Intensity ratios of emission lines from O V ions for temperature and density diagnostics, and recommended excitation rate coefficients

Katō, Takako; Lang, J.; Berrington, K.E.

doi:10.1016/0092-640x(90)90021-b

Cited by 31 publications

(14 citation statements)

References 12 publications

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“…The data for transition probabilities between n = 2 and n = 3 levels are taken from Hibbert (1980). The electron excitation rate coefficients are taken from the fitted data in the analytical formula given by Kato et al (1990) which are based on the data by Berrington (1987). We also include the excitation by protons with data from Doyle et al (1987) for the fine structure transitions within the triplet 2s2p 3 P o and 2p 2 3 P levels.…”

Section: Atomic Datamentioning

confidence: 99%

“…Furthermore, measurements of lifetimes (Engström et al 1981) have shown that the multiplet lines show different lifetimes due to a J -selective transition in the multiplet. We have constructed a collisional radiative model for OV with fine structure levels and studied the line intensity ratios for density and temperature diagnostics (Kato et al 1990). In this paper the calculated electron density and temperature dependences of the line ratios of these multiplet lines are compared with measurements from the Extrap T1 and T2 RFP experiments.…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Observations and modelling of line intensity ratios of OV multiplet lines for -

Katō¹,

Rachlew-Källne²,

Hörling³

et al. 1996

J. Phys. B: At. Mol. Opt. Phys.

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Line intensity ratios of OV multiplet lines for the 2s3s 3 S 1 -2s3p 3 P J (J = 2, 1, 0) transitions are studied using a collisional radiative model and the results are compared with measurements from the reversed field pinch experiments Extrap T1 and T2 at KTH. The measured line intensity ratios deviate from the predictions of the model and the possible causes for the discrepancy are discussed with regard to errors in rate coefficients and non-quasi-steady state.

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Section: Atomic Datamentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Observations and modelling of line intensity ratios of OV multiplet lines for -

Katō¹,

Rachlew-Källne²,

Hörling³

et al. 1996

J. Phys. B: At. Mol. Opt. Phys.

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show abstract

“…also provide relativistic DW collision strengths among the n = 2 levels. Collision strengths to the n = 3 levels are provided by Kato et al (1990) who use the R-matrix calculations of Berrington & Kingston (1990). The values of Kato et al have been recently updated (Kato 1996).…”

Section: O Vmentioning

confidence: 99%

CHIANTI - an atomic database for emission lines

Dere

Landi

Mason

et al. 1997

Astron. Astrophys. Suppl. Ser.

1,979

1,669

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Abstract. A comprehensive set of accurate atomic data is required for analyses of astrophysical and solar spectra. CHIANTI provides a database of atomic energy levels, wavelengths, radiative data and electron excitation data for ions which are abundant in cosmic plasmas. The most recent electron excitation data have been assessed and stored following the method of Burgess & Tully (1992). The current version is essentially complete for specifying the emission spectrum at wavelengths greater than 50Å. A list of observed lines in the spectral region between 50 and 1100Å has been compiled and compared with the lines predicted by the CHIANTI database. The CHIANTI database reproduces the vast majority of lines observed at these wavelengths. CHIANTI includes IDL (Interactive Data Language) routines to calculate optically thin synthetic spectra for equilibrium conditions. IDL routines to calculate theoretical line intensities required for electron density or temperature diagnostics and emission measure studies are also included. The CHIANTI atomic database and supporting IDL routines are available by anonymous FTP.

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“…The remaining rates were taken from Kato et al (1990). Kato et al give only the total rates for the following transitions involving a singlet and a triplet: 2s 2 -2p 2 3 P, 2s 2p 3 P-2s 2p 1 P, 2p 2 3 P-2p 2 1 D and 2p 2 3 P-2p 2 1 S. Lacking more information, we therefore subdivided these rates according to the statistical weights of the triplets involved.…”

Section: Transition Ratesmentioning

confidence: 99%

X-ray/UV campaign on the Mrk 279 outflow: Density diagnostics in Active Galactic Nuclei using O v K-shell absorption lines

Kaastra

Raassen

Mewe

et al. 2004

A&A

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Abstract.One of the main problems in modeling the ionised outflows in Active Galactic Nuclei is the unknown distance of the outflowing wind to the central source. Only if the density is known this distance can be determined through the ionisation parameter. Here we study density diagnostics based upon O  transitions. O  is known to have metastable levels that are density dependent. We study the population of those levels under photoionisation equilibrium conditions and determine for which parameter range they can have a significant population. We find that resonance line trapping plays an important role in reducing the critical densities above which the metastable population becomes important. We investigate the K-shell absorption lines from these metastable levels. Provided that there is a sufficient population of the metastable levels, the corresponding K-shell absorption lines are detectable and are well separated from the main absorption line originating from the ground state. We then present the Chandra LETGS spectrum of the Seyfert 1 galaxy Mrk 279 that may show for the first time the presence of these metastable level absorption lines. A firm identification is not yet possible due to both uncertainties in the observed wavelength of the strongest line as well as uncertainties in the predicted wavelength. If the line is indeed due to absorption from O , then we deduce a distance to the central source of one light week to a few light months, depending upon the importance of additional heating processes.

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Intensity ratios of emission lines from O V ions for temperature and density diagnostics, and recommended excitation rate coefficients

Cited by 31 publications

References 12 publications

Observations and modelling of line intensity ratios of OV multiplet lines for -

Observations and modelling of line intensity ratios of OV multiplet lines for -

CHIANTI - an atomic database for emission lines

X-ray/UV campaign on the Mrk 279 outflow: Density diagnostics in Active Galactic Nuclei using O v K-shell absorption lines

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