Emission‐Line Spectra of S<scp>vii</scp>–S<scp>xiv</scp>in the 20–75 A Wavelength Region

Lepson, J. K.; Beiersdörfer, P.; Behar, E.; Kahn, S. M.

doi:10.1086/429879

Cited by 46 publications

(46 citation statements)

References 24 publications

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“…calculated the complete S xiii dataset adopted in the present CHIANTI 6. They collected the experimental energy levels from Edlén (1983Edlén ( , 1985, Fawcett & Hayes (1987), Goldsmith et al (1974), Lepson et al (2005), Fawcett et al (1970), Khardi et al (1994) and Version 3 of the NIST database (Ralchenko et al 2007) that we use here.…”

Section: Si XImentioning

confidence: 99%

CHIANTI – an atomic database for emission lines

Dere¹,

Landi²,

Young³

et al. 2009

A&A

460

451

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Aims. The goal of the CHIANTI atomic database is to provide a set of atomic data for the interpretation of astrophysical spectra emitted by collisionally dominated, high temperature, optically thin sources. Methods. A complete set of ground level ionization and recombination rate coefficients has been assembled for all atoms and ions of the elements of H through Zn and inserted into the latest version of the CHIANTI database, CHIANTI 6. Ionization rate coefficients are taken from the recent work of Dere (2007, A&A, 466, 771) and recombination rates from a variety of sources in the literature. These new rate coefficients have allowed the calculation of a new set of ionization equilibria and radiative loss rate coefficients.For some ions, such as Fe viii and Fe ix, there are significant differences from previous calculations. In addition, existing atomic parameters have been revised and new atomic parameters inserted into the database. Results. For each ion in the CHIANTI database, elemental abundances, ionization potentials, atomic energy levels, radiative rates, electron and proton collisional rate coefficients, ionization and recombination rate coefficients, and collisional ionization equilibrium populations are provided. In addition, parameters for the calculation of the continuum due to bremsstrahlung, radiative recombination and two-photon decay are provided. A suite of programs written in the Interactive Data Language (IDL) are available to calculate line and continuum emissivities and other properties. All data and programs are freely available at http://wwwsolar.nrl.navy.mil/ chianti

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Section: Si XImentioning

confidence: 99%

CHIANTI – an atomic database for emission lines

Dere¹,

Landi²,

Young³

et al. 2009

A&A

460

451

View full text Add to dashboard Cite

show abstract

“…3,4 For laboratory astrophysics surveys, the high-resolution EUV measurements help to discover a number of coronal lines which are not yet identified in the current databases. 5,6 In addition, the intensity ratios of iron lines are good candidates to determine the plasma density or even the magnetic field strength in the solar corona. 7,8 For the extensive utilization in plasma diagnostics, a portable high-resolution extreme ultraviolet spectrometer has been designed and developed at Shanghai electron beam ions trap (EBIT) laboratory 9 Much work has been done using EUV spectrometer at EBIT devices for identification of new lines and plasma diagnostics.…”

Section: Introductionmentioning

confidence: 99%

“…7,8 For the extensive utilization in plasma diagnostics, a portable high-resolution extreme ultraviolet spectrometer has been designed and developed at Shanghai electron beam ions trap (EBIT) laboratory 9 Much work has been done using EUV spectrometer at EBIT devices for identification of new lines and plasma diagnostics. [5][6][7][8][10][11][12][13] The line intensity ratios of Fe xiv 264.8 Å/274.2 Å, 219.1 Å/211.3 Å and 270.5 Å/274.2 Å and Fe xv 233.9 Å/243.8 Å were studied in Ref. 11.…”

Section: Introductionmentioning

confidence: 99%

Responsivity calibration of the extreme ultraviolet spectrometer in the range of 175-435 Å

et al. 2017

AIP Advances

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We reported the relative responsivity calibration of the grazing-incidence flat-field EUV spectrometer between 175 and 435 Å by means of two methods. The first method is implemented by measuring the diffraction efficiency of the grating with synchrotron radiation light source. Considering the transmission efficiency and quantum efficiency of the other optical components in the spectrometer, the total responsivity was then obtained. The second one was carried out by measuring line emissions from C3+, N4+ and O3+ ions at Shanghai high temperature super conductor electron beam ion trap (SH-HtscEBIT). The EUV spectra were also simulated theoretically via a collisional radiative model. In the calculation, the second-order relativistic many-body perturbation theory approach based on the flexible atomic code was used to calculate the energy levels and transition rates; the close-coupling R-matrix approach and relativistic distorted wave method were utilized to calculate the collision strength of electron impact excitation. In comparison with the spectroscopic measurements at EBIT device, the differences between the measured and simulated relative line intensities were obtained. The responsivity calibration for the spectrometer was then achieved by a 3rd degree polynomial function fitting. Our measurement shows that the responsivity between 175 and 435 Å varies by factor of ∼ 46. The two results of calibration demonstrated a consistency within an average deviation of 24%. In addition, an evaluation of our calculations on C iv, N v and O iv line emissions in this wavelength region was given.

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“…This paper presents our work for Be-like ions with a nuclear charge number Z = 10-30. Many lines of these ions have been observed in both astrophysical and laboratory plasmas (Kelly 1987;Kaufman & Martin 1991;Brown et al 1998Brown et al , 2002Brown et al , 2008Shirai et al 2000;Landi et al 2002;Lepson et al 2003Lepson et al , 2005Curdt et al 2004;Werner et al 2004;Landi & Phillips 2005;Kramida & Buchet-Poulizac 2006;Brosius et al 2008;Del Zanna 2008;Sansonetti 2008;Chen et al 2007;Gu et al 2007Gu et al , 2011Del Zanna & Woods 2013).…”

Section: Introductionmentioning

confidence: 99%

SYSTEMATIC CALCULATIONS OF ENERGY LEVELS AND TRANSITION RATES OF BE-LIKE IONS WITH Z = 10–30 USING A COMBINED CONFIGURATION INTERACTION AND MANY-BODY PERTURBATION THEORY APPROACH

Wang

Guo

Liu

et al. 2015

ApJS

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We report calculations of energy levels and radiative rates for transitions among the lowest 116 fine-structure levels arising from the ⩽ n 5 configurations in Be-like ions with Z = 10-30. The wavelengths, oscillator strengths, line strengths, and radiative rates for all possible electric dipole, magnetic dipole, electric quadrupole, and magnetic quadrupole transitions among the 116 levels have been calculated using the combined configuration interaction and many-body perturbation method. The accuracy of the results is determined through extensive comparisons with existing laboratory measurements and theoretical results. The present complete set of results should be of great help in line identification and the interpretation of spectra, as well as in the modeling and diagnostics of astrophysical and fusion plasmas.

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Emission‐Line Spectra of Svii–Sxivin the 20–75 A Wavelength Region

Cited by 46 publications

References 24 publications

CHIANTI – an atomic database for emission lines

CHIANTI – an atomic database for emission lines

Responsivity calibration of the extreme ultraviolet spectrometer in the range of 175-435 Å

SYSTEMATIC CALCULATIONS OF ENERGY LEVELS AND TRANSITION RATES OF BE-LIKE IONS WITH Z = 10–30 USING A COMBINED CONFIGURATION INTERACTION AND MANY-BODY PERTURBATION THEORY APPROACH

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