A critical compilation and extended analysis of the Ne V spectrum

Kramida, Alexander; Bastin, Thierry; Biémont, Émile; Dumont, Paul-Dominique; Garnir, Henri-Pierre

doi:10.1007/s100530050381

Cited by 25 publications

(28 citation statements)

References 1 publication

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“…Differences between the old CHIANTI A values and the Merkelis et al (1999) ones are within 30%, with only one exception ( 2 D 3/2 -2 P 3/2 ) having a difference of 40%. In addition the Ne iv experimental energy values have been replaced with the values from Kramida et al (1999).…”

Section: Ne IVmentioning

confidence: 99%

Chianti—an Atomic Database for Emission Lines. Xii. Version 7 of the Database

Landi

Zanna

Young

et al. 2011

ApJ

328

330

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The CHIANTI spectral code consists of an atomic database and a suite of computer programs to calculate the optically thin spectrum of astrophysical objects and carry out spectroscopic plasma diagnostics. The database includes atomic energy levels, wavelengths, radiative transition probabilities, collision excitation rate coefficients, and ionization and recombination rate coefficients, as well as data to calculate free-free, free-bound, and two-photon continuum emission. Version 7 has been released, which includes several new ions, significant updates to existing ions, as well as Chianti-Py, the implementation of CHIANTI software in the Python programming language. All data and programs are freely available at http://www.chiantidatabase.org, while the Python interface to CHIANTI can be found at http://chiantipy.sourceforge.net.

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Section: Ne IVmentioning

confidence: 99%

Chianti—an Atomic Database for Emission Lines. Xii. Version 7 of the Database

Landi

Zanna

Young

et al. 2011

ApJ

328

330

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“…If an experimental spectrum was to show a few hundred lines, and the theory predicted a few hundred lines, there would be no easy mapping of one set to the other, and most likely it would turn out (as it regularly does) that the experiment shows a plenitude of lines that are not identifiable from current calculations. As an example, we cite the long-drawn and not yet fully successful quest for the analysis of beam-foil spectra of four-to six-electron ions of an element as light as Ne (Z = 10) [2][3][4][5][6]. It would be a mark of substantial progress if even the most prominent lines in spectra of ions with two to four valence electrons could be predicted well enough to enable immediate identification within the experimental and calculational uncertainties.…”

Section: Introductionmentioning

confidence: 99%

Relativistic multireference many-body perturbation theory calculations on F-, Ne-, Na-, Mg-, Al-, Si- and P-like xenon ions

Vilkas

Ishikawa

2006

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

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“…Wavelengths and energy levels of Ne iv were assessed by Kramida et al (1999). The 2 D-2 P forbidden transitions lie between 4715 and 4727 Å and so are not found in the present UVES spectra, thus the wavelengths of Bowen (1960) still represent the best measurements of these lines.…”

Section: Ne IVmentioning

confidence: 74%

On maps of the two-dimensional sphere

Shchepin¹

2003

Russ. Math. Surv.

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Ultraviolet and visible spectra of the symbiotic nova RR Telescopii are used to derive reference wavelengths for many forbidden and intercombination transitions of ions +1 to +6 of elements C, N, O, Ne, Na, Mg, Al, Si, P, S, Cl, Ar, K, and Ca. The wavelengths are then used to determine new energy values for the levels within the ions' ground configurations or first excited configuration. The spectra were recorded by the Space Telescope Imaging Spectrograph of the Hubble Space Telescope and the Ultraviolet Echelle Spectrograph of the European Southern Observatory in 2000 and 1999, respectively, and cover 1140-6915 Å. Particular care was taken to assess the accuracy of the wavelength scale between the two instruments. An investigation of the profiles of the emission lines reveals that the nebula consists of at least two plasma components at different velocities. The components have different densities, and a simple model of the lines' emissions demonstrates that most of the lines principally arise from the high density component. Only these lines were used for the wavelength study.

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A critical compilation and extended analysis of the Ne V spectrum

Cited by 25 publications

References 1 publication

Chianti—an Atomic Database for Emission Lines. Xii. Version 7 of the Database

Chianti—an Atomic Database for Emission Lines. Xii. Version 7 of the Database

Relativistic multireference many-body perturbation theory calculations on F-, Ne-, Na-, Mg-, Al-, Si- and P-like xenon ions

On maps of the two-dimensional sphere

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