Experimental M1 Transition Rates of Coronal Lines from Ar<scp>x</scp>, Ar<scp>xiv</scp>, and Ar<scp>xv</scp>

Trabert, E; Beiersdörfer, P.; Utter, S. B.; Brown, Gregory V.; Chen, H.; Harris, C. L.; Neill, P.; Savin, D. W.; Smith, A. J.

doi:10.1086/309427

Cited by 75 publications

(45 citation statements)

References 37 publications

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“…The earlier measurements of Serpa et al (1998) and Moehs & Church (1998) give values of 8.7 ± 0.5 ms and 9.12 ± 0.15 ms, respectively. However, the later measurement by Träbert et al (2000) gives a value of 9.70 ± 0.15 ms, which also agrees very well with our result of 9.714 ms. Additional measurements of τ for other levels of Ar XIV will be helpful in further assessing the accuracy of our calculations.…”

Section: Ar XIVsupporting

confidence: 92%

Energy levels and radiative rates for transitions in Ar XIII, Ar XIV and Ar XV

Aggarwal¹,

Keenan²,

Nakazaki

2005

A&A

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Abstract. Energies for 524 levels of Ar XIII, 460 levels of Ar XIV and 156 levels of Ar XV have been calculated using the  code of Dyall et al. (1989). Additionally, radiative rates, oscillator strengths, and line strengths are calculated for all electric dipole (E1), magnetic dipole (M1), electric quadrupole (E2), and magnetic quadrupole (M2) transitions among these levels. Comparisons are made with the limited results available in the literature, and the accuracy of the data is assessed. Our energy levels are estimated to be accurate to better than 1%, whereas results for other parameters are probably accurate to better than 20%. Additionally, the level lifetimes derived from our radiative rates are in excellent agreement with measured values.

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Section: Ar XIVsupporting

confidence: 92%

Energy levels and radiative rates for transitions in Ar XIII, Ar XIV and Ar XV

Aggarwal¹,

Keenan²,

Nakazaki

2005

A&A

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“…The gas of interest is injected ballistically at reservoir pressures below 10 −7 mbar into the ultrahigh vacuum of the EBIT vessel; the gas plume expands to a pressure well below 10 −9 mbar where it traverses the actual trap volume and the electron beam (Träbert et al 2000). Collisions with the electron beam disintegrate the molecules; any resulting positively charged particles are being trapped in the combination of electric and magnetic fields of a Penning trap plus the space charge effects caused by the electron beam.…”

Section: Measurementmentioning

confidence: 99%

Low-density laboratory spectra near the He iiλ304 line

Beiersdörfer

Brickhouse

Golub

2016

A&A

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Aims. To interpret the EUV spectra of the solar corona, one hopes for laboratory data of specific chemical elements obtained under coronal conditions. Methods. EUV spectra of He, C, N, O, F, Ne, S, Ar, Fe, and Ni in a 40 Å wide wavelength interval near λ304 were excited in an electron beam ion trap. Results. We observe some two hundred lines about half of which are not yet identified and included in spectral models. Conclusions. Our data provide a check on the atomic data bases underlying the spectral models that are used to interpret solar corona data. However, a multitude of mostly weak additional lines taken together represent a flux that is comparable to that of various primary lines.

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“…In the same year and by the same approach, Koc produced fine structure intervals and M1/E2 transition rates within the ground term of B-like ions with an atomic number Z from 10 to 30, and so on [39][40][41]. This latter topic ties in with the demand for accurate ab initio calculations to compare with accurate wavelength and lifetime measurements at electron beam ion traps (EBIT) [42][43][44][45]. However, in this latter suite of studies, only a single transition is of primary interest (see [46]), the electric-dipole (E1) forbidden transition in the 2s 2 2p 2 P o ground term.…”

Section: Earlier Workmentioning

confidence: 99%

MCDHF Calculations and Beam-Foil EUV Spectra of Boron-Like Sodium Ions (Na VII)

Jönsson

Ekman

Trabert

2015

Atoms

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Atomic data, such as wavelengths and line identifications, are necessary for many applications, especially in plasma diagnostics and for interpreting the spectra of distant astrophysical objects. The number of valence shell electrons increases the complexity of the computational problem. We have selected a five-electron ion, Na 6+(with the boron-like spectrum Na VII), for looking into the interplay of measurement and calculation. We summarize the available experimental work, perform our own extensive relativistic configuration interaction (RCI) computations based on multi-configuration Dirac-Hartree-Fock (MCDHF) wave functions, and compare the results to what is known of the level structure. We then discuss problems with databases that have begun to combine observations and computations.

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Experimental M1 Transition Rates of Coronal Lines from Arx, Arxiv, and Arxv

Cited by 75 publications

References 37 publications

Energy levels and radiative rates for transitions in Ar XIII, Ar XIV and Ar XV

Energy levels and radiative rates for transitions in Ar XIII, Ar XIV and Ar XV

Low-density laboratory spectra near the He iiλ304 line

MCDHF Calculations and Beam-Foil EUV Spectra of Boron-Like Sodium Ions (Na VII)

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