Classification of sulphur VII to XIV spectra between 22 and 73 Å with wavelengths, oscillator strengths and energy levels

Fawcett, B C; Hayes, R. W.

doi:10.1088/0031-8949/36/1/013

Cited by 37 publications

(28 citation statements)

References 18 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%

“…The experimental energy levels for the n = 2 levels are taken from Edlén (1983), while those for the n = 3 levels come from Fawcett & Hayes (1987) and Bengtsson et al (1993). The effective collision strengths were published by Witthoeft et al (2007b) for the 4.1 ≤ log T ≤ 8.1 temperature range but we used them only in the 4.5 ≤ log T ≤ 7.3 range to improve the fit of the original data in the range where S viii has significant fractional abundance.…”

Section: S VIIImentioning

confidence: 99%

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CHIANTI – an atomic database for emission lines

Dere¹,

Landi²,

Young³

et al. 2009

A&A

461

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%

Section: S VIIImentioning

confidence: 99%

CHIANTI – an atomic database for emission lines

Dere¹,

Landi²,

Young³

et al. 2009

A&A

461

451

View full text Add to dashboard Cite

show abstract

“…Such lines have been observed in the Sun only once, because of the paucity of observations in that wavelength range, by Acton et al (1985), but they have been identified in laboratory spectra in several occasions (Fawcett, Hardcastle, & Tondello 1970;Fawcett & Hayes 1973, 1987. The X-ray lines are primarily emitted by levels in the 2s 2 2p3l (l ¼ s, d ) configurations, but Fawcett & Hayes (1987) also identified for the first time a few transitions coming from the 2s 2 2p4d configurations. EUV lines are emitted by allowed transitions within the n ¼ 2 configurations, and they provide excellent density-sensitive line pairs, which allow us to measure electron densities in the 10 7 -10 10 cm À3 range.…”

Section: Introductionmentioning

confidence: 99%

Atomic Data and Spectral Line Intensities for S xi

Landi

Bhatia

2003

ASTROPHYS J SUPPL S

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Electron impact collision strengths, energy levels, oscillator strengths, and spontaneous radiative decay rates are calculated for S xi. The configurations included are 2s 2 2p 2 , 2s2p 3 , 2p 4 , 2s 2 2p3l, and 2s 2 2p4l (l ¼ s, p, d ), giving rise to 72 fine-structure levels in intermediate coupling. Collision strengths are calculated at five incident energies, 32, 60, 90, 120, and 150 ryd. Excitation rate coefficients are calculated as a function of electron temperature by assuming a Maxwellian electron velocity distribution. Using the excitation rate coefficients and the radiative transition rates, statistical equilibrium equations for level populations are solved. The effects of resonances, proton rates, photoexcitation, and cascades on level populations have been investigated. The predicted S xi line intensities are compared with EUV and UV observations of the quiet and active Sun.

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“…Aa9*Il&u r Theoretical investigation of the Ne-like isoelectronic sequence spectroscopic properties was performed by a number of authors [13][14][15][16]. Experimentally it was investigated up to Z = 60 (for 3-2 transitions) [17].…”

Section: Aiamentioning

confidence: 99%

Inexpensive Capillary Discharge X-Ray Laser Driver

Panin¹

1993

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Classification of sulphur VII to XIV spectra between 22 and 73 Å with wavelengths, oscillator strengths and energy levels

Cited by 37 publications

References 18 publications

CHIANTI – an atomic database for emission lines

CHIANTI – an atomic database for emission lines

Atomic Data and Spectral Line Intensities for S xi

Inexpensive Capillary Discharge X-Ray Laser Driver

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