wavelength ˚) (A

Temperature (K)

Electron density (1017 cm3)

wm ˚) (A

wm/wth, wth (Popovic´ and Dimitrijevic´, 1997)

˚) dm(A

dm/dth, dth (Popovic´ and Dimitrijevic´, 1997)

Acc.

Ref.

1.

4s–4p

a7S–z7P0

2593.724 2605.684 2933.055 2939.308 2949.205 3441.988 3482.905 2610.20 2618.14 2632.35 2701.70

49,000 49,000 49,000 49,000 49,000 49,000 49,000 49,000 49,000 49,000 49,000

1.3 1.3 1.3 1.3 1.3 1.3 1.3 1.3 1.3 1.3 1.3

0.182 0.192 0.212 0.158 0.208 0.278 0.260 0.104 0.120 0.140 0.170

5.44 5.72 4.36 3.28 4.28

.008 .012 .030 .020 .O26 .012

1.0 1.5 2.68 1.80 2.32

B B B B B B B B B B B

Djenizˇe Djenizˇe Djenizˇe Djenizˇe Djenizˇe Djenizˇe Djenizˇe Djenizˇe Djenizˇe Djenizˇe Djenizˇe

a5S–z5P0

2.

3d6–4p

a5D–z5P0

3.

4s–4p

a5G– z5H0 a5G– z5G0

.008 .032

et et et et et et et et et et et

al. al. al. al. al. al. al. al. al. al. al.

(2006b) (2006b) (2006b) (2006b) (2006b) (2006b) (2006b) (2006b) (2006b) (2006b) (2006b)

broadening were neglected. Measured values are compared with the theoretical ones by Popovic´ and Dimitrijevic´ (1997). Measured to calculated values are shown in the ‘‘numerical result” table. Authors attribute the factor of 3.28– 5.7 between measured and calculated value for the Mn II investigated lines to the helium ions perturber not included in Popovic´ and Dimitrijevic´ (1997) calculations.

Manganese, Mn III Ground state: 1s22s22p63s23p63d56S5/2. Ionization energy: 33.67 eV = 271,550 cm1. Djenizˇe et al. (2006c) measured three doubly-ionized manganese spectral lines in a low pressure pulsed discharge on a shot to shot basis. Observations were made end-on. Manganese was introduced in an helium plasma by eroding of manganese metal bands fixed on discharge electrodes. The working gas was helium flowing at 665 Pa. Self absorption was checked using the method described in Djenizˇe and Bukvic´ (2001), authors did not mention any correction. The standard Key data on experiments Ref.

Plasma source

Method of measurement

Remarks

Electron density

Temperature

Djenizˇe et al. (2006c)

Low-pressure pulsed arc

˚ Stark width He II Pa k 4686 A

˚ /He I 5876 A ˚ lines Relative intensity ratio of He II k 4686 A

500

A. Lesage / New Astronomy Reviews 52 (2009) 471–535

Numerical results for Mn III No.

Transition array

Multiplet

Wavelength ˚) (A

Temperature (K)

Electron density (1017 cm3)

1.

4s–4p

b4G–y4H0

2027.83

49,000

1.3

a6D–z6F0

2069.02

49,000

1.3

b4D–z4F0

2227.42

49,000

1.3

wm ˚) (A

wm/ wth

0.08

˚) dm (A

dm/ dth

Acc.

Ref.

0.0

B

0.013

B

0.015

B

Djenizˇe et al. (2006c) Djenizˇe et al. (2006c) Djenizˇe et al. (2006c)

Davies and Vaughan (1963) deconvolution procedure was applied using the least squares algorithm. van der Waals and resonance broadening were neglected. There are no measured or calculated values available for comparison. Neon, Ne I Ground state: 1s22s22p6 1S0 Ionization energy: 21.5646 eV = 173 930.17 cm1 Milosavljevic´ et al. (2004a) used a linear low-pressure pulsed arc end-on on a shot to shot basis. The working gas was pure neon at 133 Pa filling pressure in the flowing regime. The absence of self-absorption has been controlled from relative intensity ratios during plasma decay. The ion parameters Wi, and the A and D values measured by Milosavljevic´ and Djenizˇe (2002a,b, 2003c) are shown in the numerical result table despite the restrictions raised by Ivkovic´ et al. (2006), but they are not evaluated. Electron line widths are 29% lower than Griem’s (1974) calculated values. Most of the values measured before by Nubbemeyer et al. (1970) and Puric´ (1988) lie also below Griem’s (1974) data. The semi-classical perturbation formalism (SCPF) has been used to calculate 25 of the 26 measured values. As the set of calculated values is more complete for that formalism than for Griem’s (1974) semi-classical one, the experimental values are also compared to the SCPF values. The agreement in that case is better, and even it is very good for nine of the measured lines. Jovic´evic´ et al. (2005) used a low-pressure capillary discharge (plasma inner diameter 3 mm and aluminum electrode 200 mm apart) to measure 13 Ne I lines. The working gas was a mixture of 2.4% Ne, 5.6% He and 92% H2, at the initial pressure of 4 mbar. The opacity was checked by diluting neon with helium and hydrogen until constant value of the Stark width irrespective of further decrease of neon concentration. Experimental profile is compared to a Voigt profile convolution of a Lorenzian and Gaussian ones. That later one is calculated as a sum of the squares of instrumental and Doppler widths. Contrary to Milosavljevic´ et al. (2004) they are symmetric (within experimental uncertainty). Comparisons are done with semi-classical calculations, with or without inclusion of ion broadening or proton impact width, with previous measured values, reported to the corresponding semi-classical calculated value. The best agreement is found with del Val ˚ line, with Nubbemeyer measured values. Milosavljevic´ et al. (2004) width et al. (1999) values and except for the 6266.50 A values are systematically narrower. A fact that raises a doubt about the asymmetry of their observed line shapes. The numerical value written in the accuracy column is as in Jovic´evic´ et al. (2005) article. Dzierzˇega et al. (2006) measured 4 Ne I lines in an atmospheric-pressure arc discharge (80–100 A) operated in argon– neon mixture with variable partial pressures of Ne/Ar from 2:3 to 2:1, in flowing regime. Sub-Doppler degenerate fourwave mixing technique was used to measure the line profiles, while Thomson scattering yielded the plasma electron density and temperature. As stated by the authors, the local character of these methods make them very suitable to study Stark broadening in plasmas for which the assumptions of homogeneity and symmetry are frequently questionable and where the cold boundary layers can significantly distort the observed profiles. For all observed line by Dzierzˇega et al. (2006) the shape is symmetric (within uncertainty limits), as in the Jovic´evic´ et al. (2005) case and in contradiction with Milosavljevic´ et al. (2004a) finding. Key data on experiments Ref.

Milosavljevic´ et al. (2004a) Jovic´evic´ et al. (2005) Dzierzˇega et al. (2006)

Plasma source

Method of measurement

Remarks

Electron density

Temperature

Modified linear lowpressure pulsed arc

˚ and from the Laser interferometer at 6328 A deconvolution procedure.

Boltzman plot of relative intensities of 14 Ne II lines and from the deconvolution procedure

Low-pressure capillary discharge Atmospheric pressure arc

˚) Stark width of two triplets (388.65, 4713.15 A ˚ ) of He I and one singlet (5015.68 A Thomson scattering method

Boltzmann plot of six O II impurity lines (4317.1, ˚) 4345.6, 4347.4, 4351.3, 4349.4, and 4366.9 A Thomson scattering method

A. Lesage / New Astronomy Reviews 52 (2009) 471–535

501

Numerical results for Ne I (Milosavljevic´ et al., 2004; Jovic´evic´ et al., 2005) No.

Transition array

Multiplet

Wavelength ˚) (A

Temperature (K)

Electron density (1017 cm3)

we ˚) (A

Acc.

we/ wG

we/ wscpf

wt ˚) (A

wi ˚) (A

Ref.

1.

2p5 ð2 Po3=2 Þ3s 2p5 ð2 Po3=2 Þ3p

2

7032.41

33,000

0.67

.39

B+

0.86

1.10

.44

.05

Milosavljevic´ et al. (2004a)

36,500 33,000 33,000 36,500 33,000 33,000 36,500

0.88 0.42 0.67 0.88 0.42 0.67 0.88

.50 0.309 .43 .52 0.332 .31 .40

B+

0.81

1.03

.56

.06

B+ B+ 16% B+ B+

0.87 0.77

1.14 1.00

.46 .61

.03 .09

0.88 0.84

.34 .44

.03 .04

Milosavljevic´ et al. (2004a) Jovic´evic´ et al. (2005) Milosavljevic´ et al. (2004a) Milosavljevic´ et al. (2004a) Jovic´evic´ et al. (2005) Milosavljevic´ et al. (2004a) Milosavljevic´ et al. (2004a)

33,000 36,500 33,000 33,000 36,500 33,000 33,000 36,500 33,000

0.67 0.88 0.42 0.67 0.88 0.42 0.67 0.88 0.42

.31 .38 0.312 .30 .34 0.348 .33 .41 0.337

B+ B+ 16% B+ B+ 16 B+ B+ 16%

0.72 0.65

0.92 0.83

.36 .45

.05 .07

0.91 0.75

.35 .41

.05 .07

0.95 0.86

.36 .45

.03 .04

33,000 36,500 33,000 36,500 33,000 36,500 33,000 36,500

0.67 0.88 0.67 0.88 0.67 0.88 0.67 0.88

.39 .48 .32 .44 .32 .41 .27 .34

B+ B+

B+ B+ B+ B+

1.16 1.04 0.92 0.93 0.97 0.91 0.76 0.70

.43 .53 .37 .51 .37 ..47 .30 .40

.04 .05 .05 .07 .05 .06 .03 .06

Milosavljevic´ Milosavljevic´ Milosavljevic´ Milosavljevic´ Milosavljevic´ Milosavljevic´ Milosavljevic´ Milosavljevic´

33,000

0.67

.36

B+

1.18

.40

.04

Milosavljevic´ et al. (2004a)

36,500 33,000 36,500 33,000 33,000 36,500 33,000 36,500 33,000

0.88 0.67 0.88 0.42 0.67 0.88 0.67 0.88 0.42

.44 .27 .37 0.242 .22 .30 .28 .35 0.286

B+ B+ B+ 16% B+ B+ B+ B+ 16%

0.72 0.73

1.05 0.90 0.90

.50 .32 .43

.06 .05 .06

0.70 0.64

0.69 0.68 0.88 0.81

.26 .38 .30 .39

.04 .06 .02 .04

Milosavljevic´ et al. (2004a) Milosavljevic´ et al. (2004a) Milosavljevic´ et al. (2004a) Jovic´evic´ et al. (2005) Milosavljevic´ et al. (2004a) Milosavljevic´ et al. (2004a) Milosavljevic´ et al. (2004a) Milosavljevic´ et al. (2004a) Jovic´evic´ et al. (2005)

33,000 36,500 33,000 36,500

0.67 0.88 0.67 0.88

.25 .31 .32 .41

B+ B+ B+ B+

0.83 0.75 1.01 0.94

.29 .37 .37 .48

.04 .06 .05 .07

Milosavljevic´ Milosavljevic´ Milosavljevic´ Milosavljevic´

33,000 36,500 33,000 33,000 36,500 33,000 33,000 36,500 33,000 33,000

0.67 0.88 0.42 0.67 0.88 0.42 0.67 0.88 0.42 0.67

.30 .37 0.282 .35 .45 0.369 .39 .49 0.363 .31

B+ B+ 16% B+ B+ 16% B+ B+ 16% B+

0.65 0.59

0.82 0.74

.36 .44

.06 .07

0.62 0.59

0.84 0.79

.38 .50

.03 .05

0.92 0.85

.42 .53

.03 .04

0.74

0.92

.35

.04

Milosavljevic´ et al. (2004a) Milosavljevic´ et al. (2004a) Jovic´evic´ et al. (2005) Milosavljevic´ et al. (2004a) Milosavljevic´ et al. (2004a) Jovic´evic´ et al. (2005) Milosavljevic´ et al. (2004a) Milosavljevic´ et al. (2004a) Jovic´evic´ et al. (2005) Milosavljevic´ et al. (2004a)

36,500 33,000

0.88 0.42

.41 0.296

B+ 16%

0.72

0.89

.46

.05

[3/2]o–2[1/2]

7245.17

6074.34 2

[3/2]o–2[5/2]

2.

6402.25

6334.43

6506.53

2

[3/2]o–2[3/2]

3.

6217.28 6304.79 6143.06 6382.99

4.

2p5 ð2 Po3=2 Þ3s 2p5 ð2 Po1=2 Þ3p

2

[3/2]o–2[3/2]

5975.53

5944.83

6128.45 6096.16

2

[3/2]o–2[1/2]

5.

5881.90 6030.00

2

[1/2]o–2[3/2]

6.

6532.88

6929.47

[1/2]o–2[5/2]

7.

8.

2p5 ð2 Po1=2 Þ3s 2p5 ð2 Po1=2 Þ3p

2

7173.94

2

6266.50

[1/2]o–2[3/2]

0.74 .67

Milosavljevic´ et al. (2004a) Milosavljevic´ et al. (2004a) Jovic´evic´ et al. (2005) Milosavljevic´ et al. (2004a) Milosavljevic´ et al. (2004a) Jovic´evic´ et al. (2005) Milosavljevic´ et al. (2004a) Milosavljevic´ et al. (2004a) Jovic´evic´ et al. (2005) et et et et et et et et

et et et et

al. al. al. al. al. al. al. al.

al. al. al. al.

(2004a) (2004a) (2004a) (2004a) (2004a) (2004a) (2004a) (2004a)

(2004a) (2004a) (2004a) (2004a)

Milosavljevic´ et al. (2004a) Jovic´evic´ et al. (2005) (contined on next page)

502

A. Lesage / New Astronomy Reviews 52 (2009) 471–535

Table (continued) No.

Transition array

Multiplet

Wavelength ˚) (A

Temperature (K)

Electron density (1017 cm3)

we ˚) (A

Acc.

6717.04

33,000 36,500 33,000 36,500

0.67 0.88 0.67 0.88

.36 .46 .37 .50

B+ B+ B+ B+

33,000 36,500 33,000 33,000 36,500 33,000 36,500

0.67 0.88 0.42 0.67 0.88 0.67 0.88

.28 .38 0.276 .31 .43 .35 .45

B+ B+ 16% B+ B+ B+ B+

33,000

0.67

.36

36,500 33,000

0.88 0.42

.45 0.242

6678.28 2

9.

[1/2]o–2[1/2]

6163.59

6598.95 5852.49 10.

2p5 ð2 Po3=2 Þ3p 2p5 ð2 Po3=2 Þ4d

2

[3/2]–2[5/2]o

5974.63

we/ wG

we/ wscpf

wt ˚) (A

wi ˚) (A

Ref.

0.73 0.73

0.93 0.87 0.97 0.96

.39 .50 .41 .55

.03 .04 .04 .05

Milosavljevic´ Milosavljevic´ Milosavljevic´ Milosavljevic´

0.85 0.84

.32 .44

.04 .06

0.81 0.82 0.88 0.84

.36 .50 .42 .54

.05 .07 .07 .09

Milosavljevic´ et al. (2004a) Milosavljevic´ et al. (2004a) Jovic´evic´ et al. (2005) Milosavljevic´ et al. (2004a) Milosavljevic´ et al. (2004a) Milosavljevic´ et al. (2004a) Milosavljevic´ et al. (2004a)

B+

.42

.06

Milosavljevic´ et al. (2004a)

B+ 16%

.53

.08

Milosavljevic´ et al. (2004a) Jovic´evic´ et al. (2005)

et et et et

al. al. al. al.

(2004a) (2004a) (2004a) (2004a)

Dzierzˇega et al. (2006) measured width and shift values (in cm1) are shown in a separate table of numerical results. Comparison using equations (226) and (227) from Griem (1974) including electron impact and ionic broadening is done. In the case of Stark widths the agreement is within 10 to 20%. The comparison with previous experimental results shows that the best agreement is found with del Val et al. (1999) values obtained in a similar range of temperature. While the discrepancy with Jovic´evic´ et al. (2005) values can be explained by the almost two time higher temperature difference. The factor 1.3 to 2.0 with Puric´ et al. (1987) results has already been explained by a self-absorption problem. In the case of the Stark shifts, the theoretical values are lower than Dzierzˇega et al. (2006) measured values by a factor of 1.06 to 1.6. For the experimental one, a good agreement is found with Puric´ et al. (1987) values which confirms the self absorption problem, as stated before, but lower values are reported by del Val et al. (1999) Neon Ne II Ground state: 1s2 2s2 2p52 P03=2 . Ionization energy: 40.963 eV = 330,391.0 cm1. Djenizˇe et al. (2002a), Djenizˇe and Milosavljevic´ (2000), Milosavljevic´ et al. (2001) used a modified version of a linear low-pressure pulsed arc. The working gas was pure neon at filling pressure 133 Pa in a flowing regime. Spectroscopic observations were made end-on. Line profiles were recorded using a step-by-step technique. Plasma reproducibility was 3%. van der Waals and resonance broadening were neglected. A standard (Davies and Vaughan (1963)) computerized deconvolu-

Finding List ˚) Wavelength (A

No.

˚) Wavelength (A

No.

˚) Wavelength (A

No.

˚) Wavelength (A

No.

2780.02 3001.66 3027.04 3028.86 3030.79 3034.48 3035.98 3037.73 3039.65 3319.75 3320.29

19 3 22 3 18 22 18 22 18 21 6

2333.73 3327.16 3329.16 3330.78 3334.84 3336.12 3357.82 3360.60 3362.94 3371.80 3374.06

5 2 6 9 2 26 6 2 6 11 6

3377.16 3378.22 3379.39 3411.38 3414.82 3416.91 3417.69 3503.58 3565.83 3568.50 3571.23

17 5 8 25 10 7 8 12 15 20 13

3628.04 3632.68 3659.89 3664.07 3694.21 3697.12 3727.11 3751.24 4391.94 4409.30

16 14 14 1 1 16 4 1 23 24

A. Lesage / New Astronomy Reviews 52 (2009) 471–535

503

Key data on experiments Ref.

Plasma source

Method of measurement

Hey et al. (1990), Hey and Breger (1982), Djenizˇe et al. (2006e)

Modified low-pressure pulsed discharge

Remarks

Electron density

Temperature

Single wavelength laser interferometer

Boltzmann plot of N II lines

Numerical results for Ne II (see Note added in proof) No.

Transition array

Multiplet

Wavelength ˚) (A

Temperature (K)

Electron density (1017 cm3)

1.

2p4(3P)3s– 2p4(3P)3p

4

3664.07 3694.21

35,300 31,000 34,500 35,300 31,000 34,500 35,300 31,000 34,500 35,300 31,000 34,500 35,300 31,000 34,500 35,300 31,000 34,500 35,300 31,000 34,500 35,300 31,000

1.83 0.95 1.83 1.83 0.95 1.83 1.83 0.95 1.83 1.83 0.95 1.83 1.83 0.95 1.83 1.83 0.95 1.83 1.83 0.95 1.83 1.83 0.95

34,500

1.83

35,300 31,000 34,500 35,300 31,000 34,500 35,300 31,000 34,500 35,300 31,000 34,500 35,300 31,000 34,500 35,300 31,000 34,500 31,000 34,500 35,300 31,000 34,500

1.83 0.95 1.83 1.83 0.95 1.83 1.83 0.95 1.83 1.83 0.95 1.83 1.83 0.95 1.83 1.83 0.95 1.83 0.95 1.83 1.83 0.95 1.83

P–4Po

3694.21 4

2.

P–4D0

3334.84

3360.60

3327.16

4

3.

P–4S0

3001.66

3028.86

2

4.

2

5.

P–2D0

P–2P0

3727.11

3323.73

3378.22

6.

2p4(3P)3p– 2p4(3P)3d

4

D0–4D

3362.94

3379.39

3374.06

3357.82

3320.29 3329.16

wm ˚) (A

wm/ wth

0.112 0.196

0.92 0.86

0.116 0.205

0.95 0.90

0.133 0.207

1.19 0.98

0.125 0.218

1.12 1.03

0.140 0.220

1.25 1.04

˚) dm (A 0.002

dm/ dth

Acc.

Ref. Djenizˇe et al. (2002a) Milosavljevic´ et al. (2001) Milosavljevic´ et al. (2001) Djenizˇe et al. (2002a) Milosavljevic´ et al. (2001) Milosavljevic´ et al. (2001) Djenizˇe et al. (2002a) Milosavljevic´ et al. (2001) Milosavljevic´ et al. (2001) Djenizˇe et al. (2002a) Milosavljevic´ et al. (2001) Milosavljevic´ et al. (2001) Djenizˇe et al. (2002a) Milosavljevic´ et al. (2001) Milosavljevic´ et al. (2001) Djenizˇe et al. (2002a) Milosavljevic´ et al. (2001) Milosavljevic´ et al. (2001) Djenizˇe et al. (2002a) Milosavljevic´ et al. (2001) Milosavljevic´ et al. (2001) Djenizˇe et al. (2002a) Djenizˇe and Milosavljevic´ (2000), Milosavljevic´ et al. (2001) Djenizˇe and Milosavljevic´ (2000), Milosavljevic´ et al. (2001) Djenizˇe et al. (2002a) Milosavljevic´ et al. (2001) Milosavljevic´ et al. (2001) Djenizˇe et al. (2002a) Milosavljevic´ et al. (2001) Milosavljevic´ et al. (2001) Djenizˇe et al. (2002a) Milosavljevic´ et al. (2001) Milosavljevic´ et al. (2001) Djenizˇe et al. (2002a) Milosavljevic´ et al. (2001) Milosavljevic´ et al. (2001) Djenizˇe et al. (2002a) Milosavljevic´ et al. (2001) Milosavljevic´ et al. (2001) Djenizˇe et al. (2002a) Milosavljevic´ et al. (2001) Milosavljevic´ et al. (2001) Milosavljevic´ et al. (2001) Milosavljevic´ et al. (2001) Djenizˇe et al. (2002a) Milosavljevic´ et al. (2001) Milosavljevic´ et al. (2001) (continued on next page)

0.128

0.90

– B+ B+ – B+ B+ – B+ B+ – B+ B+ – B+ B+ – B+ B+ – B+ B+ – B+

0.225

0.84

B+

0.007

0.006

0.0

.008

.008 0.082 0.146 0.0 0.080 0.150 0.0025

0.0 0.150 0.238 0.0 0.146 0.242 0.009 0.128 0.245 0.025 0.128 0.243 0.031 0.129 0.245

– B+ B+ – B+ B+ – B+ B+ B+ B+ B+ – B+ B+

0.014 0.130 0.247 0.127 0.245 0.008 0.128 0.243

B+ B+ B+ B+ – B+ B+

504

A. Lesage / New Astronomy Reviews 52 (2009) 471–535

Table (continued) No.

Transition array

7.

Multiplet

Wavelength ˚) (A

Temperature (K)

Electron density (1017 cm3)

2

3416.91

35,300 31,000 34,500 35,300 31,000

1.83 0.95 1.83 1.83 0.95

34,500

2

8.

D0–2D

D0–4F

3417.69

9.

2

D0–2F

3330.78

10

2

D0–4F

3414.82

2

11.

D0–4P

2 0 2

S–P

12.

4 0 4

S–F

13.

4 0 2

S–D

14.

3371.80

3503.58 3571.23

3632.68

3659.89

4 0 4

S–P

15.

2 0 2

P–P

16.

3565.83

3697.12 3628.04

17.

2p4(3P)3p– 2p4(3P)4s

2 0 2

P–P

4

18.

D0–4P

3377.16

3039.65

3035.98

3030.79 19. 20.

21.

4 0 4

2p4(1D)3s– 2p4(1D)3p

2

2

P–P D–2F0

D–2P0

2780.02 3568.50

3319.75

wm ˚) (A

wm/ wth

˚) dm (A 0.042

dm/ dth

Acc.

Ref. Djenizˇe et al. (2002a) Milosavljevic´ et al. (2001) Milosavljevic´ et al. (2001) Djenizˇe et al. (2002a) Djenizˇe and Milosavljevic´ (2000), Milosavljevic´ et al. (2001) Djenizˇe and Milosavljevic´ (2000), Milosavljevic´ et al. (2001) Milosavljevic´ et al. (2001) Milosavljevic´ et al. (2001) Djenizˇe et al. (2002a) Djenizˇe and Milosavljevic´ (2000), Milosavljevic´ et al. (2001) Djenizˇe and Milosavljevic´ (2000), Milosavljevic´ et al. (2001) Djenizˇe et al. (2002a) Milosavljevic´ et al. (2001) Milosavljevic´ et al. (2001) Djenizˇe et al. (2002a) Milosavljevic´ et al. (2001) Djenizˇe et al. (2002a) Milosavljevic´ et al. (2001) Milosavljevic´ et al. (2001) Djenizˇe et al. (2002a) Milosavljevic´ et al. (2001) Milosavljevic´ et al. (2001) Djenizˇe et al. (2002a) Milosavljevic´ et al. (2001) Milosavljevic´ et al. (2001) Djenizˇe et al. (2002a) Milosavljevic´ et al. (2001) Milosavljevic´ et al. (2001) Milosavljevic´ et al. (2001) Milosavljevic´ et al. (2001) Djenizˇe et al. (2002a) Milosavljevic´ et al. (2001) Milosavljevic´ et al. (2001) Djenizˇe et al. (2002a) Milosavljevic´ et al. (2001) Milosavljevic´ et al. (2001) Djenizˇe et al. (2002a) Milosavljevic´ et al. (2001) Milosavljevic´ et al. (2001) Djenizˇe et al. (2002a) Milosavljevic´ et al. (2001) Milosavljevic´ et al. (2001) Milosavljevic´ et al. (2001) Milosavljevic´ et al. (2001) Milosavljevic´ et al. (2001) Djenizˇe et al. (2002a) Milosavljevic´ et al. (2001) Milosavljevic´ et al. (2001) Djenizˇe et al. (2002a) Milosavljevic´ et al. (2001) Milosavljevic´ et al. (2001)

0.14

0.91

– B+ B+ – B+

1.83

0.251

0.86

B+

31,000 34,500 35,300 31,000

0.95 1.83 1.83 0.95

0.161 0.278 0.145

0.95

B+ B+ – B+

34,500

1.83

0.262

0.90

B+

35,300 31,000 34,500 35,300 31,000 35,300 31,000 34,500 35,300 31,000 34,500 35,300 31,000 34,500 35,300 31,000 34,500 31,000 34,500 35,300 31,000 34,500 35,300 31,000 34,500 35,300 31,000 34,500 35,300 31,000 34,500 31,000 34,500 34,500 35,300 31,000 34,500 35,300 31,000 34,500

1.83 0.95 1.83 1.83 0.95 1.83 0.95 1.83 1.83 0.95 1.83 1.83 0.95 1.83 1.83 0.95 1.83 0.95 1.83 1.83 0.95 1.83 1.83 0.95 1.83 1.83 0.95 1.83 1.83 0.95 1.83 0.95 1.83 1.83 1.83 0.95 1.83 1.83 0.95 1.83

0.156 0.296 0.024

0.031

0.007 0.143 0.265 0.0 0.165

0.98 0.029

0.174 0.318 0.069 0.175 0.317 0.04 0.176 0.318 0.022 0.177 0.318 0.176 0.320

0.97 0.92

– B+ B+ – B+ – B+ B+ – B+ B+ – B+ B+ – B+ B+ B+ B+

0.035 0.175 0.320 0.054 0.160 0.287

B+ B+ – B+ B+

0.064 B+ B+

0.159 0.289 0.020 0.164 0.293 0.162 0.293 0.207 0.006 0.132 0.232 0.01 0.120 0.221

B+ B+ B+ B+ B+ – B+ B+ – B+ B+

A. Lesage / New Astronomy Reviews 52 (2009) 471–535

505

Table (continued) No.

Transition array

Multiplet

Wavelength ˚) (A

Temperature (K)

Electron density (1017 cm3)

22.

2p4(3P)3p– 2p4(3P)3d

4 0 4

3034.48

35,300 31,000 34,500 35,300 31,000 34,500 35,300 31,000 34,500 35,300 34,500 35,300 31,000 40000 31,000 34,500 35,300

1.83 0.95 1.83 1.83 0.95 1.83 1.83 0.95 1.83 1.83 1.83 1.83 0.95 1.0 0.95 1.83 1.83

P–D

3027.04

3037.73

4

23.

2

24.

2p4(1D)3p– 2p4(1D)3d

25.

F–4F0 F–2F0

2 0 2

P–P

2 0 2

P–D

26.

4391.94 4409.30 4612.89 3411.38 3336.12

wm ˚) (A

wm/ wth

0.101 0.198

0.93 0.96

0.111 0.205

1.03 1.00

0.112 0.209

1.04 1.02

˚) dm (A

dm/ dth

Acc.

Ref.

B+ B+ – B+ B+ – B+ B+ – B+ B+ B+ B+ B+ B+ B+

Djenizˇe et al. (2002a) Milosavljevic´ et al. (2001) Milosavljevic´ et al. (2001) Djenizˇe et al. (2002a) Milosavljevic´ et al. (2001) Milosavljevic´ et al. (2001) Djenizˇe et al. (2002a) Milosavljevic´ et al. (2001) Milosavljevic´ et al. (2001) Djenizˇe et al. (2002a) Milosavljevic´ et al. (2001) Djenizˇe et al. (2002a) Milosavljevic´ et al. (2001) Milosavljevic´ et al. (2001) Milosavljevic´ et al. (2001) Milosavljevic´ et al. (2001) Djenizˇe et al. (2002a)

0.0

0.004

0.002

0.072 1.078 0.055 1.013 3.37 0.167 0.309 0.013

tion procedure was used to obtain the Stark width. The opacity was checked by measuring relative intensity ratios within the low-lying Ne II multiplet (1) lines. The measured shifts by Djenizˇe et al. (2002a) agree with their own calculated values in the case of lines that belong to the 3p–3d transition, as with the earlier measured values by Puric´ et al. (1987b) Their calculated values using the semi-classical perturbation formalism are smaller than those of Griem (1974), by up to a factor 6. They estimate their experimental shift ˚. accuracy as ±0.008 A The widths measured by Milosavljevic´ et al. (2001) agree within the experimental uncertainties, with existing experimental Stark width values in the case of the 3s–3p and 3p–3d transitions. But the values measured by del Val et al. (2000) lie, on average, 25% above all other experimental and theoretical values, especially in the case of multiplets 2, 5, 7, 9 and 10 lines. The values measured by Milosavljevic´ et al. (2001) agree with their own calculated values using the semi-classical perturbation formalism (which in general lie above Griem’s semi-classical calculations) and the modified semi-empirical values of Dimitrijevic´ and Konjevic´ (1980) and Uzelac et al. (1993). Neon, Ne III Ground state: 1s22s22p43P2. Ionization energy: 63.46 eV = 511,800 cm1. Key data on experiments Ref.

Plasma source

Method of measurement

Remarks

Electron density

Temperature

Milosavljevic´ et al. (2001)

Modified low-pressure pulsed discharge

Single wavelength laser interferometer

Boltzmann plot of N II lines

Numerical results for Ne III No.

Transition array

Multiplet

Wavelength ˚) (A

Temperature (K)

Electron density (1017 cm3)

wm ˚) (A

wm/wth wth (Milosavljevic´ et al., 2001)

1.

3s–3p

5 0 5 S–P (11 UV)

2990.04 2593.60 2595.68 2678.64 2677.90 2610.03 2613.41 2615.87 2264.91 2095.54

34,500 34,500 34,500 34,500 34,100 34,500 34,500 34,500 34,500 34,500

1.83 1.83 1.83 1.83 1.83 1.83 1.83 1.83 1.83 1.83

0.135 0.121 0.141 0.141 0.150 0.159 0.141 0.150 0.121 0.141

1.05 0.94 1.10 0.95 1.0 1.22 1.08 1.15 1.10 1.48

3 0 3

S–P

2.

3s0 –3p0

3

D0–3F

3.

3p0 –3d0

3

F–3F0 D–3D0

3

˚) dm(A

dm/ dth

Acc.

Ref.

B+ B+ B+ B+

Milosavljevic´ Milosavljevic´ Milosavljevic´ Milosavljevic´ Milosavljevic´ Milosavljevic´ Milosavljevic´ Milosavljevic´ Milosavljevic´ Milosavljevic´

B+ B+ B+ B+ B+

et et et et et et et et et et

al. al. al. al. al. al. al. al. al. al.

(2001) (2001) (2001) (2001) (2001) (2001) (2001) (2001) (2001) (2001)

506

A. Lesage / New Astronomy Reviews 52 (2009) 471–535

Milosavljevic´ et al. (2001) used a modified low-pressure pulsed discharge, end-on, for Ne II line width measurements. Line profiles were recorded with a step-by-step technique. Reproducibility was 3%. Working gas was pure neon at 133 Pa in a flowing regime. Absence of self absorption was checked by measuring relative line intensity ratios within the low-lying Ne II multiplet (1) lines. Comparison with calculated ratio of corresponding g (statistical weight) and A (spontaneous emission probability) values shows an agreement within ±14%. Measured values are in agreement with semiclassical perturbation (SCPF) calculated values (Milosavljevic´ et al., 2001). Neon, Ne IV Ground state: 1s2 2s2 2p34 S03=2 . Ionization energy: 97.12 eV = 783,300 cm1. Milosavljevic´ et al. (2001) used a modified low-pressure pulsed discharge, end-on, for Ne II line width measurements. Profiles were recorded with a step-by-step technique. Reproducibility was 3%. Working gas was pure neon at 133 Pa in a flowing regime. Absence of self absorption was checked by measuring relative line intensity ratios within the low-lying Ne II multiplet (1) lines. Comparison with calculated ratio of corresponding g (statistical weight) and A (spontaneous emission probability) values shows an agreement within ±14%. Measured values are in agreement with semiclassical perturbation (SCPF) calculated values (Milosavljevic´ et al., 2001). Key data on experiments Ref.

Plasma source

Milosavljevic´ et al. (2001)

Method of measurement

Modified low-pressure pulsed discharge

Remarks

Electron density

Temperature

Single wavelength laser interferometer

Boltzmann plot of N II lines

Numerical results for Ne IV No.

Transition array

Multiplet

Wavelength ˚) (A

Temperature (K)

Electron density (1017 cm3)

wm ˚) (A

wm/ wth

1.

3s–3p

4

P–4D0

2

P–2D0

2372.16 2352.52 2357.96 2365.49 2363.28

34,500 34,500 34,500 34,500 34,500

1.83 1.83 1.83 1.83 1.83

0.115 0.121 0.121 0.150 0.159

1.06 1.12 1.12 1.21 1.29

dm ˚) (A

dm/ dth

Acc.

Ref.

B+ B+ B+ B+ B+

Milosavljevic´ Milosavljevic´ Milosavljevic´ Milosavljevic´ Milosavljevic´

et et et et et

al. al. al. al. al.

(2001) (2001) (2001) (2001) (2001)

Neon, Ne VIII Ground state: 1s22s2S1/2. Ionization energy: 239.099 eV = 1,928,462 cm1. ˚ line Hegazy et al. (2003) used the gas-liner pinch facility (Bu¨scher et al., 2000) to observe the Ne VIII 3s–3p k 2820.7 A emitted by a neon plasma column surrounded by a helium plasma. The geometry and the timing of the discharge are devised in order to avoid the boundary layer problem. Varying the test gas concentration checked effects of optical thickKey data on experiments Ref.

Plasma source

Hegazy et al. (2003)

Gas-liner pinch

Method of measurement

Remarks

Electron density

Temperature

90° Thomson scattering

90° Thomson scattering

Numerical results for Ne VIII No.

Transition array

Multiplet

Wavelength ˚) (A

Temperature (K)

Electron density (1017 cm3)

wm ˚) (A

1.

3s–3p

2

2820.7

46,4000

10

0.29

S–2P0

wm/ wth

dm ˚) (A

dm/ dth

Acc.

Ref.

B

Hegazy et al. (2003)

A. Lesage / New Astronomy Reviews 52 (2009) 471–535

507

ness. A least square procedure was used to fit the components of the calculated profile to the observed line shape. The obtained value is 25% lower than the previous value measured by Glenzer et al. (1992) with the same device, but nevertheless within mutual error bar. The authors explain that the previous Ne VIII width measurements were obtained at neon concentrations high enough to induce plasma inhomogeneities along the axis. The new value fits well with the Z-scaling of line width along the isoelectronic sequence. But it is 2.3 times larger than the most recent quantum-mechanical calculated Ralchenko et al. (2003) values. Oxygen, O II Ground state: 1s2 2s2 2p34 S03=2 . Ionization energy: 35.1211 eV = 283,270.9 cm1. Key data on experiments Ref.

Plasma source

Method of measurement

Remarks

Electron density

Temperature

Srec´kovic´ et al. (2001a)

Modified low-pressure pulsed arc

˚ Laser interferometer at 6328 A

Boltzmann plot of 12 O II lines

Numerical results for O II No.

Transition array

Multiplet

Wavelength ˚) (A

Temperature (K)

Electron density (1017 cm3)

wm ˚) (A

wm/ wth

1.

2p2(3P)3s– 2p2(3P)3p

2

3954.36

12,000 13,800 15,700 18,300 20,300 12,000 13,800 15,700 18,300 20,300 12,000 13,800 15,700 18,300 20,500 12,000 13,800 15,700 18,300 20,500 12,000 13,800 15,700 18,300 20,500 12,000 13,800 15,700 18,300 20,500 12,000 13,800 15,700 18,300 20,500 15,700 18,300 20,500 15,700 18,300 20,500

0.76 0.91 1.45 1.82 1.25 0.76 0.91 1.45 1.82 1.25 0.76 0.91 1.45 1.82 0.98 0.76 0.91 1.45 1.82 0.98 0.76 0.91 1.45 1.82 0.98 0.76 0.91 1.45 1.82 0.98 0.76 0.91 1.45 1.82 0.98 1.45 1.82 0.98 1.45 1.82 0.98

0.288 0.312 0.495 0.477 0.278 0.252 0.358 0.349 0.546 0.464 0.370 0.359 0.443 0.575 0.336 0.373 0.425 0.554 0.568 0.310 0.305 0.310 0.555 0.528 0.290 0.284 0.293 0.370 0.520 0.295 0.312 0.360 0.374 0.462 0.328 0.448 0.356 0.232 0.419 0.358 0.222

1.38 1.30 1.34 1.08 0.94 1.2 1.5 0.95 1.24 1.57 1.53 1.30 1.03 1.10 1.22 1.54 1.54 1.29 1.09 1.13 1.26 1.12 1.29 1.01 1.06 1.18 1.06 0.86 1.00 1.08 1.26 1.27 0.86 0.86 1.15

P–2P0

3945.05

2

2p2(3P)3p– 2p2(3P)3d

4

D0–4F

4075.86

4072.15

4092.93

4085.11

3.

4.

2p2(3P)3p– 2p2(3P)3d

2p2(1D)3p – 2p2(1D)3d

4 0 4

P–P

2 0 2

F–G

4132.90

4185.46

4189.79

˚) dm (A

dm/dth

0.037 ± 0.01

0.20

0.046 ± 0.01

0.26

0.096 ± 0.025

0.54

0.088 ± 0.025

0.49

0.134 ± 0.025

0.75

0.047 ± 0.025

0.19

0.077

0.087

Acc.

Ref.

B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+

Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´

et et et et et et et et et et et et et et et et et et et et et et et et et et et et et et et et et et et et et et et et et

al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al.

(2001a) (2001a) (2001a) (2001a) (2001a) (2001a) (2001a) (2001a) (2001a) (2001a) (2001a) (2001a) (2001a) (2001a) (2001a) (2001a) (2001a) (2001a) (2001a) (2001a) (2001a) (2001a) (2001a) (2001a) (2001a) (2001a) (2001a) (2001a) (2001a) (2001a) (2001a) (2001a) (2001a) (2001a) (2001a) (2001a) (2001a) (2001a) (2001a) (2001a) (2001a)

508

A. Lesage / New Astronomy Reviews 52 (2009) 471–535

Srec´kovic´ et al. (2001a) measured the Stark widths and shifts of nine O II lines with a low-pressure pulsed arc as in Djenizˇe et al. (1998, 1991a) at different temperatures. The working gas was CO2 at 133 Pa (1 mm Hg). The plasma was reproducible within 3%, as monitored by O II, O III and C II lines. The opacity was checked by measuring relative line intensity ratios within multiplet (10) lines and compared to theoretical ones. Experimental ratios remained constant during plasma decay and were in agreement within the error bars and with the theoretical results. Consequently self-absorption was considered to be negligible. The deconvolution procedure used a computerized version of the Davies and Vaughan (1963) tables. The measured O II line widths are in agreement with Griem (1974) theoretical predictions at electron temperature of 20,000 K. But at a lower temperature (T = 12,000 K) the experimental values lie above Griem (1974) values. Oxygen, O III Ground state: 1s22s22p23P0. Ionization energy: 54.936 eV = 443,086 cm1. Sreckovic´ et al. (2001b) measured Stark widths and shifts of seven O III lines in a modified version of a low-pressure pulsed arc, end-on, with a shot-to-shot scanning technique. The working gas was either a mixture of 83% N2, 17% O2, or pure CO2 at 70 and 133 Pa respectively, with a constant flux at flowing regime. The plasma reproducibility was ± 3%. The opacity was checked by measuring the relative line intensity ratios within multiplet (2) during the plasma decay. The standard deconvolution procedure (Davies and Vaughan, 1963) was applied using the least-squares algorithm. ˚ line widths, the agreement is very good with Blagojevic´ et al. (2000) measured values and For the k 3754.7 and 3757.2 A ˚ lines the agreement is very good within error bar with those of Platisˇa et al. (1975). For the k 2983.8, 4073.9 and 4081.1 A with Puric´ et al. (1988b,c) measured values. As for the three above mentioned mult. (2), (6) and (23) lines the agreement is also very good with the semiclassical perturbation formalism calculated values of Dimitrijevic´ and Sahal-Bre´chot (1996b,c), they are among those that could be recommended for diagnostic purpose. Comparisons are graphically shown with: semiempirical Griem (1968b), modified semi-empirical Dimitrijevic´ and Konjevic´ (1981) and simplified semi-classical Griem (1974) calculated values. The agreement is most of the time within error bar, except in the semi-empirical case where calculated values for the multiplets.(2), (3), (6) lines are up to a factor of two narrower. Djenizˇe et al. (2003) measured 33 O III line shifts in the same source as in Sreckovic´ et al. (2001b) in pure oxygen. The value mentioned in the accuracy column is the error bar as estimated by the authors. Eleven of the values are in agreement with those of Puric´ et al. (1988c) and Sreckovic´ et al. (2001b). For the 22 others lines no comparison is possible as they have never been measured before. Calculations presented in Sreckovic´ et al. (2001b) provide values several times smaller than the ˚ line shift measured values for experimental ones. Despite of that, authors recommend their O III k 3312.32 and 3340.76 A plasma diagnostics in astrophysical applications. Djenizˇe et al. (2004c) measured five O III lines belonging to the 3p–3d and forbidden 3s–4d transitions. The test gas was pure oxygen and helium-oxygen mixture (He/O = 0.9) at 133 Pa filling pressure in the flowing regime. According to the technique described in Djenizˇe and Bukvic´ (2001) and applied in present case, self-absorption was found to be negligible. The standard deconvolution procedure was applied using the least-square algorithm. van der Waals and resonance broadening were neglected. There are no previously measured or calculated values for comparison. Bukvic´ et al. (2004b) measured three O III lines belonging to the 3p–3d transition array in a low pressure pulsed arc. The working gas was a helium oxygen mixture (1/1.1) at 266 Pa filling pressure in the flowing regime. The opacity was checked by a technique described in Djenizˇe and Bukvic´ (2001). Deconvolution is as in Djenizˇe et al. (2004c). For the comparison with previously measured values obtained at the same or at higher temperature a formula ([T(K)]1/2) is proposed to relate the width and the temperature. According to that formula the measured values by Platisˇa et al. (1975) at the same temperature and by Puric´ et al. (1988b) and Blagojevic´ et al. (2000) at higher temperature agree within the error bar, except for one value obtained by Blagojevic´ et al. (2000) at 46,000 K. A similar formula, as the one mentioned for the width, is proposed for the variation of the shift versus temperature. That formula fits quite well with Bukvic´ et al. (2004b), Djenizˇe et al. (2003) and Puric´ et al. (1988c) measured values. Srec´kovic´ et al. (2005) measured 23 O III lines belonging to ten multiplets in the 3s–3p and 3p–3d transition arrays. The spectroscopic source and the experimental procedures are as in the Bukvic´ et al. (2004b) work, except that the working gas was pure oxygen at 130 Pa filling pressure. The 3p3D–4d 3F0 transition normalized averaged width values agree within 6% with those of the averaged three lines belonging to the same transition measured by Blagojevic´ et al. (2000) at 39,700 K. For the 3s5P–3p5D0 and 3p3P–3d 3D0 multiplets, the agreement is within 3.5% with the values of Puric´ et al. (1988c) obtained at 42,500 K. But in the case of the 3p3D–3d3F0, 3p3D–3d 3D0 and 3p3S0–3d3P multiplets, the values of Srec´kovic´ et al. (2005) are 13% higher than those of Puric´ et al. (1988c) and for the 3s3P0–3p3P multiplet, they are 22% higher. The measured values of Srec´kovic´ et al. (2005) agree with the calculated values of Dimitrijevic´ and Konjevic´ (1981) who used the simplified semi-classical method (SSC) (Griem et al., 1962). But they lie above all other calculated values (Griem,

A. Lesage / New Astronomy Reviews 52 (2009) 471–535

509

1968b, 1974; Dimitrijevic´ and Konjevic´, 1981). As they represent the electron contribution to the Stark broadening only, the inclusion of the ion one may lead to their increase and improve the agreement. Ivkovic´ et al. (2005) measured Stark widths of O III lines in a capillary discharge plasma, inner diameter 3 mm and aluminum electrode (with 3 mm diameter holes) 200 mm apart. Observations are done end-on, and line profiles recorded on a step by step procedure. Averaging of eight signals at each wavelength step is performed. The filling gas, at initial pressure of 4 mbar, is a mixture of 1.5% N2 + 1.5% CO2 in 97% He. To check the optical thinness of the plasma, authors compare the line intensity ratios within the studied multiplets with their theoretical predictions. The measured ratio (4.1) at the time of observation is closed to the calculated one (4.14). Within the studied multiplets the strongest line of the O III 3s–3p tran˚ , is the only one found slightly self-absorbed. A computerized procedure is used to fit the experimental sition, k 3759.9 A profiles to Voigt profiles (Davies and Vaughan, 1963). In addition the Stark widths of investigated O III lines were measured again in the low-pressure pulsed arc used by Blagojevic´ et al. (2000) earlier for O III line width measurements. The new measured widths do not differ by more than a few percent within the studied multiplets when compared to the widths measured with the capillary discharge. Then measurements done with the capillary discharge are the only one reported. Measured values are in good agreement with semi-classical (SC) Sahal-Bre´chot (1969a,b, 1974), Dimitrijevic´ and Sahal-Bre´chot (1995a, 1984), modified semi-empirical (MSE) Dimitrijevic´ and Konjevic´ (1980) and simplified semi-classical (SSC) Griem (1974) calculated ones. For the O III 3s3P0–3p3D multiplet Ivkovic´ et al. (2005) values are in agreement within error bar with Blagojevic´ et al. (2000), Platisˇa et al. (1975) previous measured values. For the OIII 3p3D–3d3F0 multiplet, Ivkovic´ et al. (2005) values compare well with Blagojevic´ et al. (2000), Platisˇa et al. (1975), Puric´ et al. (1988b) measured ones. Key data on experiments Ref.

Plasma source

Method of measurement Electron density

Temperature

Sreckovic´ et al. (2001b) Djenizˇe et al. (2003, 2004c) Bukvic´ et al. (2004b)

Modified low-pressure pulsed arc

Laser interferometer at ˚ 6328 A

Modified low-pressure pulsed arc

Laser interferometer at ˚ 6328 A

(a)Boltzmann plot of 12 O II lines and intensity ratio of N IV, N III, N II lines (b) ratio of relative intensities of NIV/NIII and NIII/ NI lines Saha equation, relative intensity of OIII/OII lines Saha equation, relative intensity of OIII/OII lines

Low-pressure pulsed arc

Laser interferometer at ˚ 6328 A Laser interferometer at ˚ 6328 A

Srec´kovic´ et al. (2005) Ivkovic´ et al. (2005)

Low-pressure pulsed arc

Low pressure capillary discharge (and check with a low-pressure pulsed arc)

Remarks

Saha equation, relative intensity of OIII/OII lines and Boltzmann plot using six OIV relative intensity ˚ lines Botzmann plot of four N II k 3995, 4447, 4630, 4803 A

Stark of He II Paschen beta line k ˚ 3202 A

Numerical results for O III No.

Transition array

Multiplet

˚) Wavelength (A

Temperature (K)

Electron density (1017 cm3)

wm ˚) (A

1.

2p(2P0)3s– 2p(2P0)3p

3 0 3

3759.80 Slightly self-abs. 3754.70

30,300

0.86

0.138

42,000 54,000 30,300 42,000 54,000 30,300 42,000 30,300 42,000 30,300 42,000 42,000 42,000 54,000

1.0 2.80 0.86 1.0 2.80 0.86 1.0 0.86 1.0 0.86 1.0 1.0 1.0 2.80

P–D

3757.23

3774.02

2.

3 0 3

P–S

3753.83 3791.27 3299.38 3312.32 3340.76

wm/ wth

˚) dm (A

dm/ dth

0.85

.026 ± .0048 0.0 ± .008

5

0.38 0.139

0.90

.015 ± .0048 0.0 ± .008

2.9

0.40 0.141

.025 ± .0048

4.8

Ref.

B+

Ivkovic´ et al. (2005)

B+ B+ B+ B+ B+

0.140 .016 ± .0048

3.0 B+

0.138

0.26

Acc.a

0.74

.008 ± .0048 .007 ± .0048 .006 ± .0048 0.00 ± .008

2.1 1.9 1.6 B+

Djenizˇe et al. (2003) Sreckovic´ et al. (2001b) Ivkovic´ et al. (2005) Djenizˇe et al. (2003) Sreckovic´ et al. (2001b) Ivkovic´ et al. (2005) Djenizˇe et al. (2003) Ivkovic´ et al. (2005) Djenizˇe et al. (2003) Ivkovic´ et al. (2005) Djenizˇe et al. (2003) Djenizˇe et al. (2003) Djenizˇe et al. (2003) Sreckovic´ et al. (2001b) (continued on next page)

510

A. Lesage / New Astronomy Reviews 52 (2009) 471–535

Table (continued) No.

Transition array

Multiplet

Wavelength ˚) (A

Temperature (K)

Electron density (1017 cm3)

3 0 3

3035.41

42,000 42,000 42,000 42,000 42,000 42,000 42,000 17,000 17,800 18,300 19,000 54,000 42,000 4200 42,000 42,000 26,000 33,300 26,000 26,000 42,000 30,300 42,000 42,000 42,000 30,300 42,000 42,000 42,000 42,000 42,000 42,000 42,000 42,000 42,000 42,000 42,000 42,000 42,000 42,000 42,000 42,000 42,000 42,000 42,000 42,000 42,000 42,000 42,000 42,000 42,000 42,000 42,000 42,000 42,000 42,000 42,000 42,000

1.0 1.65 1.0 1.0 1.65 1.0 1.0 1.87 1.96 1.82 1.66 2.80 1.65 1.0 1.0 1.0 1.10 0.86 1.10 1.10 1.0 0.86 1.0 1.65 1.0 0.86 1.0 1.65 1.65 1.65 1.0 1.0 1.65 1.0 1.65 1.0 1.65 1.0 1.65 1.0 1.65 1.00 1.65 1.65 1.0 1.65 1.65 1.65 1.0 1.65 1.0 1.65 1.65 1.65 1.0 1.65 1.0 1.65

P–P

3.

3059.27 3023.42

1 0 1

P–D

4.

1

5. 6.

2p(2P0)3p– 2p(2P0)3d

3047.10 2983.78

P–1D0

2959.69

1D  1F0

3961.59 3265.46

3

D–3F0

3260.98 3267.31

3281.83 3260.85 3284.45 3

7.

3

8.

D–3D0

S–3P0

2996.48 2997.69 3004.34 3017.61 3115.67 3121.63 3132.79

9.

2p(2P0)3p– 2p(2P0)3d

10.

11.

2s2p2(4P)3s2s2p2(4P)3p

3

P–3D0

3

P–3P0

5

P–5D0

3707.27 3725.31 3715.08 3428.626 3444.052 3430.568 3695.37 3703.35 3704.74

12.

5

P–5S0

3720.89 3721.92 2665.68 2674.58 2686.15

wm ˚) (A

wm/ wth

0.23

1.24

˚) dm (A

dm/ dth

Acc.a

.021 ± .0048 12% .009 ± .0048 .014 ± .0048 0.23

1.24

12% .038 ± .0048 .012 ± .0048

0.396 0.394 0.389 0.380 0.340 .26

1.12 1.10 1.19 1.33 1.10

0.009 ± .008 0.0 ± .008 .003 ± .0048 .005 ± .0048 .020 ± .0048 .032 ± 0.005

0.151 0.102 0.152 0.145

.029 ± 0.005 .034 ± 0.005 .029 ± .0048

6.7 B+ B+ B+ B+ B+ 12%

B+ B+ B+ B+ B+

0.103 .011 ± .0048 .18

15% .020 ± .0048 B+

0.099 .007 ± .0048 .24 .24 .20

17% 15% 15% .027 ± .0048 .029 ± .0048

.24

10% .022 ± .0048

.28

10% .026 ± .0048

.26

10% .012 ± .0048

.35

1.08

10% .005 ± .0048

.38

1.18

10% .030 ± .0048 .019 ± .008 .015 ± .008 .009 ± .0048 .012 ± .008

0.32 0.31 0.35 .28 .30

1.08 1.15

.28

1.08

B+ B+ B+ 10% 10%

.030 ± .0048 10% .014 ± .0048 .26 .28 .12

1.00 1.08 0.80

.12

0.80

10% 10% 15% .011 ± .0048 15% .007 ± .0048

.12

0.80

15%

Ref.

Djenizˇe et al. (2003) Srec´kovic´ et al. (2005) Djenizˇe et al. (2003) Djenizˇe et al. (2003) Srec´kovic´ et al. (2005) Djenizˇe et al. (2003) Djenizˇe et al. (2003) Sreckovic´ et al. (2001b) Sreckovic´ et al. (2001b) Sreckovic´ et al. (2001b) Sreckovic´ et al. (2001b) Sreckovic´ et al. (2001b) Srec´kovic´ et al. (2005) Djenizˇe et al. (2003) Djenizˇe et al. (2003) Djenizˇe et al. (2003) Bukvic´ et al. (2004b) Ivkovic´ et al. (2005) Bukvic´ et al. (2004b) Bukvic´ et al. (2004b) Djenizˇe et al. (2003) Ivkovic´ et al. (2005) Djenizˇe et al. (2003) Srec´kovic´ et al. (2005) Djenizˇe et al. (2003) Ivkovic´ et al. (2005) Djenizˇe et al. (2003) Srec´kovic´ et al. (2005) Srec´kovic´ et al. (2005) Srec´kovic´ et al. (2005) Djenizˇe et al. (2003) Djenizˇe et al. (2003) Srec´kovic´ et al. (2005) Djenizˇe et al. (2003) Srec´kovic´ et al. (2005) Djenizˇe et al. (2003) Srec´kovic´ et al. (2005) Djenizˇe et al. (2003) Srec´kovic´ et al. (2005) Djenizˇe et al. (2003) Srec´kovic´ et al. (2005) Djenizˇe et al. (2003) Djenizˇe et al. (2004c) Djenizˇe et al. (2004c) Djenizˇe et al. (2003) Djenizˇe et al. (2004c) Srec´kovic´ et al. (2005) Srec´kovic´ et al. (2005) Djenizˇe et al. (2003) Srec´kovic´ et al. (2005) Djenizˇe et al. (2003) Srec´kovic´ et al. (2005) Srec´kovic´ et al. (2005) Srec´kovic´ et al. (2005) Djenizˇe et al. (1991a) Srec´kovic´ et al. (2005) Djenizˇe et al. (2003) Srec´kovic´ et al. (2005)

A. Lesage / New Astronomy Reviews 52 (2009) 471–535

511

Table (continued) No.

Transition array

Multiplet

Wavelength ˚) (A

Temperature (K)

Electron density (1017 cm3)

wm ˚) (A

wm/ wth

13.

2s2p2(4P)3s2s2p2(4P)3p

3

4073.984

18,300 19,000 17,000 17,800 18,300 19,000 42,000 42,000 42,000 42,000 42,000 42,000 42,000 54,000

1.82 1.66 1.78 1.96 1.82 1.66 1.65 1.65 1.65 1.0 1.65 1.0 1.65 2.80

0.522 0.512 0.532 0.571 0.589 0.597 0.82 0.92 .20

0.84 0.84 0.84 0.84 0.95 1.10

.30

1.15

P–3D0

4081.020

14. 15. 16.

17. a

2s2p2(4P)3s2s22p(2P0)4d 2s2p2(4P)3p2s2p2(4P)3d 2s2p2(4P)3p2s2p2(4P)3d

3

P–3D0

2s2p2(4P)3p2s2p2(4P)3d

5 0 5

3 0 3

S–P

5

D0–5F

S–P

3427.364 3440.363 2687.54 2695.47 3447.96 3454.97 4447.694

˚) dm (A

dm/ dth

.013 ± .008 .11 ± .008 .048 ± .008

Acc.a

Ref.

B+ B+ B+ B+ B+ B+ B+ B+ 15%

Sreckovic´ et al. (2001b) Sreckovic´ et al. (2001b) Sreckovic´ et al. (2001b) Sreckovic´ et al. (2001b) Sreckovic´ et al. (2001b) Sreckovic´ et al. (2001b) Djenizˇe et al. (2004c) Djenizˇe et al. (2004c) Srec´kovic´ et al. (2005) Djenizˇe et al. (2003) Srec´kovic´ et al. (2005) Djenizˇe et al. (2003) Srec´kovic´ et al. (2005) Sreckovic´ et al. (2001b)

.009 ± .0048 12% .015 ± .0048 .34 0.940

1.31 1.32

0.0 ± .008

12% B+

For Srec´kovic´ et al. (2005), accuracy is as in Srec´kovic´ et al. (2005).

Ivkovic´ et al. (2005) O III widths measurements were performed simultaneously with the N II ones also reported in the present review. The purpose of which was to check if the anomalous ratio N II to O III widths previously measured by Blagojevic´ et al. (2000) and not verified by the theories Elton et al. (2004a). The conclusion of their measurements is that the possible cause of the erroneous results in Blagojevic´ et al. (2000) is plasma inhomogeneity in a larger diameter discharge tube. The ratio is further exaggerated by the selection of a high normalization electron temperature taken for data comparison along the isoelectronic sequence. Oxygen, O IV Ground state: 1s2 2s2 2p2 P01=2 . Ionization energy: 77.416 eV = 624,382.0 cm1. Key data on experiments Ref.

Plasma source

Method of measurement

Remarks

Electron density

Temperature

Djenizˇe et al. (2003)

Modified low-pressure pulsed arc

˚ Laser interferometer at k 6328 A

Saha equation, relative intensity OIII/OII lines

Numerical results for O IV No.

Transition array

Multiplet

Wavelength ˚) (A

Temperature (K)

Electron density (1017 cm3)

1.

3s–(1S)3p

2

2.

3p–(1S)3d

2 0 2

3.

2s2p3s– 2s2p(3P0) 3p

4 0 4

3071.60 3063.43 3403.55 3411.69 3385.52

42,000 42,000 42,000 42,000 42,000

1.0 1.0 1.0 1.0 1.0

S–2P0 P–D P–D

wm ˚) (A

wm/ wth

˚) dm (A

dm/ dth

Acc.

Ref.

.0139 ± 0.0048 .0146 ± 0.0048 .0117 ± 0.0048 .0127 ± 0.0048 0.00 ± 0.0048

1.21 1.27 1.23 1.33

B B B B B

Djenizˇe Djenizˇe Djenizˇe Djenizˇe Djenizˇe

et et et et et

al. al. al. al. al.

(2003) (2003) (2003) (2003) (2003)

Djenizˇe et al. (2003) measured shifts of five O IV lines in a modified version of a low-pressure pulsed arc (Djenizˇe and Labat, 1983), end-on, with a shot-to-shot scanning technique. Their shift measured values are on average 26% higher than Blagojevic´ et al. (1996) calculated values. The theoretical value retained for the dm/dth ratio in column 10 is as calculated by Blagojevic´ et al. (1996). Silicon, Si II Ground state: 1s2 2s2 2p6 3s2 3p2 P01=2 . Ionization energy: 16.346 eV = 131,838.4 cm1. Gonzalez (1999), Gonzalez et al. (2001, 2002) have measured Si II lines in the linear discharge lamp, observed end-on, on a shot to shot basis. The lamp described by del Val et al. (1998) has been customized by Gonzalez (1999) for this work, to

512

A. Lesage / New Astronomy Reviews 52 (2009) 471–535

account for the particular feature of the plasma gas. The plasma is generated by discharging a capacitor bank of 20 lF, charged up to 8.5 kV, on the electrodes of the lamp filled with a continuous laminar flow of He + SiH4 mixture at 1.63  103 Pa, at helium rate 11.5 ml min1 and silane rate of 0.075 ml min1. An extensive description of the system is given in Gonzalez (1999) dissertation. An algorithms described by Gonzalez (1999) gives a measurement of the optical depth and provides the self-absorption of each spectral line. The standard deconvolution procedure Davies and Vaughan (1963) was applied. Gonzalez et al. (2001) values for Si II Mult. (1) lines are in close agreement with those of Wollschla¨ger et al. (1997) For the low-excitation multiplets a similar close agreement is found with those obtained by Lesage et al. (1983) and Konjevic´ et al. (1970). Lesage and Redon (2004) used a shock tube as spectroscopic source, filled with neon and a small admixture of a volatile silicon compound, to observe faint Si II lines. A large aperture (F/1.7) luminous spectrograph was used with an intensified RETICON detector. Physical conditions and comparison with the strong Si II (Mult. 3) line intensity ratio lead the authors to neglect self-absorption. But no direct check was done. A new unfolding procedure described in Lesage and Redon (2004) is used. The method takes in account the fact that the line profiles cover a limited number of the detector pixels. The obtained experimental value is much lower than calculated by Dimitrijevic´ in Lanz et al. (1988). Wilke (2003) has measured Si II lines emitted by a laser-created plasma. His measurements are unpublished. For the Si II Mult. 7.26 lines, his values ˚ and cannot be compared with the present one due to the unknown variation of the obtained at T = 21,000 K is 0.52 A Stark parameter versus temperature (Ralchenko et al., 2003).

Key data on experiments Ref.

Gonzalez (1999), Gonzalez et al. (2001, 2002) Lesage and Redon (2004)

Plasma source

Method of measurement Electron density

Temperature

Remarks

Linear discharge lamp Shock tube

Two-wavelength Twyman–Green interferometer, at k 6328 and ˚ , and calibrated He I k 5016, 7281 A ˚ and Ha line widths. 4880 A

Boltzmann plot of He I and Si II lines and absolute emission of intensity He I lines. Absolute intensity of Ne I line at ˚ 5852 A

˚ and 6328 A ˚ Michelson interferometer at 4880 A

Numerical results for Si II No.

Transition array

Multiplet

˚) Wavelength (A

Temperature (K)

Electron density (1017 cm3)

wm ˚) (A

1.

3p–4p

2

3856.02

16,000– 20,000 16,000– 20,000 16,000– 20,000 16,000– 20,000 16,000– 20,000 16,000– 20,000 16,000– 20,000 16,000– 20,000 16,000– 20,000 16,000– 20,000 16,000– 20,000 16,000– 20,000 16,000– 20,000 16,000– 20,000

1.0

0.50

1.0

D–2P0

3862.60 3853.66 2.

3d–4f

2

D–2F0

4130.89 4128.07

3.

4s–4p

2

S–2P0

6371.36 6347.10

4.

4p–4d

2 0 2

P–D

5055.98 5041.03

5.

4p–5s

2 0 2

P–S

5957.56 5978.93

6.

4d–5f

2

D–2F0

7848.82–7849.72

7.

4d–6f

2

5466.46–5466.87

8.

3p0 -3d0

4

5202.41

D–2F0 D–4F0

wm/ wth

dm ˚) (A

dm/ dth

Acc.

Ref.

0.05

21%

0.50

0.03

25%

1.0

0.52

0.17

32%

1.0

1.01

0.20

11%

1.0

0.97

0.23

15%

1.0

0.99

0.29

25%

1.0

1.13

0.31

23%

1.0

2.58

0.93

13%

1.0

2.54

0.86

7%

1.0

2.72

1.32

20%

1.0

2.78

1.19

15%

1.0

4.39

0.32

49%

1.0

9.48

1.0

1.33

Gonzalez (1999), Gonzalez et al. (2001, 2002) Gonzalez (1999), Gonzalez et al. (2001, 2002) Gonzalez (1999), Gonzalez et al. (2001, 2002) Gonzalez (1999), Gonzalez et al. (2001, 2002) Gonzalez (1999), Gonzalez et al. (2001, 2002) Gonzalez (1999), Gonzalez et al. (2001, 2002) Gonzalez (1999), Gonzalez et al. (2001, 2002) Gonzalez (1999), Gonzalez et al. (2001, 2002) Gonzalez (1999), Gonzalez et al. (2001, 2002) Gonzalez (1999), Gonzalez et al. (2001, 2002) Gonzalez (1999), Gonzalez et al. (2001, 2002) Gonzalez (1999), Gonzalez et al. (2001, 2002) Gonzalez (1999), Gonzalez et al. (2001, 2002) Gonzalez (1999), Gonzalez et al. (2001, 2002)

58% 0.16

30%

A. Lesage / New Astronomy Reviews 52 (2009) 471–535

513

Table (continued) No.

Transition array

Multiplet

Wavelength ˚) (A

Temperature (K)

Electron density (1017 cm3)

wm ˚) (A

9.

3d0 -4p0

4 0 4

5669.56

16,000– 20,000 16,000– 20,000 16,000– 20,000 16,000– 20,000 11000 11000 11000 16,000– 20,000 16,000– 20,000 16,000– 20,000 16,000– 20,000 16,000– 20,000 16,000– 20,000 16,000– 20,000

1.0

0.67

1.0

F–D

5688.81 5701.37 5706.37 10.

3d0 -4p0

2

D0–2P

11.

4s0 -4p0

4 0 4

P–P

4190.724 4198.133 4183.345 5800.47 5806.74

2

4p0 -4d0

12.

P–2D0

5785.73 5794.9

4

4p0 -4d’

13.

S–4P0

5496.45 5447.26

2

4d-7p

D–2P0

5478.73

wm/ wth

dm/ dth

Acc.

Ref.

0.24

33%

0.77

0.30

22%

1.0

0.68

0.32

20%

1.0

0.83

0.19

21%

1.0 1.0 1.0 1.0

0.095 0.095 0.095 0.88

1.0

0.51

75%

1.0

1.45

32%

1.0

1.84

45%

1.0

1.92

30%

1.0

1.84

19%

1.0

2.00

22%

Gonzalez (1999), Gonzalez et al. (2001, 2002) Gonzalez (1999), Gonzalez et al. (2001, 2002) Gonzalez (1999), Gonzalez et al. (2001, 2002) Gonzalez (1999), Gonzalez et al. (2001, 2002) Lesage and Redon (2004) Lesage and Redon (2004) Lesage and Redon (2004) Gonzalez (1999), Gonzalez et al. (2001, 2002) Gonzalez (1999), Gonzalez et al. (2001, 2002) Gonzalez (1999), Gonzalez et al. (2001, 2002) Gonzalez (1999), Gonzalez et al. (2001, 2002) Gonzalez (1999), Gonzalez et al. (2001, 2002) Gonzalez (1999), Gonzalez et al. (2001, 2002) Gonzalez (1999), Gonzalez et al. (2001, 2002)

1.86 1.86 1.86

dm ˚) (A

B+ B+ B+ 75%

For references Gonzalez (1999), Gonzalez et al. (2001, 2002) the noted accuracy in column 11 is as provided by the authors.

Silicon, Si III Ground state: 1s22s22p63s21S0. Ionization energy: 33.493 eV = 270,139.3 cm1. Djenizˇe et al. (2002b) employed the same linear pulsed arc as in Djenizˇe et al. (1992b) (Pyrex tube 5 mm inner diameter and 7.7 cm length). Silicon is sputtered from the discharge tube wall. Oxygen and SF6 have been used at filling pressures of 130 and 70 Pa, respectively in order to facilitate erosion of the glass. The measured Stark shifts of seven, over the nine measured Si III lines are compared with calculated values by Dimitrijevic´ et al. (1991), on the basis of the semi-classical perturbation formalism (SCPF). Measured and calculated shifts values agree in the case of line belonging to the 4p3P0– 5s3S and 4p3P0–5s3S transitions within experimental accuracy and calculation uncertainties. But in the case of the 4f3F0–5g3G transition, lines calculated values are three times larger. This could be explained by the unknown composition ˚ lines, the different sign of the terms of these Si III lines and of the perturbing terms. For the k = 3096.83 and 4716.65 A between measured and calculated values can be explained by the uncertainties of the theoretical predictions related to the atomic data needed for such calculations.

Key data on experiments Ref.

Djenizˇe et al. (2002b)

Plasma source

Modified low-pressure pulsed arc

Method of measurement

Remarks

Electron density

Temperature

Single wavelength laser interferometer

Boltzmann plot of relative intensities on nine O III lines, Saha equation applied to O III and O IV lines

514

A. Lesage / New Astronomy Reviews 52 (2009) 471–535

Numerical results for Si III No.

Transition array

Multiplet

Wavelength ˚) (A

Temperature (K)

Electron density (1017 cm3)

1. 2. 3. 4.

3s3p–3p2 3d–4p 4p–4d 4p–5s

1 0 1

2541.82 3096.83 3806.53 3241.62 3233.95 4716.65 4813.33 4828.96 3258.66

53,000 53,000 53,000 53,000 53,000 53,000 52,000 52,000 52,000

1.00 1.00 1.00 1.00 1.00 1.00 1.00 1.00 1.00

5. 6.

4d–5f 4f–5g

1

7.

3d0 –4p0

3

P–D D–3P0 3 0 3 P–D 3 0 3 P–S 3

D–1F0 F–G

3 0 3

D0–3P

wm ˚) (A

wm/ wth

˚) dm (A

dm/ dth

Acc.

Ref.

0.010 ± 0.008 0.017 ± 0.008 0.063 ± 0.008 0.068 ± 0.008 0.116 ± 0.008 0.015 ± 0.008 0.128 ± 0.008 0.147 ± 0.008 0.025 ± 0.008

– 3.7 1.43 0.6 1.04 0.53 0.3 0.35 –

B B B B B B B B B

Djenizˇe Djenizˇe Djenizˇe Djenizˇe Djenizˇe Djenizˇe Djenizˇe Djenizˇe Djenizˇe

et et et et et et et et et

al. al. al. al. al. al. al. al. al.

(2002b) (2002b) (2002b) (2002b) (2002b) (2002b) (2002b) (2002b) (2002b)

The noted accuracy for dm is as provided by the authors.

Silicon, Si IV Ground state: 1s22s22p63s2S1/2. Ionization energy: 45.142 eV = 364,093.1 cm1. Djenizˇe et al. (2002b) employed the modified low pressure pulsed arc Milosavljevic´ et al. (2000) operated in pure oxygen plasma. Silicon is sputtered from the Pyrex discharge tube. The measured Stark shifts of six Si IV lines are compared with calculated values by Dimitrijevic´ et al. (1991), on the basis of the semi-classical perturbation formalism (SCPF). Agreement ˚ line. According to the authors the Stark is within mutual error bar, except for the higher lying 5p2P0–5d2D, k = 6701.21 A ˚. shifts accuracy is ± 0.008A Key data on experiments Ref.

Plasma source

Djenizˇe et al. (2002b)

Low-pressure pulsed arc

Method of measurement

Remarks

Electron density

Temperature

˚ and Stark widths of Laser interferometer at 6328 A S III and O III lines

Boltzmann plot of O III lines and intensity ratios of S III to S II lines

Numerical results for Si IV No.

Transition array

Multiplet

Wavelength ˚) (A

Temperature (K)

Electron density (1017 cm3)

1. 2.

4s–4p 4p–4d

2

3.

4d–5p

2

4.

5p–5d

2 0 2

4088.85 3149.56 3165.71 3762.44 3773.15 6701.21

33,000 52,000 31,000 32,000 32,000 52,000

1.0 1.0 1.0 1.0 1.0 1.0

S–2P0 P–D

2 0 2

D–2P0 P–D

wm ˚) (A

wm/ wth

˚) dm (A

dm/ dth

Acc.

Ref.

0.012 0.020 0.017 0.015 0.003 0.075

1.4 1.7 1.5 8 1.6 3

– – – – – –

Djenizˇe Djenizˇe Djenizˇe Djenizˇe Djenizˇe Djenizˇe

et et et et et et

al. al. al. al. al. al.

(2002b) (2002b) (2002b) (2002b) (2002b) (2002b)

Silver, Ag I Ground state: 1s22s22p63s23p63d104s24p64d105s2S1/2. Ionization energy: 7.57623 eV = 61,106.45 cm1. Djenizˇe et al. (2005c) measured two neutral silver lines in a modified version of a linear low pressure pulsed arc (Wang et al., 1990). Observations were made end-on and spectral profiles recorded by a step-by-step technique. Thin (200 lm) silver cylindrical plates (l = 16 mm) have been posted inside the cylindrical linear part of the discharge tube (l = 14 cm, 5 mm diameter) on its ends. The working gas was nitrogen (97% N + 3% O) flowing at 133 Pa. The absence of self absorption for the two Ag I lines was checked using the method described in Sharon et al. (1997). The standard Davies and Vaughan (1963) deconvolution procedure was applied using the least squares algorithm. van der Waals and resonance broadening were neglected. The Ag ion contribution was assumed to be small and consequently the experimental profile symmetrical. No theoretical or experimental parameters exist for comparison.

A. Lesage / New Astronomy Reviews 52 (2009) 471–535

515

Key data on experiments Ref.

Plasma source

Method of measurement

Djenizˇe et al. (2005c)

Modified low-pressure pulsed arc

Remarks

Electron density

Temperature

˚ N III 4634.13 and 4640.64 A Stark widths

˚ /NIII Relative intensity ratio of NII 4630.54, 4643.09 A ˚ lines 4634.13, 4640.64 A

Numerical results for Ag I No.

Transition array

Multiplet

Wavelength ˚) (A

Temperature (K)

Electron density (1017 cm3)

wm ˚) (A

1.

5p–5d

2

5209.08

18,100

0.66

0.240

5465.50

18,100

0.66

0.262

P–2D

wm/ wth

˚) dm (A

dm/ dth

Acc.

Ref.

0.033 ± 0.008

B

0.036 ± 0.008

B

Djenizˇe et al. (2005c) Djenizˇe et al. (2005c)

The noted accuracy for dm is as provided by the authors.

Silver, Ag II Ground state: 1s22s22p63s23p63d104s24p64d101S0. Ionization energy: 21.47746 eV = 173,227.4 cm1. Djenizˇe et al. (2005c) measured 11 singly-ionized silver lines in a nitrogen plasma in a modified version of a linear low pressure pulsed arc (Wang et al., 1990). Observations were made end-on and spectral profiles recorded by a step-by-step technique. Thin (200 lm) silver cylindrical plates (l = 16 mm) have been posted inside the cylindrical linear part of the discharge tube (l = 14 cm, 5 mm diameter) on its ends. The working gas was nitrogen (97% N + 3% O) flowing at 133 Pa. Self absorption was checked using the method described in Sharon et al. (1997), authors did not mention any correction. The standard (Davies and Vaughan, 1963) deconvolution procedure was applied using the least squares algorithm. van der Waals and resonance broadening were neglected. No theoretical or experimental parameters exist for comparison.

Key data on experiments Ref.

Plasma source

Method of measurement

Remarks

Electron density

Temperature

Djenizˇe et al. (2005c)

Modified low-pressure pulsed arc

˚ N III k 4634.13 and 4640.64 A Stark widths

˚ /NIII k Relative intensity ratio of NII k 4630.54, 4643.09 A ˚ lines 4634.13, 4640.64 A

Numerical results for Ag II No.

Transition array

Multiplet

Wavelength ˚) (A

Temperature (K)

Electron density (1017 cm3)

wm ˚) (A

1.

5s–5p

3

2113.82 2246.43 2248.74 2320.29 2324.68 2331.40 2411.41 2413.23 2437.81 2447.93 2767.54

17,600 18,000 18,000 17,600 17,600 17,600 18,100 18,100 17,600 17,600 17,600

1.10 0.65 0.65 1.10 1.10 1.10 0.66 0.66 1.10 1.11 1.10

0.128 0.160 0.164 0.208 0.214 0.176 0.168 0.184 0.238 0.218 0.148

D–3D D–3F 3 D–3D 1 D–3F 3 D–3F 3 D–3P 3 D–3D 3 D–3F 3 D–3P 1 D–3F 1 D–3F 3

The noted accuracy for dm is as provided by the authors.

Silver, Ag III Ground state: 1s22s22p63s23p63d104s24p64d92D5/2. Ionization energy: 34.82 eV = 280,900 cm1.

wm/ wth

˚) dm (A .043 ± 0.008 .006 ± 0.008 .005 ± 0.008 .0077 ± 0.008 .0061 ± 0.008 .0055 ± 0.008 .0078 ± 0.008 .0073 ± 0.008 .0096 ± 0.008 – –

dm/ dth

Acc.

Ref.

B B B B B B B B B B B

Djenizˇe Djenizˇe Djenizˇe Djenizˇe Djenizˇe Djenizˇe Djenizˇe Djenizˇe Djenizˇe Djenizˇe Djenizˇe

et et et et et et et et et et et

al. al. al. al. al. al. al. al. al. al. al.

(2005c) (2005c) (2005c) (2005c) (2005c) (2005c) (2005c) (2005c) (2005c) (2005c) (2005c)

516

A. Lesage / New Astronomy Reviews 52 (2009) 471–535

Djenizˇe et al. (2005c) measured three doubly-ionized silver lines, in a nitrogen plasma, in a modified version of a linear low pressure pulsed arc (Wang et al., 1990). Observations were made end-on and spectral profiles recorded by a step-bystep technique. Thin (200 lm) silver cylindrical plates (l = 16 mm) have been posted inside the cylindrical linear part of the discharge tube (l = 14 cm, 5 mm diameter) on its ends. The working gas was nitrogen (97% N + 3% O) flowing at 133 Pa. Self absorption was checked using the method described in Sharon et al. (1997) authors did not mention any correction. The standard (Davies and Vaughan, 1963) deconvolution procedure was applied using the least squares algorithm. van der Waals and resonance broadening were neglected. No theoretical or experimental parameters exist for comparison.

Key data on experiments Ref.

Plasma source

Djenizˇe et al. (2005c)

Method of measurement

Modified low-pressure pulsed arc

Remarks

Electron density

Temperature

˚ N III 4634.13 and 4640.64 A Stark widths

˚ /NIII Relative intensity ratio of NII 4630.54, 4643.09 A ˚ lines 4634.13, 4640.64 A

Numerical results for Ag III No.

Transition array

Multiplet

Wavelength ˚) (A

Temperature (K)

Electron density (1017 cm3)

wm ˚) (A

1.

5s–5p

2

2161.89

19,200

1.15

.172

2310.04

19,200

1.15

.174

2395.69

19,200

1.15

.276

F–4G

4

P–4D

wm/ wth

˚) dm (A 0.007 ± 0.008

dm/ dth

Acc.

Ref.

B

Djenizˇe et al. (2005c) Djenizˇe et al. (2005c) Djenizˇe et al. (2005c)

B 0.0087 ± 0.008

B

The noted accuracy for dm is as provided by the authors.

Sodium, Na I Ground state: 1s22s22p63s2S1/2. Ionization energy: 5.1391 eV = 41,449.6 cm1. Miokovic´ et al. (2005) used 400 W, Hg–Xe and Na–Cd–Xe, high pressure discharges (l = 95 mm, diam. = 7.6 mm, current 2.6–4.2 A, 50 Hz) to measure line width and shift of five Na I lines. The central part of the plasma was spectroscopically observed side-on, with the slit parallel to the discharge axis. The light of the discharge was spectrally resolved by a Karl Zeiss, SPM-2, 10 lm wide slit, medium resolution, monochromator. The light signal was detected by an EMI 9558 QB photomultiplier at a delay time and aperture duration convenient for observation of the discharge at maximum. The elec˚ line shift values Dimitrijevic´ and Sahal-Bre´chot (1985), Kettlitz and Olttron density is measured via the Na I k 4751.8 A manns (1996). Miokovic´ et al. (2005) justify the choice of the 3P–7S transition, because in that case the two main contributions to the line shift came from the interaction with the 7S and 3P levels and lead to shifts of opposite sign (Kettlitz and Oltmanns, 1996). The validity criteria for the assumption of LTE were checked, as well as those of the isolated-line ´˚ approximation (not fulfilled in the case of the Na I k 4668 A line). van der Waals and Doppler broadening were correctly evaluated, as well as the ion contribution (the contribution of the ions to the total line width and shift of the 32P–n2S lines is estimated to be less than 10%, and for the 32P–n2D lines up to 25% of the full Stark width). The synthetic line shapes, calculated with the Bartels’ method taking in account the Stark and van der Waals broadening as well as the optical depth of the plasma (Zwicker, 1968) were numerically convoluted (Press et al., 1995) with the instrumental profile and compared to the observed experimental profile. The line width retained as the Stark contribution was the value introduced in the calculations to obtain the best fit. A slight residual is attributed to the quasi-static ion broadening. ˚´ lines are larger than Dimitrijevic´ and Miokovic´ et al. (2005) measured values of the shifts for Na I k 5153.4 and 6154.2 A ˚´ measured shift Sahal-Bre´chot (1985) and Griem (1974) calculated values. van den Hoek and Visser (1981) Na I k 6154.4 A ˚´ value agrees well, within the error bar, with Miokovic´ et al. (2005) value. Their measured width values for the k 5153.4 A line are in good agreement with calculated values in Dimitrijevic´ and Sahal-Bre´chot (1985) and in Griem (1974), while ˚´ lines are slightly larger, but still within the mutual error bar. For the Na I k 4668.56 those for k 6154.2 and 4751.8 A ´ ˚ and 4982.8 A lines, Miokovic´ et al. (2005) shifts measured values are in agreement with those of Kettlitz and Oltmanns (1996) and van den Hoek and Visser (1981). Theoretical values (Dimitrijevic´ and Sahal-Bre´chot, 1985; Kettlitz and Olt-

A. Lesage / New Astronomy Reviews 52 (2009) 471–535

517

manns, 1996; Griem, 1974) are in very good agreement with experimental measurements in the case of the Na I k 4668.56 ´˚ ´˚ and 4982.8 A lines shifts, but Dimitrijevic´ and Sahal-Bre´chot (1985) calculated value for the Na I k 4668.56 A line, is much lower than the measured values. Key data on experiments Ref.

Plasma source

Method of measurement

Remarks

Electron density Miokovic´ et al. (2005)

Wall-stabilized AC-driven high-pressure Na– Hg–Xe and Na–Cd–Xe discharges (l = 95 mm; diam. = 7.6 mm; current 2.6–4.2 A)

Temperature

˚´ line compared to Stark shift of Na I k 4751.822 A calculated (Fuhr et al., 1972) and measured (Konjevic´ and Roberts, 1976) data

Comparison of the measured sodium line profiles to the calculated ones

Numerical results for Na I Wavelength ˚) (A

Temperature (K)

Electron density (1017 cm3)

wm a ˚) (A

3P–5S

6154.225

2.

3P–6S

5153.402

3.

3P–7S

4751.822

3P–5D

4982.808

5.

3P–6D

4668.560

0.06 0.1 0.06 0.1 0.06 0.1 0.06 0.1 0.06 0.1

0.16 0.23 0.3 0.5 0.6 0.95

4.

3800 4100 3800 4100 3800 4100 3800 4100 3800 4100

No.

Transition array

1.

a

Multiplet

wm/ wth

dma ˚) (A

dm/ dth

0.3 0.7 0.5 0.8 0.65 1.1 1.0 1.9 1.0 2.0

Acc.

Ref.

C+,C C+,C C+,C C+,C C+ C+ C C C C

Miokovic´ Miokovic´ Miokovic´ Miokovic´ Miokovic´ Miokovic´ Miokovic´ Miokovic´ Miokovic´ Miokovic´

et et et et et et et et et et

al. al. al. al. al. al. al. al. al. al.

(2005) (2005) (2005) (2005) (2005) (2005) (2005) (2005) (2005) (2005)

Numerical values wm an dm read on Miokovic´ et al. (2005) graphs, for the two extreme values of Ne and T.

Sulfur, S III Ground state: 1s22s22p63s23p23P0. Ionization energy: 34.83 eV = 280,900 cm1. Srec´kovic´ et al. (2003) measured 10 widths and shifts of doubly ionized sulfur lines with the linear pulsed arc described in Sreckovic´ et al. (2001b). The Pyrex discharge tube of 5 mm inner diameter had plasma length of 6.3 cm. The test gas was SF6 at 130 Pa in a flowing regime (10 ml/min). Reproducibility was 95%. The absence of self-absorption was checked by the method described in Djenizˇe and Bukvic´ (2001). The standard deconvolution procedure (Davies and Vaughan, 1963) was applied using the least square algorithm. Srec´kovic´ et al. (2003) calculated the corresponding values using the semi-classical perturbation formalism SCPF,Dimitrijevic´ and Sahal-Bre´chot (1996b,c), the modified semiempirical method Dimitrijevic´ and Konjevic´ (1980, 1981), and the simplified semi-classical theory Eq. (526) in Griem (1974). A very good agreement is found between measured and calculated width values in the 3d–4p and 4s-4p transitions, except in the multiplet (4) where SCPF values overvalue experimental data of 35%. Modified semi-empirical and the modified semi-classical theories also agree with Srec´kovic´ et al. (2003) width measured values. Measured and calculated values by Srec´kovic´ et al. (2003) are in very good agreement with those measured by Platisˇa et al. (1979) and Djenizˇe et al. (2002c) earlier.

Key data on experiments Ref.

Plasma source

Srec´kovic´ et al. (2003)

Modified low-pressure pulsed arc

Method of measurement Electron density

Temperature

Laser interferometer ˚ at 6328 A

Boltzmann plot of six F II lines

Remarks

Diagnostics methods are not described. Authors refer to earlier publications (S IV 2002)

518

A. Lesage / New Astronomy Reviews 52 (2009) 471–535

Numerical results for S III No.

Transition array

Multiplet

Wavelength ˚) (A

Temperature (K)

Electron density (1017 cm3)

wm ˚) (A

1.

3p3d– 3p(2P0)4p

3 0 3

3709.338

30,400 31,200 33,600 38,300 30,400 31,200 33,600 38,300 30,400 31,200 33,600 38,300 30,400 31,200 33,600 38,300 30,400 31,200 33,600 38,300 30,400 31,200 33,600 38,300 30,400 31,200 33,600 38,300

2.75 2.84 2.80 2.43 2.75 2.84 2.80 2.43 2.75 2.84 2.80 2.43 2.75 2.84 2.80 2.43 2.75 2.84 2.80 2.43 2.75 2.84 2.80 2.43 2.75 2.84 2.80 2.43

.431 .361 .360 .379 .434 .440 .456 .329 .518 .477 .421 .423 .615 .470 .462 .478 .683 .669 .618 .629 .725 .695 .743 .724 .802 .665 .626 .630

30,400 31,200 33,600 38,300 30,400 31,200 33,600 38,300 30,400 31,200 33,600 38,300

2.75 2.84 2.80 2.43 2.75 2.84 2.80 2.43 2.75 2.84 2.80 2.43

.755 .647 .640 .614 .785 .794 .781 .770 .722 .669 .663 .638

P–D (1)

3710.422

3 0 3

P–P (2)

2.

3370.351

3387.092

3

D0–3P (8)

3.

3928.556

3983.723

4.

3p4s– 3p(2P0)4p

5.

3 0 3

P–D (4)

4361.468

3 0 3

P–P (5)

3899.093

3 0 3

3661.942

P–S (6)

6.

3717.717

wm/ wth

dm (pm)

1.1 ± 0.5

1.4 ± 1.2

0.0 ± 0.6

0.0 ± 0.6

5.2 ± 0.9

7.6 ± 1.2

0.3 ± 0.1

1.1 ± 0.5

3.7 ± 0.7

1.2 ± 0.6

dm/ dth

Acc.

Ref.

B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+

Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´ Srec´kovic´

B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+ B+

et et et et et et et et et et et et et et et et et et et et et et et et et et et et et et et et et et et et et et et et et

al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al.

(2003) (2003) (2003) (2003) (2003) (2003) (2003) (2003) (2003) (2003) (2003) (2003) (2003) (2003) (2003) (2003) (2003) (2003) (2003) (2003) (2003) (2003) (2003) (2003) (2003) (2003) (2003) (2003) (2003) (2003) (2003) (2003) (2003) (2003) (2003) (2003) (2003) (2003) (2003) (2003) (2003)

The noted accuracy for dm is as provided by the authors.

Sulfur, S IV Ground state: 1s22s22p63s23p2P1/2. Ionization energy: 47.29 eV = 381,541.4 cm1. Djenizˇe et al. (2002c) used a pulsed discharge described in Djenizˇe et al. (1992b) and Djenizˇe et al. (2002a) to observe, end-on, Stark broadened line profiles of S IV, on a shot-to-shot basis. The test gas was pure SF6 at 130 Pa filling pressure in a flowing regime (10 ml/min) and the plasma reproducibility was 95%. The optical depth was checked via line intensity ratios within multiplets during the plasma decay. Compared to theoretical ratios, they differed by less than ±1%. The line widths were corrected for instrumental and Doppler contributions. van der Waals and resonance broadening were found to be negligible. The effects of possible inhomogeneous plasma end-layers were not discussed. Calculated values obtained with the semi-classical perturbation formalism SCPF, Dimitrijevic´ et al. (1996) and the simplified Griem (1974) semi-classical method calculated by Dimitrijevic´ and Konjevic´ (1981) agree better with the experimental results than those done with Griem (1968b) semi-empirical calculations or their modified version Dimitrijevic´ et al. (1996).

A. Lesage / New Astronomy Reviews 52 (2009) 471–535

519

Key data on experiments Ref.

Plasma source

Method of measurement

Remarks

Electron density

Temperature

Djenizˇe et al. (2002c)

Low-pressure pulsed arc

˚ Laser interferometer at 6328 A

Boltzmann plot of six F II spectral lines

Numerical results for S IV No.

Transition array

Multiplet

Wavelength ˚) (A

Temperature (K)

Electron density (1017 cm3)

wm ˚) (A

1.

4s–4p

2

3097.273

30,400 33,600 30,400 33,600

2.75 2.80 2.75 2.80

0.638 0.602 0.580 0.532

S–2P0

2.

3117.615

wm/ wth

˚) dm (A

dm/ dth

0.039 ± 0.08 0.0 ± 0.08

Acc.

Ref.

B+ B+ B+ B+

Djenizˇe Djenizˇe Djenizˇe Djenizˇe

et et et et

al. al. al. al.

(2002c) (2002c) (2002c) (2002c)

Tin, Sn I Ground state: 1s22s22p63s23p63d104s24p64d105s25p23P0. Ionization energy: 7.3439 eV = 59,232.5 cm1. Djenizˇe et al. (2006d) measured widths of 12 Sn I lines in a modified version of a low-pressure pulsed arc (Djenizˇe et al., 2006a; Djenizˇe et al., 2005c), end-on, with a shot-to-shot scanning technique. The working gas was helium (90% He + 7% N + 3% O) flowing at 1330 Pa. Thin (150 lm) tin cylindrical plates were posted inside the cylindrical part of the discharge tube on its ends, in order to provide uniform distribution of the tin atoms in the plasma. The absence of self absorption was checked using the method described in Djenizˇe and Bukvic´ (2001). For the estimation of the spectral line parameters a deconvolution procedure (Davies and Vaughan, 1963) based on the least-squares algorithm is applied. The estimation of the spectrum base line is done according to the method proposed by Bukvic´ and Spasojevic´ (2005). van der Waals and resonance broadening were neglected, as the Tin ion contribution to the line shape and consequently the symmetrical Voigt profile was used. Taking into account the proportionality of the width with the electron density, the comparison with ˚ Miller et al. (1979b) and Martinez and Blanco (1999) experimental value shows that for Sn I k 3175.05, 4524.74, 3262.34 A ˚ line more lines, Djenizˇe et al. (2006d) values are about four times smaller, and for the most investigated Sn I k 4524.74 A ˚ , lines, Djenizˇe et al. (1992a) previously measured values at than four times than theirs. For k 2839.99, 2863,32, 3034.12 A much higher temperature are about two times smaller. For six of the Sn I measured lines there are no previously measured values. No theoretical value exist for comparison. Key data on experiments Ref.

Plasma source

Djenizˇe et al. (2006d)

Low-pressure pulsed arc

Method of measurement Electron density Laser interferometer at ˚ 6328 A

Remarks

Temperature ˚ and O III k 3961.57 A ˚ and Relative intensity ratio between O II k 3973.26 A ˚ ˚ between Sn I k 3330.62 A and Sn II k 3351.97 A

Numerical results for Sn I No.

Transition array

Multiplet

Wavelength ˚) (A

Temperature (K)

Electron density (1017 cm3)

wm ˚) (A

1.

5p2–6s

3

2839.99 2863.32 2706.51 3034.12 3009.14 3175.05 2661.24 4524.74 5631.71 3262.34 3330.62 3801.02

13,000 13,000 12,800 13,000 13,000 13,000 12,800 13,000 13,000 13,000 13,000 13,000

.51 .51 .60 .51 .51 .51 .60 .51 .51 .51 .51 .51

.176 .124 .164 .200 .210 .120 .134 .134 .424 .176 .216 .228

3

P–3P

D-1P S-1P 1 3 S- P 1 D-1P 1 D-3P 1

In column 10 the accuracy is as in Djenizˇe et al. (2006d) publication.

wm/ wth

dm ˚) (A

dm/ dth

Acc. Dwm ˚) (A

Ref.

± .028 ± .020 ± .026 ± .032 ± .034 ± .019 ± .021 ± .021 ± .068 ± .028 ± .035 ± .036

Djenizˇe Djenizˇe Djenizˇe Djenizˇe Djenizˇe Djenizˇe Djenizˇe Djenizˇe Djenizˇe Djenizˇe Djenizˇe Djenizˇe

et et et et et et et et et et et et

al. al. al. al. al. al. al. al. al. al. al. al.

(2006d) (2006d) (2006d) (2006d) (2006d) (2006d) (2006d) (2006d) (2006d) (2006d) (2006d) (2006d)

520

A. Lesage / New Astronomy Reviews 52 (2009) 471–535

Tin, Sn II Ground state: 1s22s22p63s23p63d104s24p64d105s2 5p2P1/2. Ionization energy: 14.632 eV = 118,017.0 cm1. Djenizˇe et al. (2006d) measured widths of 16 Sn II lines in a modified version of a low-pressure pulsed arc (Djenizˇe et al., 2005c; Sreckovic´ et al., 2000), end-on, with a shot-to-shot scanning technique. The working gas was helium (90% He + 7% N + 3% O) flowing at 1330 Pa. Thin (150 lm) tin cylindrical plates were posted inside the cylindrical part of the discharge tube on its ends, in order to provide uniform distribution of the tin atoms in the plasma. The absence of self absorption was checked using the method described in Djenizˇe and Bukvic´ (2001). For the estimation of the spectral line parameters a deconvolution procedure (Davies and Vaughan, 1963) based on the least-squares algorithm is applied. The estimation of the spectrum base line is done according to the method proposed by Bukvic´ and Spasojevic´ (2005). van der Waals and resonance broadening were neglected. Djenizˇe et al. (2006d) measured values are four times smaller, on average, in comparison with those measured by Miller et al. (1979b), Puric´ et al. (1985) and Martinez and Blanco (1999) (when the data are scaled to the same electron density) and confirm the data found by Djenizˇe et al. (1990) earlier. Comparison with values calculated by Konjevic´ and Konjevic´ (2000) according to the semi-empirical approach are noted in column 8 of the numerical results table. The agreement is within the experimental accuracy and the estimated uncertainties of the calculated values.

Key data on experiments Ref.

Plasma source

Djenizˇe et al. (2006d)

Low-pressure pulsed arc

Method of measurement

Remarks

Electron density

Temperature

Laser interferometer at ˚ 6328 A

˚ and O III k 3961.57 A ˚ and between Sn Relative intensity ratio between O II k 3973.26 A ˚ and Sn II k 3351.97 A ˚ spectral lines I k 3330.62 A

Numerical results for Sn II No.

Transition array

Multiplet

Wavelength ˚) (A

Temperature (K)

Electron density (1017 cm3)

wm ˚) (A

1.

6s–6p

2

S–2P0

2 3

5p2–6p 5p2–4f

2

D–2P0 D–2F0

4 5

5p2–7p 5d–4f

2

6 7

5d–7p 6p–7s

2

8

6p–6d

2 0 2

9 10

6p–8s 6p–7d

2 0 2

6453.50 6844.05 7387.79 3283.21 3351.97 3047.50 5588.92 5797.20 5799.18 4877.22 6761.45 7191.40 5332.36 5561.95 3841.44 3472.46

13,000 13,000 13,000 13,000 13,000 13,000 13,000 13,000 13,000 13,000 13,000 13,000 13,000 13,000 13,000 13,000

0.51 0.51 0.51 0.51 0.51 0.51 0.51 0.51 0.51 0.51 0.51 0.51 0.51 0.51 0.51 0.51

.428 .560 1.10 .194 .228 .228 .310 .548 .366 .445 .920 .502 .298 .355 .660 .496

2

2

D–2P0 D–2F0

D–2P0 P–S

2 0 2

P–D P–S P–D

2 0 2

wm/wthwth: ref. (Konjevic´ and Konjevic´, 2000) .66 .77 0.83 0.98 .58 0.70 0.65 0.61 .56 .51 .54 .32 1.22

˚) dm(A

dm/ dth

Acc. Dwm ˚) (A

Ref.

± .06 ± .078 ± .15 ± .037 ± .032 ± .032 ± .043 ± .077 ± .051 ± .062 ± .13 ± .070 ± .042 ± .050 ±.092 ± .069

Djenizˇe Djenizˇe Djenizˇe Djenizˇe Djenizˇe Djenizˇe Djenizˇe Djenizˇe Djenizˇe Djenizˇe Djenizˇe Djenizˇe Djenizˇe Djenizˇe Djenizˇe Djenizˇe

et et et et et et et et et et et et et et et et

al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al.

(2006d) (2006d) (2006d) (2006d) (2006d) (2006d) (2006d) (2006d) (2006d) (2006d) (2006d) (2006d) (2006d) (2006d) (2006d) (2006d)

In column 11 the accuracy is as in Djenizˇe et al. (2006d) publication.

Tin, Sn III Ground state: 1s22s22p63s23p63d104s24p64d105s21S0. Ionization energy: 30.503 eV = 246,020.0 cm1. Kieft et al. (2004a) observed four Sn III lines in a pinched discharge plasma used for semiconductor lithography (Kieft et al., 2004b). A thin layer of liquid tin is spread on the cathode discharge and vaporized during the trigger phase of the discharge. The plasma has a needle-like shape with a radius of 100 lm and is observed with an intensified charge-coupled

A. Lesage / New Astronomy Reviews 52 (2009) 471–535

521

device (ICCD) camera, side-on. No Abel inversion has been applied to the spectra. Consequently the authors estimated that the determination of the electron density is affected by an error of 25%. The line width is determined by adjusting a convolution of the apparatus function with a variable Lorentzian profile to the experimental one. The width of the apparatus profile is measured by using one of the Sn III lines emitted from outer regions of the plasma during the decay phase. Due to experimental conditions, natural broadening is neglected and Doppler broadening is estimated to be of the order of ˚ . Kieft et al. (2004a) do not mention self-absorption but the possible contribution of the electric and magnetic fields 0.25 A to the line broadening. Comparison with Griem (1968b) semi-empirical calculation is shown in column 8 of the table. Key data on experiments Ref.

Plasma source

Method of measurement

Kieft et al. (2004a)

Discharge used for semiconductor lithography

Remarks

Electron density

Temperature

˚ lines Known Stark widths of Sn II k 5333.9 A and cross-calibration of the Stark width of Sn II to Sn III lines. Thomson scattering method

Thomson scattering method

Stark width data used for Ne measurement are not very accurate

Numerical results for Sn III No.

Transition array

Multiplet

Wavelength ˚) (A

Temperature (K)

Electron density (1017 cm3)

wm ˚) (A

wm/wth wth: Griem (1968b)

1.

6p–5d

3 0 3

5293

11,600

1.0

0.43

5351

11,600

1.0

5371

11,600

5226

11,600

2.

6p–6s

P–D

1 0 1

P–S

dm ˚) (A

dm/ dth

Acc.

Ref.

1.43

C

0.34

1.13

C

1.0

0.32

1.06

C

1.0

0.61

1.69

C

Kieft et (2004a) Kieft et (2004a) Kieft et (2004a) Kieft et (2004a)

al. al. al. al.

Xenon, Xe II Ground state: 1s2 2s2 2p6 3s2 3p6 3d10 4s2 4p6 4d10 5s2 5p52 P03=2 . Ionization energy: 21.21 eV = 171,068.4 cm1. Djurovic´ et al. (2006f), measured 80 Xe II lines in a pulsed (300 ls long, 20 lF, 9000 V) capacitor discharge plasma source. A 175 mm long and 19 mm internal diameter Pyrex glass tube was continuously flowed with helium at 3 kPa. Approximately 5% of xenon was added to the carrier gas and the flow was adjusted to obtain minimal self-absorption and maximal intensity of the lines. Spectroscopic observation and interferometric measurement were performed along the tube axis and symmetrically to the axis. The spectra was time resolved and recorded with a monochromator and a optical multichannel analyzer. Profiles were recorded with and without a mirror positioned behind the discharge tube in order to check possible self-absorption, found as negligible for all measured lines. The Davies and Vaughan (1963) procedure was used to obtain the Stark width from the experimental profile. van der Waals, ionic and resonance broadening were negligibly small for the experimental conditions. Djurovic´ et al. (2006f) measurements are compared with Lesage et al. (1981), Miller et al. (1982), Richou et al. (1984), Nick and Helbig (1986), Vitel and Skowronek (1987a), Manola et al. (1988), Lesage et al. (1989), Konjevic´ and Uzelac (1990), Bertuccelli et al. (1991a,b) and Gigosos et al. (1994) experimental values. But we do not retain for such a comparison those obtained in the pioner’s experiments done using photographic techniques by Lesage et al. (1981), Miller et al. (1982) and Lesage et al. (1989) as well as the ones by Bertuccelli et al. (1991a,b) because in that last two cases electron density is measured by comparison of Xe II line widths with those obtained before by several authors. The present comparison takes in account the temperature variation of the Stark parameter as predicted by the theory ˚ line. The case of that line is Dimitrijevic´ and Konjevic´ (1980) and measured by Manola et al. (1988) for the Xe II k 5419 A of particular interest because the comparison for that line width is graphically done by Djurovic´ et al. (2006f), versus temperature, with most of the previous measured and calculated values, and all results show similar behavior as those shown in these figure. That graph shows that: (1) Measurements done with the same experimental set up earlier by Gigosos et al. (1994) but using a different method of ˚ Stark broadening parameter and a He Ne laser interferometer at k 6328 A ˚) electron density measurement (the He I 5016 A provides values larger than those obtained in Djurovic´ et al. (2006f), but using a two wavelength laser interferometer. As the second method of measurement provides a better accuracy that last value is retained for further comparison.

522

A. Lesage / New Astronomy Reviews 52 (2009) 471–535

(2) Nick and Helbig (1986), Vitel and Skowronek (1987a) values seems systematically too small. Possible explanation of these discrepancies could be, in both cases, the inhomogeneity of the sources due to boundary layers for the wall stabilized cascade arc observed end-on in the first case and the narrow pulsed linear discharge observed side-on in the second case. (3) A remarkable agreement is found between Djurovic´ et al. (2006f), Richou et al. (1984), Manola et al. (1988), Konjevic´ and Uzelac (1990) measured values. In the tree cases the homogeneity and the optical depth of the plasma has been carefully checked. The modified semi-empirical calculations of Djurovic´ et al. (2006f) according to Dimitrijevic´ and Konjevic´ (1980), using the jj-coupling with a complete set of perturbing levels, provide values in good agreement with their measured values except ˚ , as well as with those of: Richou et al. (1984), Manola et al. (1988), Konjevic´ and for Xe II k 4844.33 and k 3420.73 A Uzelac (1990). The theoretical values published by Popovic´ and Dimitrijevic´ (1996), which use the same theory but with the jk coupling agree within error bars. Djurovic´ et al. (2006f) have attributed an estimated accuracy to each of their Stark half-widths measurement. As such estimates are largely justified by their description of the experimental set-up, plasma diagnostic, spectral treatments and by ˚ line, with the four above mentioned earlier experimental results, they are the agreement, in the case of the Xe II k 5419 A kept in the table of numerical results. ´ irisˇan et al. (2007) measured the shifts of 110 Xe II lines with the same experimental set up and methods as for the C widths (Djurovic´ et al., 2006f), measured values are compared with the values measured by Vitel and Skowronek ˚ . The shift is toward the blue in both cases but C ´ irisˇan et al. (2007) values are (1987a) for the k 5292.22 and 5419.15 A almost two times larger. In the case of Gigosos et al. (1994) measurements, they are 15 spectral lines to compare and except ˚ ) the agreement is in some instances very good. Calculations done in four cases (k 4603.03, 5372.39, 5260.44 and 4991.17 A ´ ˇ by Cirisan et al. (2007) according to the modified semi-empirical formula Dimitrijevic´ and Krsˇljanin (1986), using the jk coupling scheme, provide values larger than the experimental ones for the 6s–6p and 5d–6p transitions (0.3 < dm/ dth < 0.97), only in a few case this ratio is below 0.3. For the 6p–7s, 6p–5d and 6p–6d transitions, the calculated shift values are always smaller (1.4 < dm/dth < 5, in most cases, and above 5 in several cases).

Ref.

Plasma source

Djurovic´ et al. (2006f)

Pulsed discharge

Method of measurement

Remarks

Electron density

Temperature

Two wavelengths Twyman–Green interferometer

Boltzmann plot of 24 Xe II lines

Numerical results for Xe II line width values No.

Configuration

Multiplet

Wavelength ˚) (A

Temperature (K)

Electron density (1017 cm3)

wm ˚) (A

1. 2. 3.

5s5p6–5p4(3P2)6p

2

S 1=2 –½203=2 S 1=2 –½101=2 2 S 1=2 –½103=2 2 S 1=2 –½201=2 ½25=2 –½205=2

4779.18 4384.93 3250.56 3384.13 5292.22

22,000 22,000 22,000 22,000 22,000

1.0 1.0 1.0 1.0 1.0

.4124 .4476 .2852 .309 .4903

½23=2 –½203=2 ½25=2 –½307=2 ½25=2 –½305=2 ½23=2 –½305=2 ½23=2 –½103=2 ½23=2 –½101=2 ½25=2 –½103=2

5976.46 4844.33 4890.09 5419.15 4603.03 5372.39 3500.36

22,000 22,000 22,000 22,000 22,000 22,000 22,000

1.0 1.0 1.0 1.0 1.0 1.0 1.0

½23=2 –½103=2

3420.73

22,000

½25=2 –½205=2

6036.20

½23=2 –½205=2 ½23=2 –½203=2 ½25=2 –½307=2 ½23=2 –½103=2 [2]3/2–[1]1/2

6277.54 6343.96 5460.39 4818.02 5667.56

4.

2

5s5p6–5p4(3P0)6p 5p4(3P2)6s– 5p4(3P2)6p

5.

6. 7 8. 9.

10. 11.

5p4(3P2)6s– 5p4(3P0)6p 5p4(3P2)6s– 5p4(3P1)6p 5p4(3P2)5d– 5p4(3P2)6p

wm/ wtha

dm ˚) (A

dm/ dth

Acc. (%)

Ref.

1.04

6–10 6–10 20–30 15–20 20–30

Djurovic´ Djurovic´ Djurovic´ Djurovic´ Djurovic´

et et et et et

al. al. al. al. al.

(2006f) (2006f) (2006f) (2006f) (2006f)

.5401 .5603 .4822 .5154 .4257 .4305 .2059

.86 1.39 1.18 .97 1.07 .85 .99

15–20 20–30 B 20–30 15–20 15–20 20–30

Djurovic´ Djurovic´ Djurovic´ Djurovic´ Djurovic´ Djurovic´ Djurovic´

et et et et et et et

al. al. al. al. al. al. al.

(2006f) (2006f) (2006f) (2006f) (2006f) (2006f) (2006f)

1.0

.3367

1.53

20–30

Djurovic´ et al. (2006f)

22,000

1.0

.5645

15–20

Djurovic´ et al. (2006f)

22,000 22,000 22,000 22,000 22,000

1.0 1.0 1.0 1.0 1.0

.59.98 .6060 .4659 .5496 .4979

6–10 15–20 15–20 20–30 20–30

Djurovic´ Djurovic´ Djurovic´ Djurovic´ Djurovic´

et et et et et

al. al. al. al. al.

(2006f) (2006f) (2006f) (2006f) (2006f)

A. Lesage / New Astronomy Reviews 52 (2009) 471–535

523

Table (continued) ˚ ) wm/wtha dm (A ˚ ) dm/dth Acc. wm (A (%)

Ref.

No.

Configuration

Multiplet

Wavelength ˚) (A

Temperature (K)

Electron density (1017 cm3)

12.

5p4(3P2)5d– 5p4(3P0)6p 5p4(3P2)5d– 5p4(3P2)6p

½25=2 –½103=2

3811.05

22,000

1.0

.2328

15–20

Djurovic´ et al. (2006f)

½37=2 –½205=2

6051.15

22,000

1.0

.5939

15–20

Djurovic´ et al. (2006f)

½37=2 –½307=2 ½37=2 –½305=2 ½37=2 –½205=2

5472.61 5531.07 3612.37

22,000 22,000 22,000

1.0 1.0 1.0

.5237 .5090 .2704

15–20 15–20 20–30

Djurovic´ et al. (2006f) Djurovic´ et al. (2006f) Djurovic´ et al. (2006f)

½11=2 –½101=2

5945.53

22,000

1.0

.5575

6–10

Djurovic´ et al. (2006f)

½13=2 –½103=2

5268.31

22,000

1.0

1.1513

20–30

Djurovic´ et al. (2006f)

½01=2 –½103=2

6397.99

22,000

1.0

.6980

.92

20–30

Djurovic´ et al. (2006f)

½01=2 –½103=2

4883.53

22,000

1.0

.3784

.95

15–20

Djurovic´ et al. (2006f)

½01=2 –½101=2 ½01=2 –½101=2

5191.37 4269.84

22,000 22,000

1.0 1.0

.4492 .3675

1.02 1.12

15–20 15–20

Djurovic´ et al. (2006f) Djurovic´ et al. (2006f)

½13=2 –½001=2

5438.96

22,000

1.0

.4488

.89

15–20

Djurovic´ et al. (2006f)

½13=2 –½203=2 ½13=2 –½205=2 ½11=2 –½101=2 ½13=2 –½103=2

4887.30 4921.48 5659.38 3720.80

22,000 22,000 22,000 22,000

1.0 1.0 1.0 1.0

.4786 .4647 .6666 .2307

1.13 1.13 1.05 .99

15–20 15–20 15–20 15–20

Djurovic´ Djurovic´ Djurovic´ Djurovic´

½11=2 –½101=2 ½11=2 –½103=2

3869.63 4988.77

22,000 22,000

1.0 1.0

.2915 .8076

1.05

20–30 15–20

Djurovic´ et al. (2006f) Djurovic´ et al. (2006f)

½13=2 –½203=2

4162.16

22,000

1.0

.3843

15–20

Djurovic´ et al. (2006f)

½01=2 –½103=2

6375.28

22,000

1.0

.5581

20–30

Djurovic´ et al. (2006f)

½01=2 –½203=2

5776.39

22,000

1.0

.5756

15–20

Djurovic´ et al. (2006f)

½01=2 –½101=2

3731.18

22,000

1.0

.4497

15–20

Djurovic´ et al. (2006f)

½25=2 –½407=2

3121.87

22,000

1.0

.6470

15–20

Djurovic´ et al. (2006f)

½25=2 –½307=2

3225.08

22,000

1.0

.4463

20–30

½35=2 –½307=2

6528.65

22,000

1.0

.8633

15–20

Djurovic´ et al. (2006f) Djurovic´ et al. (2006f) Djurovic´ et al. (2006f)

½25=2 –½307=2

4876.50

22,000

1.0

.3947

1.00

15–20

Djurovic´ et al. (2006f)

½25=2 –½305=2 ½23=2 –½305=2 ½25=2 –½103=2 ½25=2 –½205=2 ½23=2 –½205=2 ½23=2 –½203=2 ½25=2 –½307=2

5178.82 6270.82 4972.71 4414.84 5184.48 5261.95 5758.65

22,000 22,000 22,000 22,000 22,000 22,000 22,000

1.0 1.0 1.0 1.0 1.0 1.0 1.0

.4414 .6458 .4879 .3828 .4956 .4704 .5094

1.08 .92 1.10 1.13 .99 .91

6–10 15–20 15–20 20–30 15–20 20–30 6–10

Djurovic´ Djurovic´ Djurovic´ Djurovic´ Djurovic´ Djurovic´ Djurovic´

et et et et et et et

al. al. al. al. al. al. al.

(2006f) (2006f) (2006f) (2006f) (2006f) (2006f) (2006f)

½23=2 –½101=2 ½23=2 –½205=2 ½25=2 –½205=2 ½203=2 –½25=2

4668.49 4787.77 5125.70 4823.35

22,000 22,000 22,000 22,000

1.0 1.0 1.0 1.0

.5083 .5765 .5717 1.2669

20–30 6–10 15–20 15–20

Djurovic´ Djurovic´ Djurovic´ Djurovic´

et et et et

al. al. al. al.

(2006f) (2006f) (2006f) (2006f)

½205=2 –½25=2 ½203=2 –½01=2

4862.45 4296.4

22,000 22,000

1.0 1.0

1.2118 .7283

20–30 15–20

Djurovic´ et al. (2006f) Djurovic´ et al. (2006f)

13. 14. 15. 16. 17. 18. 19.

20. 21.

5p4(3P2)5d– 5p4(3P1)6p 5p4(3P2)5d– 5p4(3P2)6p 5p4(3P2)5d– 5p4(3P1)6p 5p4(3P0)6s– 5p4(3P2)6p 5p4(3P0)6s– 5p4(3P0)6p 5p4(3P0)6s– 5p4(3P1)6p 5p4(3P1)6s– 5p4(3P1)6p

22. 23. 24.

25. 26. 27. 28. 29. 30.

5p4(3P1)6s– 5p4(1D2)6p 5p4(3P1)5d– 5p4(3P1)6p 5p4(3P1)5d– 5p4(3D2)6p 5p4(3P2)5d– 5p4(3P0)6p 5p4(3P2)5d– 5p4(3P1)6p 5p4(3P2)5d– 5p4(1D2)6p 5p4(3P0)5d– 5p4(3P2)4f

31. 32. 33.

5p4(3P1)5d– 5p4(1D2)6p 5p4(1D2)6s– 5p4(1D2)6p

34. 35.

36.

5p4(3P1)5d– 5p4(1D2)6p

37. 38. 39.

40.

5p4(3P2)6p– 5p4(3P2)7s 4 3

5p ( P2)6p– 5p4(1D2)5d

1.15 1.08

et et et et

al. al. al. al.

(2006f) (2006f) (2006f) (2006f)

(continued on next page)

524

A. Lesage / New Astronomy Reviews 52 (2009) 471–535

Table (continued) No.

Configuration

Multiplet

Wavelength ˚) (A

Temperature (K)

Electron density (1017 cm3)

wm ˚) (A

41.

5p4(3P2)6p– 5p4(3P2)6d

½205=2 –½37=2

4245.38

22,000

1.0

½203=2 –½23=2 ½205=2 –½25=2 ½205=2 –½47=2 ½305=2 –½35=2 ½307=2 –½25=2 ½305=2 –½47=2 ½307=2 –½49=2 ½101=2 –½23=2

4180.10 4238.25 4057.46 3907.91 4577.06 4330.52 4462.19 5122.42

22,000 22,000 22,000 22,000 22,000 22,000 22,000 22,000

½101=2 –½11=2

4369.20

½101=2 –½01=2

42. 43. 44. 45. 46. 47. 48. 49. 50. 51. 52. 53. 54. 55. 56. 57. 58.

5p4(3P2)6p– 5p4(3P2)7s 5p4(3P2)6p– 5p4(3P2)6d 5p4(3P2)6p– 5p4(3P2)6d 5p4(3P0)6p– 5p4(3P0)6d 5p4(3P1)6p– 5p4(3P1)6d 5p4(3P1)6p– 5p4(3P1)7s 5p4(3P1)6p– 5p4(3P1)6d

5p4(1D2)5d– 5p4(1D2)4f 5p4(1D2)6p– 5p4(1D2)7s 5p4(1D2)6p– 5p4(1D2)6d

59.

wm/ wtha

dm ˚) (A

dm/ dth

Acc. (%)

Ref.

1.1240

20–30

Djurovic´ et al. (2006f)

1.0 1.0 1.0 1.0 1.0 1.0 1.0 1.0

1.1920 1.0754 1.1028 1.6781 1.1535 1.2594 1.4404 1.5582

20–30 20–30 15–20 15–20 20–30 15–20 15–20 20–30

Djurovic´ Djurovic´ Djurovic´ Djurovic´ Djurovic´ Djurovic´ Djurovic´ Djurovic´

22,000

1.0

1.3047

20–30

Djurovic´ et al. (2006f)

3990.33

22,000

1.0

1.6098

20–30

Djurovic´ et al. (2006f)

½103=2 –½25=2

4393.20

22,000

1.0

1.2134

20–30

Djurovic´ et al. (2006f)

½001=2 –½11=2

4158.04

22,000

1.0

1.2163

15–20

Djurovic´ et al. (2006f)

½205=2 –½13=2

5188.04

22,000

1.0

1.7128

20–30

Djurovic´ et al. (2006f)

½203=2 –½35=2

4223.00

22,000

1.0

1.5779

6–10

Djurovic´ et al. (2006f)

½101=2 –½13=2 ½103=2 –½25=2 ½203=2 –½35=2

4251.57 4540.89 3366.72

22,000 22,000 22,000

1.0 1.0 1.0

1.8184 1.6350 1.2666

20–30 15–20 20–30

Djurovic´ et al. (2006f) Djurovic´ et al. (2006f) Djurovic´ et al. (2006f)

½307=2 –½25=2

5091.93

22,000

1.0

1.8277

15–20

Djurovic´ et al. (2006f)

½307=2 –½49=2

4395.77

22,000

1.0

1.3386

20–30

Djurovic´ et al. (2006f)

½305=2 –½25=2

3972.58

22,000

1.0

1.8472

20–30

Djurovic´ et al. (2006f)

1.13

et et et et et et et et

al. al. al. al. al. al. al. al.

(2006f) (2006f) (2006f) (2006f) (2006f) (2006f) (2006f) (2006f)

Note: For Djurovic´ et al. (2006f) accuracy is as in Djurovic´ et al. (2006f) publication. ´ irisˇan et al. (2007) shift values are presented in a separate table. C a wth is calculated as in Dimitrijevic´ and Konjevic´ (1980) (semi-empirical calculations).

Numerical results for C´irisˇ an et al. (2007) Xe II line shift values No. Configuration Multiplet

1. 2. 3.

5s5p6– 5p4(3P2)6p 6

5s5p – 5p4(3P0)6p

˚) Wavelength Temperature Electron Density wm wm/ dm (A ˚ ) wth ˚) (A (A (K) (1017 cm3)

2

S1=2 –½203=2 4779.18

21,000

1.0

.0667

6–10

´ irisˇan et al. (2007) C

2

S1=2 –½101=2 4384.93 S1=2 –½103=2 3250.56

21,000 21,000

1.0 1.0

.0722 0 < dm < .02

6–10

´ irisˇan et al. (2007) C ´ irisˇan et al. (2007) C

S1=2 –½101=2 3384.13 ½25=2 –½205=2 5292.22

21,000 21,000

1.0 1.0

½25=2 –½305=2 ½23=2 –½305=2 ½23=2 –½103=2 ½23=2 –½101=2 ½25=2 –½103=2

4890.09 5419.15 4603.03 5372.39 3500.36

21,000 21,000 21,000 21,000 21,000

1.0 1.0 1.0 1.0 1.0

.0672 .0705 .0543 .0586 .0216

½23=2 –½103=2 3763.37 ½23=2 –½101=2 3943.57

21,000 21,000

1.0 1.0

2

2

4.

5p4(3P2)6s– 5p4(3P2)6p

5.

7

5p4(3P2)6s– 5p4(3P0)6p

Acc. for Ref. dm/dth dth ´ irisˇan (C dm (%) et al., 2007)

.74

20–30

´ irisˇan et al. (2007) C ´ irisˇan et al. (2007) C

.58 .47 .55 .39 .37

6–10 20–30 20–30 20–30 15–20

´ irisˇan C ´ irisˇan C ´ irisˇan C ´ irisˇan C ´ irisˇan C

.0628 .87 .0796 .97

20–30 15–20

´ irisˇan et al. (2007) C ´ irisˇan et al. (2007) C

jdmj < .015 .104

et et et et et

al. al. al. al. al.

(2007) (2007) (2007) (2007) (2007)

A. Lesage / New Astronomy Reviews 52 (2009) 471–535

525

Table (continued) No. Configuration Multiplet

8.

5p4(3P2)6s– 5p4(3P1)6p

9. 10. 5p4(3P2)5d– 5p4(3P2)6p 11. 12. 5p4(3P2)5d– 5p4(3P0)6p 13. 5p4(3P2)5d– 5p4(3P1)6p 14. 15. 5p4(3P2)5d– 5p4(3P2)6p 16. 5p4(3P2)5d– 5p4(1D2)6p 17. 5p4(3P2)5d– 5p4(3P2)6p 18 5p4(3P2)5d– 5p4(3P1)6p 19. 20. 21. 22. 5p4(3P0)6s– 5p4(3P0)6p 23. 5p4(3P0)6s– 5p4(3P1)6p 24. 25. 5p4(3P0)6s– 5p4(1D2)6p 26. 5p4(3P1)6s– 5p4(3P1)6p 27. 28. 5p4(3P1)6s– 5p4(1D2)6p 29. 5p4(3P1)5d– 5p4(3P1)6p 30. 5p4(3P1)5d– 5p4(3D2)6p 31. 32. 5p4(3P1)5d– 5p4(3P2)4f 33. 34. 5p4(3P2)5d– 5p4(3P1)6p 35. 36. 5p4(3P0)5d– 5p4(1D2)6p 37. 5p4(3P0)5d– 5p4(3P2)4f 38. 39. 5p4(3P1)5d– 5p4(1D2)6p

Wavelength Temperature Electron ˚) (A (K) Density (1017 cm3)

˚) wm wm/ dm (A ˚ ) wth (A

Acc. for Ref. dm/dth dth ´ irisˇan (C dm (%) et al., 2007)

½25=2 –½205=2 3327.46

21,000

1.0

.0430

½23=2 –½205=2 3564.30 ½23=2 –½103=2 3420.73 ½25=2 –½307=2 5460.39

21,000 21,000 21,000

1.0 1.0 1.0

.0430 .0387 .0737

½25=2 –½103=2 4674.56 ½23=2 –½103=2 4818.02 ½25=2 –½103=2 3811.05

21,000 21,000 21,000

1.0 1.0 1.0

.0585 .0795 .015 < dm < 0

½23=2 –½101=2 4100.34 ½23=2 –½001=2 3975.59

21,000 21,000

1.0 1.0

.015 < dm < 0 .015 < dm < 0

½23=2 –½203=2 3672.57 ½37=2 –½307=2 5472.61

21,000 21,000

1.0 1.0

.0307 .0814

20–30 15–20

´ irisˇan et al. (2007) C ´ irisˇan et al. (2007) C

½35=2 –½205=2 3885.00

21,000

1.0

.3066

15–20

´ irisˇan et al. (2007) C

½11=2 –½101=2 5945.53

21,000

1.0

.0478

15–20

´ irisˇan et al. (2007) C

½13=2 –½103=2 5268.31

21,000

1.0

.0324

20–30

´ irisˇan et al. (2007) C

½13=2 –½305=2 ½13=2 –½205=2 ½13=2 –½203=2 ½47=2 –½205=2 ½01=2 –½103=2

4244.41 3717.20 3756.87 3259.36 4883.53

21,000 21,000 2100 21,000 21,000

1.0 1.0 1.0 1.0 1.0

20–30

½01=2 –½101=2 5191.37 ½01=2 –½001=2 4993.03

21,000 21,000

1.0 1.0

½01=2 –½203=2 4524.21 ½01=2 –½103=2 3506.56

21,000 21,000

1.0 1.0

½13=2 –½001=2 5438.96

21,000

1.0

½13=2 –½203=2 4887.30 ½13=2 –½205=2 4921.48 ½13=2 –½103=2 3720.80

21,000 21,000 21,000

1.0 1.0 1.0

.015 < dm < 0 .0475 .0438

½11=2 –½101=2 3869.63 ½11=2 –½203=2 5260.44

21,000 21,000

1.0 1.0

.015 < dm < 0 .1345

½13=2 –½203=2 6512.83 ½13=2 –½101=2 4025.19

21,000 21,000

1.0 1.0

½13=2 –½203=2 4162.16 ½13=2 –½103=2 3082.62

21,000 21,000

½01=2 –½103=2 6375.28 ½01=2 –½203=2 5776.39

.61 .61 6.073

15–20

´ irisˇan et al. (2007) C

20–30 15–20 15–20

´ irisˇan et al. (2007) C ´ irisˇan et al. (2007) C ´ irisˇan et al. (2007) C

20–30 20–30

´ irisˇan et al. (2007) C ´ irisˇan et al. (2007) C ´ irisˇan et al. (2007) C ´ irisˇan et al. (2007) C ´ irisˇan et al. (2007) C

.57

20–30

´ irisˇan C ´ irisˇan C ´ irisˇan C ´ irisˇan C ´ irisˇan C

.0344 .1096

.26 .85

15–20 20–30

´ irisˇan et al. (2007) C ´ irisˇan et al. (2007) C

.015 < dm < 0 .0344

.55

15–20

´ irisˇan et al. (2007) C ´ irisˇan et al. (2007) C

.34

8–15

´ irisˇan et al. (2007) C

.37 .60

15–20 15–20

´ irisˇan et al. (2007) C ´ irisˇan et al. (2007) C ´ irisˇan et al. (2007) C

15–20

´ irisˇan et al. (2007) C ´ irisˇan et al. (2007) C

.1186 .0394

20–30 15–20

´ irisˇan et al. (2007) C ´ irisˇan et al. (2007) C

1.0 1.0

.0712 .1149

15–20 20–30

´ irisˇan et al. (2007) C ´ irisˇan et al. (2007) C

21,000 21,000

1.0 1.0

.0232 .0469

20–30 15–20

´ irisˇan et al. (2007) C ´ irisˇan et al. (2007) C

½01=2 –½101=2 5368.07 ½25=2 –½307=2 4532.49

21,000 21,000

1.0 1.0

.0791 .0278

15–20 15–20

´ irisˇan et al. (2007) C ´ irisˇan et al. (2007) C

½25=2 –½407=2 3121.87

21,000

1.0

.0718

15–20

´ irisˇan et al. (2007) C

½25=2 –½205=2 3104.40 ½23=2 –½203=2 3112.74 ½35=2 –½307=2 6528.65

21,000 21,000 21,000

1.0 1.0 1.0

.0651 .0370 .02389

20–30 20–30 20–30

´ irisˇan et al. (2007) C ´ irisˇan et al. (2007) C ´ irisˇan et al. (2007) C

.0711 .015 < dm < 0 .0333 jdmj < .015 .0635

0535

20–30

et et et et et

al. al. al. al. al.

(2007) (2007) (2007) (2007) (2007)

(continued on next page)

526

A. Lesage / New Astronomy Reviews 52 (2009) 471–535

Table (continued) No. Configuration Multiplet

40. 5p4(1D2)6s– 5p4(1D2)6p

41. 42.

43. 44. 45. 46. 47. 5p4(3P2)6p– 5p4(3P2)7s 48. 5p4(3P2)6p– 5p4(1D2)5d 49. 5p4(3P2)6p– 5p4(2P2)6d 50. 51. 52. 5p4(3P2)6p– 5p4(3P2)7s 53. 54. 55. 56. 5p4(3P2)6p– 5p4(3P2)7s 57. 5p4(3P2)6p– 5p4(3P2)6d 58.

59. 5p4(3P2)6p– 5p4(1S0)5d 60. 5p4(3P2)6p– 5p4(3P2)6d 61. 5p4(1D2)5d– 5p4(3P2)4f 62. 5p4(3P0)6p– 5p4(3P0)6d 63. 5p4(3P0)6p– 5p4(3P1)6d 64. 5p4(3P0)6p– 5p4(3P1)6d 65 5p4(3P1)6p– 5p4(3P1)6d 66. 5p4(3P1)6p– 5p4(3P1)7s 67. 5p4(3P1)6p– 5p4(3P1)7s 68. 5p4(3P1)6p– 5p4(3P1)6d 69. 70. 5p4(1D2)5d– 5p4(1D2)4f

Wavelength Temperature Electron ˚) (A (K) Density (1017 cm3)

˚) wm wm/ dm (A ˚ ) wth (A

Acc. for Ref. dm/dth dth ´ irisˇan (C dm (%) et al., 2007)

½25=2 –½307=2 4876.50

21,000

1.0

1.00 .0362

.33

15–20

´ irisˇan et al. (2007) C

½25=2 –½305=2 ½23=2 –½305=2 ½25=2 –½103=2 ½25=2 –½205=2 ½25=2 –½203=2 ½23=2 –½205=2 ½23=2 –½205=2 ½23=2 –½101=2 ½23=2 –½205=2 ½23=2 –½103=2 ½203=2 –½25=2

5178.82 6270.82 4972.71 4414.84 4470.90 5184.48 3663.93 4668.49 3461.26 3446.34 4823.35

21,000 21,000 21,000 21,000 21,000 21,000 21,000 21,000 21,000

1.0 1.0 1.0 1.0 1.0 1.0 1.0 1.0 1.0

1.08 .92 1.10 1.13

.35 .43

6–10 15–20 15–20 20–30 15–20 15–20 20–30 15–20 20–30

21,000

1.0

.0467 .0949 .0539 .0192 .0298 .99 .0234 .00887 .0288 .0628 .015 < dm < 0 1.15 .626

1.55

15–20

´ irisˇan C ´ irisˇan C ´ irisˇan C ´ irisˇan C ´ irisˇan C ´ irisˇan C ´ irisˇan C ´ irisˇan C ´ irisˇan C ´ irisˇan C ´ irisˇan C

½205=2 –½25=2 4862.45 ½203=2 –½01=2 4296.4

21,000 21,000

1.0 1.0

1.08

.6275 .1891

1.58

15–20 8–15

´ irisˇan et al. (2007) C ´ irisˇan et al. (2007) C

½205=2 –½37=2 4245.38

21,000

1.0

.3961

3.83

20–30

´ irisˇan et al. (2007) C

½203=2 –½23=2 [2]5/2–[2]5/2 [2]5/2–[4]7/2 ½305=2 –½23=2

4180.10 4238.25 4057.46 5080.62

21,000 21,000 21,000 21,000

1.0 1.0 1.0 1.0

.4691 .4211 .4996 .7221

4.73 4.70 7.854 1.49

20–30 20–30 15–20 8–15

´ irisˇan C ´ irisˇan C ´ irisˇan C ´ irisˇan C

et et et et

al. al. al. al.

(2007) (2007) (2007) (2007)

½305=2 –½35=2 [3]7/2–[2]5/2 ½305=2 –½47=2 ½101=2 –½23=2

3907.91 4577.06 4330.52 5122.42

21,000 21,000 21,000 21,000

1.0 1.0 1.0 1.0

.6253 .5331 .4497 .6682

5.12 5.50 .0932 1.36

8–15 8–15 20–30 15–20

´ irisˇan C ´ irisˇan C ´ irisˇan C ´ irisˇan C

et et et et

al. al. al. al.

(2007) (2007) (2007) (2007)

½103=2 –½35=2 4480.86

21,000

1.0

.9138

6.05

15–20

´ irisˇan et al. (2007) C

½101=2 –½13=2 ½101=2 –½11=2 ½103=2 –½23=2 ½101=2 –½23=2

3849.87 4369.20 4373.78 4098.89

21,000 21,000 21,000 21,000

1.0 1.0 1.0 1.0

.3737 .4480 .5163 .2673

3.21 4.29 3.67

15–20 15–20 15–20 15–20

´ irisˇan C ´ irisˇan C ´ irisˇan C ´ irisˇan C

½103=2 –½23=2 4698.01 ½101=2 –½01=2 3990.33

21,000 21,000

1.0 1.0

.3810 .4606

15—20 15–20

´ irisˇan et al. (2007) C ´ irisˇan et al. (2007) C

½35=2 –½407=2 4773.19

21,000

1.0

.1511

20–30

´ irisˇan et al. (2007) C

½103=2 –½25=2 4393.20

21,000

1.0

.4994

4.31

15–20

´ irisˇan et al. (2007) C

½103=2 –½23=2 4440.95 ½103=2 –½23=2 4112.14

21,000 21,000

1.0 1.0

.5031 .5685

4.36 5.95

20–30 20–30

´ irisˇan et al. (2007) C ´ irisˇan et al. (2007) C

4715.18

21,000

1.0

.5303

4.11

15–20

´ irisˇan et al. (2007) C

½001=2 –½11=2 4158.04

21,000

1.0

.5722

5.86

8–15

´ irisˇan et al. (2007) C

½001=2 –½11=2 5670.91

21,000

1.0

.7597

4.24

20–30

´ irisˇan et al. (2007) C

½205=2 –½13=2 5188.04

21,000

1.0

.7499

4.80

20–30

´ irisˇan et al. (2007) C

½203=2 –½35=2 4223.00

21,000

1.0

.5465

4.51

15–20

´ irisˇan et al. (2007) C

½205=2 –½37=2 ½205=2 –½25=2 ½203=2 –½23=2 ½13=2 –½203=2

21,000 21,000 21,000 21,000

1.0 1.0 1.0 1.0

.4960 .4207 .6974 .0929

4.03 3.54 6.14

15–20 15–20 15–20 20–30

´ irisˇan C ´ irisˇan C ´ irisˇan C ´ irisˇan C

4448.13 4310.51 4006.88 3101.51

4.08

et et et et et et et et et et et

et et et et

et et et et

al. al. al. al. al. al. al. al. al. al. al.

al. al. al. al.

al. al. al. al.

(2007) (2007) (2007) (2007) (2007) (2007) (2007) (2007) (2007) (2007) (2007)

(2007) (2007) (2007) (2007)

(2007) (2007) (2007) (2007)

A. Lesage / New Astronomy Reviews 52 (2009) 471–535

527

Table (continued) ˚ ) dm/dth dth wm/ dm (A Acc. for Ref. ´ irisˇan (C dm (%) wth et al., 2007)

Multiplet

71. 5p4(3P1)6p– 5p4(3P1)7s

½103=2 –½11=2 5363.20

21,000

1.0

.5151 3.26

20–30

´ irisˇan et al. (2007) C

½101=2 –½11=2 ½101=2 –½13=2 ½103=2 –½25=2 ½25=2 –½307=2

5445.45 4251.57 4540.89 3938.92

21,000 21,000 21,000 21,000

1.0 1.0 1.0 1.0

.8309 5.13 .6081 4.69 .5134 4.13 .1053

20–30 15–20 20–30 20–30

´ irisˇan C ´ irisˇan C ´ irisˇan C ´ irisˇan C

½23=2 –½305=2 3366.72

21,000

1.0

15–20

´ irisˇan et al. (2007) C

½307=2 –½25=2 5091.93

21,000

1.0

.8837 6.44

15–20

´ irisˇan et al. (2007) C

½307=2 –½49=2 4395.77

21,000

1.0

.5557 5.02

20–30

´ irisˇan et al. (2007) C

½305=2 –½25=2 3972.58 ½103=2 –½25=2 4991.17

21,000 21,000

1.0 1.0

.5991 5.90 .9091 6.33

15–20 20–30

´ irisˇan et al. (2007) C ´ irisˇan et al. (2007) C

½101=2 –½23=2 4571.85

21,000

1.0

20–30

´ irisˇan et al. (2007) C

½205=2 –½35=2 4676.46 ½203=2 –½25=2 4521.86

21,000 21,000

1.0 1.0

15–20 20–30

´ irisˇan et al. (2007) C ´ irisˇan et al. (2007) C ´ irisˇan et al. (2007) C

72. 73. 74 5p4(1D12)5d– 5p4(3P1)4f 75. 5p4(1D2)5d– 5p4(1D2)4f 76. 5p4(1D2)6p– 5p4(1D2)7s 77. 5p4(1D2)6p– 5p4(1D2)6d 78. 79. 5p4(1D2)6p– 5p4(1D2)7s 80. 5p4(1D2)6p– 5p4(1D2)6d 81. 82.

Wavelength Temperature Electron Density ˚) (A (K) (1017 cm3)

wm ˚) (A

No. Configuration

.0694

.0860 .7276 5.65 .7039 5.53

et et et et

al. al. al. al.

(2007) (2007) (2007) (2007)

´ irisˇan et al. (2007) accuracy is as in C ´ irisˇan et al. (2007)publication.dth is calculated as in Dimitrijevic´ and Krsˇljanin (1986) (modified semiNote: For C empirical calculations).

Xenon, Xe III Ground state: 1s22s22p63s23p63d104s24p64d105s25p43P2. Ionization energy: 31.046 eV = 250,400 cm1. Seidel et al. (2001) measured two lines of a Xe III quintet transition (4S0)6s5S0–(4S0)6p5P with a gas-liner pinch. Doppler broadening is negligible for the experimental range of electron density and temperature. The Stark width is obtained through a fit of a Lorentzian profile convoluted with the apparatus profile. The optical thinness of the plasma was checked, for the lines under investigation, by comparison of the experimental intensity ratio to the theoretical one. The agreement was within the error bars. Comparisons with previous experimental data (Konjevic´ and Pittman, 1987; Iriarte et al., 1997) show very good agreement, when the variation of the Stark parameter versus the temperature is correctly taken in account. Theoretical calculations by Iriarte et al. (1997), according to Griem (1968b) semi-empirical formula underestimate the width by a factor of 1.7, while those of Konjevic´ and Pittman (1987) underestimate it by a factor of 1.5. Pelaez et al. (2006b), measured 38 Xe III line widths in a pulsed (300 ls long, 20 lF, 9000 V) capacitor discharge plasma source. A 175 mm long and 19 mm internal diameter Pyrex glass tube was continuously flowed with helium at 3 kPa. Approximately 5% of xenon was added to the carrier gas and the flow was adjusted to obtain minimal self-absorption and maximal intensity of the lines. Spectroscopic observation and interferometric measurement were performed along the tube axis and symmetrically to the axis. The spectra was time resolved and recorded with a monochromator and a optical multichannel analyser. Profiles were recorded with and without a mirror positioned behind the discharge tube in order to check possible self-absorption, found as negligible for all measured lines. The Davies and Vaughan (1963) procedure was used to obtain the Stark width from the experimental profile. van der Waals, ionic and resonance broadening were negligibly small for the experimental conditions. Pelaez et al. (2006b) have attributed an estimated accuracy to each of their Stark half-widths measurement. As such estimates are largely justified by their description of the experimental set-up, plasma diagnostic and spectral treatments, they are kept, for that reference, in the table of the numerical results. Pelaez et al. (2006b) results measured with 6–10% and 10–15% accuracy are in very good agreement with those of Konjevic´ ˚ line where a 20% disagreement exist. The two widths measured by Seidel and Pittman (1987) except for the k 3624.06 A et al. (2001) at much higher temperature (58,000 K) are in agreement with those of Pelaez et al. (2006b) when the electron density trend is taken in account. A large discrepancy with the Iriarte et al. (1997) data seems to be a function of the line intensity (larger disagreement for higher intensity) and related to self-absorption. Iriarte et al. (1997) and Romeo y Bidegain et al. (1998) performed their experiments in a pure xenon plasma and even if it is under low pressure, it cannot be a guarantee of optical thinness for all spectral lines. A similar situation occurs with Romeo y Bidegain et al. (1998) experiment. Pelaez et al. (2006b) half-widths values are in very good agreement with Dimitrijevic´ and Konjevic´ (1980) predic˚ lines, measured with a lower accuracy. tions, except for the k 3583.65 and 3877.82 A

528

A. Lesage / New Astronomy Reviews 52 (2009) 471–535

´ irisˇan et al. (2007) measured the line shifts of 42 Xe III lines with the same experimental set up and methods as for the C widths (Pelaez et al., 2006b). Measured values are compared with the values measured by Di Rocco et al. (1989). The agreement is good for the multiplets 2, 9–11and 27, but for the 6, 8, 12, 15–17 and 26 there is a difference in the shift sign. For other lines, the line shift ratio ðd Di Rocco =d cirisan Þ is between 1.7 and 7.4. Comparison with modified semi-empirical calculated values Dimitrijevic´ and Krsˇljanin (1986) using the LS-coupling is done for the 6s–6p transitions. Experimental and calculated shift values agree in shift sign in all cases. The dm/dth ratio ranges from 0.4 to 1.24.

Key data on experiments Ref.

Plasma source

Seidel et al. (2001) ´ irisˇan et al. Pelaez et al. (2006b), C (2007)

Gas-liner pinch Pulsed discharge

Method of measurement

Remarks

Electron density

Temperature

Thomson scattering diagnostic Two wavelengths Twyman–Green interferometer

Thomson scattering diagnostic Boltzmann plot of 24 Xe II lines

Numerical results for Xe III width values Transition array

Multiplet

Wavelength ˚) (A

1.

5d–6p

3

2.

6s–6p

5 0 5

3236.84 3242.86 3522.80 3624.06

22,000 22,000 22,000 22,000

1.0 1.0 1.0 1.0

0.176 0.1665 0.2241 0.1920

3922.55

60000(5eV) 22,000

10 1.0

2.6 0.2684

60000(5eV) 22,000 22,000 22,000 22,000 22,000 22,000 22,000 22,000 22,000 22,000 22,000 22,000 22,000 22,000 22,000 22,000 22,000 22,000 22,000 22,000 22,000 22,000 22,000 22,000 22,000 22,000 22,000 22,000 22,000 22,000 22,000 22,000 22,000

10 1.0 1.0 1.0 1.0 1.0 1.0 1.0 1.0 1.0 1.0 1.0 1.0 1.0 1.0 1.0 1.0 1.0 1.0 1.0 1.0 1.0 1.0 1.0 1.0 1.0 1.0 1.0 1.0 1.0 1.0 1.0 1.0 1.0

2.6 0.2621 0.1816 0.2085 0.2586 0.4423 0.4220 0.2844 0.2756 0.3172 0.3884 0.2056 0.2183 0.2989 0.2717 0.3084 0.3392 0.2145 0.2255 0.3507 0.2246 0.2479 0.2288 0.2546 0.2149 0.2733 0.2283 0.2223 0.2307 0.2591 0.3278 0.2413 0.3221 0.2694

D0–3P

S–P

3950.59 3.

6s–6p

5 0 3

4. 5.

5d–6p 6s–6p

3 0 3

6.

6s–6p

3 0 3

7. 8. 9.

5d–6p 5d–6p

3

10.

6s–6p

3

D0–3D

11.

6s–6p

3

D0–3F

12.

6s–6p

3

D0–1F

13. 14. 15. 16. 17. 18. 19. 20. 21. 22. 23. 24.

6s–6p 6s–6p 6s–4f 5d–6p 5d–6p 5d–6p 5d–6p 6s–6p 6s–4f 6s–6p 5d–6p 6s–6p

3

S–P F–P S–P

3 0 5

S–P

D0–3P D0–3D 3 0 3 D–F 3

D0–1P D0–3P 3 0 5 D–F 1 0 3 D–D 1 0 1 D–F 1 0 1 D–F 3 0 3 P–S 1 0 3 D–P 1 0 5 D–F 1 0 1 D–D 3 0 1 F–D 3 0 3 P–D 3

3268.98 3468.22 3854.28 4683.55 4723.60 3676.63 3781.00 4050.07 5107.33 3444.24 3640.99 4272.58 4109.08 4145.74 4794.49 3579.70 3583.65 4434.17 3357.99 3877.82 3349.76 3596.59 3542.35 3861.04 3561.37 3552.12 3150.69 3992.85 4285.89 3454.27 3745.71 3776.32

Temperature (K)

Electron density (1017 cm3)

wm ˚) (A

No.

Note: For Pelaez et al. (2006b) accuracy is as in Pela´ez et al. (2006a) publication. ´ irisˇan et al. (2007) shift values are presented in a separate table. C

wm/ wth

dm/ dth

Acc. (%)

Ref.

0.76

15–20 10–15 15–20 15–20

0.95

A 15–20

Pelaez et al. (2006b) Pelaez et al. (2006b) Pelaez et al. (2006b) (Konjevic´ and Wiese, 1990) Seidel et al. (2001) (Konjevic´ and Wiese, 1990) Seidel et al. (2001) Pelaez et al. (2006b) Pelaez et al. (2006b) Pelaez et al. (2006b) Pelaez et al. (2006b) Pelaez et al. (2006b) Pelaez et al. (2006b) Pelaez et al. (2006b) Pelaez et al. (2006b) Pelaez et al. (2006b) Pelaez et al. (2006b) Pelaez et al. (2006b) Pelaez et al. (2006b) Pelaez et al. (2006b) Pelaez et al. (2006b) Pelaez et al. (2006b) Pelaez et al. (2006b) Pelaez et al. (2006b) Pelaez et al. (2006b) Pelaez et al. (2006b) Pelaez et al. (2006b) Pelaez et al. (2006b) Pelaez et al. (2006b) Pelaez et al. (2006b) Pelaez et al. (2006b) Pelaez et al. (2006b) Pelaez et al. (2006b) Pelaez et al. (2006b) Pelaez et al. (2006b) Pelaez et al. (2006b) Pelaez et al. (2006b) Pelaez et al. (2006b) Pelaez et al. (2006b) Pelaez et al. (2006b)

0.90 0.88 0.91 1.05 0.99 1.07 0.97 0.99

0.89 0.89 0.77 0.87 0.83 0.91 1.00 0.80 1.03 0.95

0.73 0.94 0.96

dm ˚) (A

A 10–15 10–15 15–20 15–20 10–15 10–15 6–10 6–10 6–10 15–20 15–20 15–20 15–20 15–20 10–15 15–20 10–15 10–15 10–15 10–15 10–15 15–20 10–15 10–15 15–20 15–20 10–15 10–15 15–20 6–10 10–15 10–15 10–15

A. Lesage / New Astronomy Reviews 52 (2009) 471–535

529

Numerical results for Xe III C´irisˇ an et al. (2007) shift values No. Transition array

4 0

S 5d–4S06p

˚) wm wm/ dm(A Multiplet Wavelength Temperature Electron ˚ ) wth ˚) (A (A (K) density (1017 cm3) D01 –3 P0 D03 –3 P2 3 0 3 D1 – P1 5S02 –5 P3 5S02 –5 P2 5S02 –5 P1 5 0 3 S – P2 5 0 3 S – P1 3 0 3 F4 – F3 3 0 5 S1 – P2 3S01 –5 P1 3S01 –3 P0 3S01 –3 P2 3 0 3 S – P1 3D01 –3 D2 3D01 –3 F2 3D02 –3 D1 3 0 3 D2 – F3 3 0 3 D3 – F4 3 0 1 D2 – F3 3 0 1 D3 – F3 3 0 1 D2 – P1 3 0 1 D1 – P1 3 0 5 D2 – F3 3 0 5 D3 – F2 3 0 5 D3 – F3 3 0 5 D3 – F4 1 0 3 D2 – D2 1 0 3 D2 – F2 1 0 1 D2 – F3 1 0 1 D2 – P1 1 0 5 D2 – F3 3 0 3 P1 – P1 3 0 3 P2 – S1 1 0 5 D2 – F3 1 D02 –1 D2 3

21,000 21,000 21,000 21,000 2. (4S06s–4S06p) 21,000 21,000 21,000 3. 22,000 21,000 4. (2D0)5d–(2D0)6p 21,000 5. (4S0)6s–(4S0)6p 21,000 21,000 6. 21,000 21,000 21,000 7. (2D0)5d–(2D0)6p 21,000 8. 21,000 9. (2D0)6s–(2D0)6p 21,000 10. 21,000 21,000 11. 6s–6p 21,000 21,000 12. 21,000 21,000 13. (2D0)6s–(4S0)4f 21,000 21,000 21,000 21,000 14. (2P0)5d–(2D0)6p 21,000 15. 21,000 16. 21,000 17. 21,000 18. (2P0)5d–(4S0)4f 21,000 19. (2P0)5d–(2D0)6p 21,000 20. (2P0)5d–(2P0)6p 21,000 21. (2D0)6s–(4S0)4f 21,000 22. (2D0)6s–(2D0)6p ´ ´ irisˇan et al. Note: For Cirisˇan et al. (2007) accuracy is as in C Krsˇljanin, 1986) (modified semi-empirical calculations). 1.

3

3236.84 3242.86 3522.80 3624.06 3922.55 3950.59 3268.98 3468.22 3083.53 4683.55 4723.60 3676.63 3781.00 4050.07 3444.24 3640.99 4109.08 3579.70 3583.65 3357.99 3877.82 3349.76 3791.67 3153.00 3542.35 3607.02 3609.46 3861.04 4110.05 3561.37 3552.12 3331.65 3654.61 3150.69 4285.89 3454.27

1.0 1.0 1.0 1.0 10 10 1.0 1.0 1.0 1.0 1.0 1.0 1.0 1.0 1.0 1.0 1.0 1.0 1.0 1.0 1.0

1.0

1.0 1.0 1.0 1.0 1.0 1.0 1.0

Acc. for Ref. dm/dthdth (Dimitrijevic´ and dm Krsˇljanin (1986))

jdmj < .015 jdmj < .015 jdmj < .015 .0651 .0579 .0858 .0228 .0241 .0159 0543 0761 .0508 .0559 .0635 jDmj < .015 .0319 .0698 .0469 0637 .0593 .0535 .0674 0590 .0313 .0511 .0928 .0820 jdmj<.015 .0824 .0347 .0245 jdmj < .015 +.0308 +.0181 .0719 jdmj < .015

1.03 .75 1.09 .42 .38

15–20% 8–15% 15–20% 20–30% 15–20% 20–30% 20–30% 15–20% 15–20% 20–30% 15–20%

.47 .65 .70 .74 .71

20–30% 20–30% 20–30% 15–20% 15–20% 20–30% 20–30% 20–30% 20–30% 8–15% 20–30% 15–20%

.77 1.04 1.11 .68 1.24 .77

15–20% 20–30% 20–30% 20–30% 20–30% 20–30%

´ irisˇan C ´ irisˇan C ´ irisˇan C ´ irisˇan C ´ irisˇan C ´ irisˇan C ´ irisˇan C ´ irisˇan C ´ irisˇan C ´ irisˇan C ´ irisˇan C ´ irisˇan C ´ irisˇan C ´ irisˇan C ´ irisˇan C ´ irisˇan C ´ irisˇan C ´ irisˇan C ´ irisˇan C ´ irisˇan C ´ irisˇan C ´ irisˇan C ´ irisˇan C ´ irisˇan C ´ irisˇan C ´ irisˇan C ´ irisˇan C ´ irisˇan C ´ irisˇan C ´ irisˇan C ´ irisˇan C ´ irisˇan C ´ irisˇan C ´ irisˇan C ´ irisˇan C ´ irisˇan C

et et et et et et et et et et et et et et et et et et et et et et et et et et et et et et et et et et et et

al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al. al.

(2007) (2007) (2007) (2007) (2007) (2007) (2007) (2007) (2007) (2007) (2007) (2007) (2007) (2007) (2007) (2007) (2007) (2007) (2007) (2007) (2007) (2007) (2007) (2007) (2007) (2007) (2007) (2007) (2007) (2007) (2007) (2007) (2007) (2007) (2007) (2007)

(2007) publication and dth is calculated as in Dimitrijevic´ and Krsˇljanin (Dimitrijevic´ and

Note added in proof: neon, Ne II, and nitrogen, N II, data After completion of this Review, numerical results for Ne II, and a section on N II were added. Neon, Ne II Numerical results added for Ne II (Nos. 24 and 26) No. Transition Multiplet Wavelength ˚) array (A

Temperature (K)

Electron density (1017 cm3)

˚ ) wm/ wm (A wth

24.

34,500

1.83

1.854

35,300 35,300 31,000

1.83 1.83 0.95

0.931

34,500

1.83

1.702

35,300

1.83

26.

2 0 4

P 2D F4G0

3336.12 4290.40

4413.20

˚ ) dm/ dm(A dth

0.013 .033

.149

Acc. Ref. Milosavljevic´ et al. (2001) Djenizˇe et al. (2002a) Djenizˇe et al. (2002a) Milosavljevic´ et al. (2001) Milosavljevic´ et al. (2001) Djenizˇe et al. (2002a)

530

A. Lesage / New Astronomy Reviews 52 (2009) 471–535

Nitrogen, N II Ground State: 1s22s22p2 3P0 Ionization Energy: 29.601 eV = 238 750.5 cm1 Ivkovic´ et al. (2005) measured Stark widths of N II lines in a capillary discharge plasma with inner diameter 3 mm and aluminum electrode (with 3 mm diameter holes) 200 mm apart. Observations are done end-on and line profiles recorded on a step by step procedure. Averaging of eight signals at each wavelength step is performed. The filling gas, at initial pressure of 4 mbar is a mixture of 1.5% N2 + 1.5% CO2 in 97% He. To check the optical thinness of the plasma, the authors compared the line intensity ratios within the studied multiplets with their theoretical predictions. The measured ratio at the time of observation (4.1) is close to the calculated one (4.14). A computerized procedure is used to fit the experimental profiles to Voigt profiles, Davies and Vaughan, 1963. Measured values are in good agreement with semi-classical, Sahal-Bre´chot (1969a,b) and Dimitrijevic´ (1996), and modified semi-empirical, Dimitrijevic´ and N. Konjevic´ (1980), calculated ones. For the N II 3s3P0 - 3p3D multiplet Ivkovic´ et al., 2005 values are in perfect agreement with those of Djenizˇe et al. (1992b) and within error bar with others, even if unexpectedly those of Purcell and Barnard (1984) and Milosavljevic´ and Djenizˇe, 1998 show a large spread of widths within multiplet. For the N II 3p3D - 3d3F0 multiplet, Ivkovic´ et al. (2005) values compare well with Glenzer et al. (1994) and Mar et al. (2000) measured ones even if those of Glenzer et al. (1994) are done at much lower temperature. Key data on experiments Ref.

Plasma source

Method of measurement Electron density

Remarks Temperature

Ivkovic´ et al. Low- pressure capillary discharge Stark width of the He II Pb line at ˚ 3202 A (2005)

Boltzmann plot of N II lines: 3995, 4447, 4630, ˚ 4803 A

Numerical results for N II No. 1.

2.

Transition array

Multiplet

Wavelength ˚) (A

Temperature (K)

Electron density (1017 cm3)

wm ˚) (A

3 0 3

5679.56

30300

0.86

5666.63

30300

5676.02

P–D

3

D–3F0

wm/ wth

˚) dm(A

dm/ dth

Acc.

Ref.

0.334

B+

0.86

0.333

B+

30300

0.86

0.336

B+

5686.21

30300

0.86

0.335

B+

5710

30300

0.86

0.348

B+

5005.15

30300

0.86

0.280

B+

5001.47

30300

0.86

0.285

B+

5001.13

30300

0.86

0.26

B+

5016.38

30300

0.86

0.290

B+

5025.66

30300

0.86

0.303

B+

Ivkovic´ (2005) Ivkovic´ (2005) Ivkovic´ (2005) Ivkovic´ (2005) Ivkovic´ (2005) Ivkovic´ (2005) Ivkovic´ (2005) Ivkovic´ (2005) Ivkovic´ (2005) Ivkovic´ (2005)

et al. et al. et al. et al. et al. et al. et al. et al. et al. et al.

Acknowledgements The author gratefully acknowledges the valuable assistance of Jeff Fuhr from NIST in the process of data collection and of correction of the manuscript, especially for the spectral classification and of Milan Dimitrijevic´ from the Observatory of Belgrade for his suggestions concerning the comparisons with theories. The present publication was made possible thanks to the research fellow position granted to the author by the Scientific Council of the Observatory of Paris.

A. Lesage / New Astronomy Reviews 52 (2009) 471–535

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