ATOMIC DATA AND SPECTRAL LINE INTENSITIES FOR Ni XVI

Bhatia, A. K.; Doschek, G. A.

doi:10.1006/adnd.1998.0800

Cited by 13 publications

(24 citation statements)

References 29 publications

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“…The previous versions of CHIANTI had only a few observed energies listed for Ni xvi despite the fact that there have been many observations available in the literature. We have retained the theoretical energy levels from Bhatia & Doschek (1999) and have replaced the experimental energies with the values from Fawcett & Hatter (1980), Träbert et al (1988), Redfors & Litzen (1989), Hinnov et al (1990), and Sugar et al (1992). Most of the 40 levels have now been assigned an observed energy.…”

Section: Ni XVImentioning

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: Ni XVImentioning

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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“…Previously, fine-structure excitation energies, absorption oscillator strengths and radiative decay rates for resonance transitions in Fe XIV and Ni XVI were studied both experimentally and theoretically (Corliss and Sugar 1982, Buchet-Poulizac and Buchet 1988, Redfors and Litzen 1989, Levashov et al 1990, Hinnov et al 1990, Pinnington et al 1990, Churilov and Levashov 1993, Trabert et al 1988, Jupen and Curtis 1996, Mendoza et al 1995, Farrag et al 1982, Fawcett 1983, Huang 1986, Froese Fischer and Liu 1986, Fuhr et al 1988, Bhatia and Doschek 1999. Trabert et al (1988Trabert et al ( , 1993) also reported the experimental lifetimes in Fe XIV and Ni XVI for high-spin 3s3p 2 4 P and 3s3p3d 4 F o levels.…”

Section: Introductionmentioning

confidence: 99%

“…These ions are also known to produce resonance transitions in the EUV solar spectra (Behring et al 1972) and in the spectra of many solar-type stars as well as in other astrophysical objects. Accurate atomic data for these cosmically abundant ions are needed to interpret observational data, now becoming available from the EUVE spacecraft, the solar and heliospheric observatory (SOHO) spacecraft, and the Hubble Space Telescope (Feldman et al 1988, Bhatia andDoschek 1999). These data are also useful for estimating the energy loss through impurity ions in fusion plasma and for diagnostics and modelling of the plasma.…”

Section: Introductionmentioning

confidence: 99%

“…Wavelengths, energy levels, oscillator strengths and radiative transition probabilities for various highly ionized nickel ions have been critically reviewed and tabulated by Shirai et al (1987). Recently, Bhatia and Doschek (1999) have reported electron impact collision strengths and spontaneous radiative decay rates for Ni XVI within the 3s 2 3p, 3s3p 2 , 3s 2 3d, 3p 3 and 3s3p3d configurations, while Deb and Msezane (2001) have calculated fine-structure energy levels for the 40 lowest states and oscillator strengths for transitions among the fine-structure levels for Ni XVI using program CIV3 of Hibbert (1975), with relativistic effects incorporated through the Breit-Pauli Hamiltonian.…”

Section: Introductionmentioning

confidence: 99%

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Fine-structure energy levels and lifetimes in Al-like iron and nickel

Gupta

Msezane²

2001

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

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“…Blackbody radiation has also been added to Eq. (4) by assuming [31] that close to a stellar surface the number of absorptions, F i j , per second between lower level i and upper level j is given bywhere T B is the stellar equivalent blackbody temperature which has been assumed as 5800 K. The factor of 1 2 in Eq. (7), called the dilution factor, reflects the fact that the stellar atmosphere blackbody radiation arises from 2π , and not 4π steradians.…”

mentioning

confidence: 99%

Atomic Data and Spectral Line Intensities for Fe VIII

Bhatia

Eissner²

2000

Atomic Data and Nuclear Data Tables

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Electron impact collision strengths, energy levels, oscillator strengths and spontaneous radiative decay rates are calculated for Fe VIII. The configurations used are 3 p 6 3d, 3p 5 3d 2 , 3p 6 4s, 3p 6 4p, and 3 p 5 3d4s giving rise to 73 fine-structure levels in intermediate coupling. Collision strengths are calculated at four incident energies, 10, 30, 50, and 70 Ry. Excitation rate coefficients are calculated by assuming a Maxwellian electron velocity distribution at an electron temperature of log T e (K) = 5.57, corresponding to maximum abundance of Fe VIII. Using the excitation rate coefficients and the radiative transition rates, statistical equilibrium equations for level populations are solved at electron densities 10 8 -10 14 cm −3 . Relative spectral line intensities are calculated. Proton excitation rates and solar blackbody radiative excitation are also included in the statistical equilibrium equations. C [2,3]. The same set of lines has also been observed by Malinovsky and Heroux [4], who measured the spectra photoelectrically using a double spectrometer flown on an Aerobee rocket. The 185.221Å line has been observed from the SERTS-95 flight [5] but it is blended with the Ni XVI line at 185.231Å. The same line has also been observed with the RES-K spectroheliograph on board the KORONAS-I satellite [6]. There are a number of unidentified lines in the recent compilation of lines observed from the UV spectrometer SUMER on SOHO [7] and it is suspected that some of these lines could be Fe VIII lines. Accurate atomic data for this ion must be available for identification of various spectral lines and to infer properties of solar and astrophysical plasmas. The presently calculated data will be useful for any present and future observations.In order to interpret data from these missions, atomic data such as energy levels, oscillator strengths, radiative transition rates, and collision strengths are required. provides all the quantities required for diagnostic purposes. In this paper we carry out a distorted wave calculation for Fe VIII in the same way as for the other Fe ions mentioned above. Since coupling between various channels is not included in the distorted wave approximation, the present calculation does not include resonances which could be important for forbidden transitions but usually not for dipole-allowed transitions for which most of the contribution to collision strengths comes from a very large number of incident partial waves.We present energy levels, oscillator strengths, radiative transition rates, and collision strengths for Fe VIII for 73 finestructure levels obtained by using the configurations 3 p 6 3d, 3 p 5 3d 2 , 3p 6 4s, 3p 6 4p, and 3 p 5 3d4s, above the Mg-like 1s 2 2s 2 2 p 6 3s 2 core. Although Fe VIII is K-like, the outermost electron is in the 3d orbital, not in the 4s orbital as in neutral potassium. Therefore, the lowest configuration is 3 p 6 3d. We solve the statistical equilibrium equations for level populations at log T e (K) = 5.57 where T e is the temperature of...

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ATOMIC DATA AND SPECTRAL LINE INTENSITIES FOR Ni XVI

Cited by 13 publications

References 29 publications

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

Fine-structure energy levels and lifetimes in Al-like iron and nickel

Atomic Data and Spectral Line Intensities for Fe VIII

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