Intercombination lines in delayed beam-foil spectra

Träbert, E.; Heckmann, P. H.; Hutton, R.; Martinson, I.

doi:10.1364/josab.5.002173

Cited by 115 publications

(77 citation statements)

References 65 publications

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“…The experimental values of the radiative decay rates for the 3s 2 1 S 0 -3s3p 3 P 1 from Träbert et al (1988) replaces the theoretical values available in CHIANTI 5.2. The new value for Fe XV is less than 5% different from the value in CHIANTI 5.2, but for Ni XVII the new value is 3.5 times larger.…”

Section: Fe XV Ni Xviimentioning

confidence: 99%

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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: Fe XV Ni Xviimentioning

confidence: 99%

“…The A-values for the 3s 2 3p 2 P 3/2 -3s3p 2 4 P 5/2 transitions of these two ions have been replaced with the experimental values measured by Träbert et al (1988). The differences from the values in CHIANTI 5.2 are less than 5% for Fe xiv and a factor 1.5 for Ni xvi.…”

Section: New Atomic Data For the Aluminum Isoelectronic Sequencementioning

confidence: 99%

CHIANTI – an atomic database for emission lines

Dere¹,

Landi²,

Young³

et al. 2009

A&A

460

451

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“…A portion is shown here for guidance regarding its form and content.) For some higher excited levels, such as 3s3p 24 P 1/2,5/2 and 3s3p3d 4 F o 3/2,5/2,7/2 , experimental data for the lifetimes are available in the works of Träbert et al (1988Träbert et al ( , 1993. A comparison of the lifetimes for the 3s3p 24 P 1/2,5/2 levels indicates that the present AS results are similar to the previous calcula- level, all theories are higher than the measurement by at least 60%.…”

Section: Oscillator Strengths and Lifetimesmentioning

confidence: 99%

R -MATRIX ELECTRON-IMPACT EXCITATION OF Fe ¹³⁺ AND ITS APPLICATION TO THE SOFT X-RAY AND EXTREME-ULTRAVIOLET SPECTROSCOPY OF CORONA-LIKE PLASMAS

Liang¹,

Badnell²,

López‐Urrutia³

et al. 2010

ApJS

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Accurate excitation parameters are required to interpret the ultraviolet and X-ray spectra of Fe 13+ . In this work, we use the autostructure code to describe the atomic structure of Fe 13+ . The 197 lowest-lying fine-structure levels of the 3sx 3p y 3d z (x + y + z = 3), 3s 2 4l, and 3s3p4{s, p, and d} configurations are included along with further correlation configurations: 3s3p4f , 3px 3d y 4l (x + y = 2), 3l4l 4l , and 3l3l 5l . The resultant level energies, lifetimes of excited states, and oscillator strengths of transitions between these levels are assessed by comparison with available experimental data and previous calculations. Electron-impact excitation data among these lowestlying levels are generated using the intermediate-coupling frame transformation R-matrix method. We assess the present results by comparisons with laboratory measurement for the excitation to the metastable level 3s 2 3p 2 P o 3/2 and with available close-coupling calculations for other excitations. Using these data and a collisional-radiative model, we have analyzed soft X-ray and extreme-ultraviolet spectra from space satellite observations of a stellar corona and of solar flares, as well as measurements from an electron beam ion trap. We assess the contribution from Fe 13+ emission lines in the solar and Procyon corona observations, and find and identify new lines in the X-ray region observed in the solar and Procyon coronae. The laboratory measurements also confirm that weak lines (218.177 Å and 224.354 Å) of Fe 13+ contribute to the observed intensities in solar observations. The polarization effect due to the directional monoenergetic distribution of the electron energy has been taken into account in comparison with the laboratory measurements. Electron density diagnostics for the astrophysical plasma sources have been performed using the updated data so as to investigate their sensitivity to the atomic data source.

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“…Also, the calculations allowed new lines to be identified; see, for example, Träbert et al (2011). On the experimental side, Träbert and coworkers have reported lifetimes as well as spectra for line identification from accelerator based work (Träbert et al 1985(Träbert et al , 1988(Träbert et al , 1989(Träbert et al , 2003Träbert 1986Träbert , 1998Träbert , 2005. Calculated excitation energies can be directly validated against observations and conversely, once a computational method and strategy was shown to be accurate, computed excitation energies aid further line identifications.…”

Section: Introductionmentioning

confidence: 99%

Accurate multiconfiguration calculations of energy levels, lifetimes, and transition rates for the silicon isoelectronic sequence

Jönsson

Radžiūtė

Gaigalas

et al. 2015

A&A

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Multiconfiguration Dirac-Hartree-Fock (MCDHF) calculations and relativistic configuration interaction (RCI) calculations are performed for states of the 3s 2 3p 2 , 3s3p 3 and 3s 2 3p3d configurations in the Si-like ions Ti IX -Ge XIX, Sr XXV, Zr XXVII and Mo XXIX. Valence and core-valence electron correlation effects are accounted for through large configuration state function expansions. Calculated energy levels are compared with data from other calculations and with experimental data from the reference databases. Lifetime and transition rates along with uncertainty estimations are given for all ions. Energies from the calculations are in excellent agreement with observations and computed wavelength are almost of spectroscopic accuracy, aiding line identification in spectra.

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Intercombination lines in delayed beam-foil spectra

Cited by 115 publications

References 65 publications

CHIANTI – an atomic database for emission lines

CHIANTI – an atomic database for emission lines

R -MATRIX ELECTRON-IMPACT EXCITATION OF Fe ¹³⁺ AND ITS APPLICATION TO THE SOFT X-RAY AND EXTREME-ULTRAVIOLET SPECTROSCOPY OF CORONA-LIKE PLASMAS

Accurate multiconfiguration calculations of energy levels, lifetimes, and transition rates for the silicon isoelectronic sequence

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Intercombination lines in delayed beam-foil spectra

Cited by 115 publications

References 65 publications

CHIANTI – an atomic database for emission lines

CHIANTI – an atomic database for emission lines

R -MATRIX ELECTRON-IMPACT EXCITATION OF Fe 13+ AND ITS APPLICATION TO THE SOFT X-RAY AND EXTREME-ULTRAVIOLET SPECTROSCOPY OF CORONA-LIKE PLASMAS

Accurate multiconfiguration calculations of energy levels, lifetimes, and transition rates for the silicon isoelectronic sequence

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Product

Resources

About

R -MATRIX ELECTRON-IMPACT EXCITATION OF Fe ¹³⁺ AND ITS APPLICATION TO THE SOFT X-RAY AND EXTREME-ULTRAVIOLET SPECTROSCOPY OF CORONA-LIKE PLASMAS