He-like ion resonance-line satellites radiated from Be-like ions

Бойко, В. А.; Chugunov, A Yu; Ivanova, T. G.; Faenov, A. Ya.; Holin, I. V.; Pikuz, S. A.; Urnov, A. M.; Vaĭnshteĭn, L. A.; Safronova, U. I.

doi:10.1093/mnras/185.2.305

Cited by 46 publications

(24 citation statements)

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“…Our Si detector begins spectral observations from 4 keV and it is therefore not possible to observe the Ca-line feature around 3.8 keV. However the observed increase in T e unambiguously leads to a change in peak energy because of the excitation of different principal lines of the He-like Fe XXV, satellites and resonance lines in agreement with earlier calculations (Gabriel, 1972, Boiko et al, 1978, Doschek et al, 1981, Feldman et al, 1995, Kato et al, 1997.…”

Section: Discussionsupporting

confidence: 89%

The Fe-Line Feature in the X-Ray Spectrum of Solar Flares: First Results from the SOXS Mission

et al. 2006

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We present the first results from the "Low Energy Detector" payload of the "Solar earlier by various investigators and propose that these measurements may improve theoretical models. We interpret the variation of both E p and w with temperature as due to the changes in the ionization and recombination conditions in the plasma during the flare interval and as a consequence the contribution from different ionic emission lines also varies.

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Section: Discussionsupporting

confidence: 89%

The Fe-Line Feature in the X-Ray Spectrum of Solar Flares: First Results from the SOXS Mission

et al. 2006

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“…Comparison of present FAC2 wavelengths with theoretical results from Palmeri et al (2008) and Boiko et al (1979) confirms that the average wavelength differences are smaller than 3 mÅ. No wavelength shifts need to be applied to our results.…”

Section: Discussionsupporting

confidence: 88%

“…The average wavelength difference between our results and theirs is 1 mÅ ± 2.4 mÅ. Boiko et al (1979) also reported the experimental measurements, which were reanalyzed by Faenov et al (1994). Comparison with those wavelengths presented by Palmeri et al (2008) are also shown in Fig.…”

Section: Energy Levels and Wavelengthssupporting

confidence: 86%

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K-shell energy levels and radiative rates for transitions in Si xi

Wei

Shi

Zhao

et al. 2010

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Context. Atomic data for K-shell transitions are essential for modeling the K absorption lines, which have been observed in the spectra of active galaxies by high-resolution X-ray observatories, e.g. XMM, Chandra, and Suzaku. These accurate atomic data are also needed for line identifications and spectroscopic diagnostic of plasmas in laboratory generated by laser or beam-foil method. Aims. We calculate atomic data using the atomic code flexible atomic code (FAC) taking relativistic effects and configuration interactions into account. Methods. We calculate the K-shell transitions among the configurations of 1s 2 2s 2 , 1s 2 2s2p, 1s 2 2p 2 , 1s 2 2sn l , 1s 2 2pn l , 1s2s 2 2p, 1s2s2p 2 , 1s2p 3 , 1s2s2pn l , and 1s2p 2 n l , n ≤ 4, l ≤ n for beryllium-like Si xi. We present the K-shell energy levels, wavelengths, radiative rates, and oscillator strengths for Si xi. To assess the accuracy of current data, we compare our results with both former experiments and other theoretical works.Results. The present K-shell level energies and wavelengths are accurate to within 2 eV and 10 mÅ, respectively. The radiative rates have an accuracy of around 20% for the majority of our transitions.

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“…The NIST database is available at http://www.physics. nist.gov/PhysRefData and the data for this ion is attributed to Artru (1977), Boiko et al (1978), Edlen (1979), Fawcett (1970), Hoory et al (1970), Ridgely & Burton (1972) and Söderqvist (1944). Good agreement is observed between the NIST values and those from the current calculation using the CIV3 structure code, with the current values differing on average by 0.0346 Rydbergs.…”

Section: Calculation Detailsmentioning

confidence: 96%

Breit-Pauli R-matrix calculation for fine structure effective collision strengths from electron impact excitation of Mg IX

Hudson¹

2008

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Context. Electron impact excitation collision strengths are required for analysing and interpreting stellar observations.Aims. This calculation aims to provide fine-structure effective collision strengths for the Mg ix ion using a method that includes contributions from resonances. Methods. A 26-state Breit-Pauli R-matrix calculation has been performed. The target states are represented by configuration interaction wavefunctions and consist of the 26 lowest LS states, having configurations 2s 2 , 2s2p, 2p 2 , 2s3s, 2s3p, 2s3d, 2p3s, 2p3p, and 2p3d. These target states give rise to 46 fine structure levels and 1035 possible transitions. The effective collision strengths are calculated by averaging the electron collision strengths over a Maxwellian distribution of electron velocities. Results. The non-zero effective collision strengths for transitions between the fine structure levels are given for electron temperatures (T e ) in the range log 10 T e (K) = 3.0-7.0. Values for selected transitions are given in this paper and links provided to the entire data set.

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He-like ion resonance-line satellites radiated from Be-like ions

Cited by 46 publications

References 0 publications

The Fe-Line Feature in the X-Ray Spectrum of Solar Flares: First Results from the SOXS Mission

The Fe-Line Feature in the X-Ray Spectrum of Solar Flares: First Results from the SOXS Mission

K-shell energy levels and radiative rates for transitions in Si xi

Breit-Pauli R-matrix calculation for fine structure effective collision strengths from electron impact excitation of Mg IX

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