Influence of core polarisation on oscillator strengths along the copper isoelectronic sequence

Migdałek, J.; Baylis, W. E.

doi:10.1088/0022-3700/12/7/014

Cited by 80 publications

(80 citation statements)

References 20 publications

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“…The multiplet f -value (0.78 ± 0.06) of the As v resonance transition was determined with the help of arbitrarily normalized decay curve (ANDC) analyses, which were confirmed by calculations of Fischer (1977), Migdalek & Baylis (1979), and Curtis & Theodosiou (1989). Morton (2000) lists both components in his compilation, λ 987.65 Å (4s 2 S 1/2 −4p 2 P • 3/2 , f = 0.528) and λ 1029.48 Å (4s 2 S 1/2 −4p 2 P • 1/2 , f = 0.253).…”

Section: Photospheric Abundancesmentioning

confidence: 88%

Stellar laboratories

Rauch¹,

Quinet²,

Hoyer³

et al. 2016

A&A

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Context. For the spectral analysis of high-resolution and high signal-to-noise (S/N) spectra of hot stars, state-of-the-art non-local thermodynamic equilibrium (NLTE) model atmospheres are mandatory. These are strongly dependent on the reliability of the atomic data that is used for their calculation. Aims. To identify molybdenum lines in the ultraviolet (UV) spectra of the DA-type white dwarf G191−B2B and the DO-type white dwarf RE 0503−289 and, to determine their photospheric Mo abundances, reliable Mo iv-vii oscillator strengths are used. Methods. We newly calculated Mo iv-vii oscillator strengths to consider their radiative and collisional bound-bound transitions in detail in our NLTE stellar-atmosphere models for the analysis of Mo lines exhibited in high-resolution and high S/N UV observations of RE 0503−289.Results. We identified 12 Mo v and 9 Mo vi lines in the UV spectrum of RE 0503−289 and measured a photospheric Mo abundance of 1.2−3.0 × 10 −4 (mass fraction, 22 500−56 400 times the solar abundance). In addition, from the As v and Sn iv resonance lines, we measured mass fractions of arsenic (0.5−1.3 × 10 −5 , about 300−1200 times solar) and tin (1.3−3.2 × 10 −4 , about 14 300−35 200 times solar). For G191−B2B, upper limits were determined for the abundances of Mo (5.3 × 10 −7 , 100 times solar) and, in addition, for Kr (1.1 × 10 −6 , 10 times solar) and Xe (1.7 × 10 −7 , 10 times solar). The arsenic abundance was determined (2.3−5.9 × 10 −7 , about 21−53 times solar). A new, registered German Astrophysical Virtual Observatory (GAVO) service, TOSS, has been constructed to provide weighted oscillator strengths and transition probabilities. Conclusions. Reliable measurements and calculations of atomic data are a prerequisite for stellar-atmosphere modeling. Observed Mo v-vi line profiles in the UV spectrum of the white dwarf RE 0503−289 were well reproduced with our newly calculated oscillator strengths. For the first time, this allowed the photospheric Mo abundance in a white dwarf to be determined.

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Section: Photospheric Abundancesmentioning

confidence: 88%

Stellar laboratories

Rauch¹,

Quinet²,

Hoyer³

et al. 2016

A&A

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“…The temporal dynamics of several lines is shown in Figure 2. While the temporal decay of some lines can be fitted, at least roughly, by an exponential function (Curtis and Theodosiou, 1989) b Laser-induced fluorescence from sputtered metal vapors (Hannaford and Lowe, 1983) c Numerical Coulomb-like approximation (Lindgård et al, 1980) d Relativistic Hartree-Fock calculation with account for core polarisation effects (Migda lek and Baylis, 1978) e Relativistic Hartree-Fock calculation with model potential accounting for exchange and core polarisation (Migda lek, 1978) f Relativistic Hartree-Fock calculation with model potential and core polarisation (Migda lek and Baylis, 1979) g Calculation using the level-crossing measurement of lifetimes and configuration coupling coefficient deduced by fitting other experimental measurements of lifetimes and relative oscillator strengths (Siefart et al, 1974) h Atomic absorption measurements on flames (Lvov, 1970) i Atomic-beam absorption (Bell and Tubbs, 1970) j Critical survey of experimentally-determined oscillator strengths (Corliss, 1970) k Curves of growth in absorption measurement (Moise, 1966) l Rozhdestvenskii's hook method (Slavenas, 1966) m Atomic-beam absorption (Bell et al, 1958) n Arc emission measurements (Allen and Asaad, 1957) a Time profile demonstrates significant deviation from the exponential decay b The decay curve has essentially non-exponential form with a plateau or secondary maxima; τ value is absent or roughly approximate several lines display essentially non-exponential behavior including some "plateaux" or even secondary maxima at 35-50 µs after the laser shot. Their decay time, T , values are therefore estimated in Table 3 in a rough approximation; it is seen from this table that for essentially non-exponential decays the uncertainity ∆T is of the same order of magnitude as T itself.…”

Section: Lines Observedmentioning

confidence: 99%

Time-resolved FTIR emission spectroscopy of Cu in the 1800–3800 cm⁻¹region: transitions involving f and g states and oscillator strengths

Civiš

Matulková

Cihelka

et al. 2011

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

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Time-resolved Fourier-transform spectroscopy was applied to the study of the emission spectra of Cu vapours in a vacuum (10 −2 Torr) produced in ablation of a Cu metal target by a high-repetition rate (1.0 kHz) pulsed nanosecond ArF laser (λ = 193 nm, output energy of 15 mJ). The time-resolved infrared emission spectrum of Cu was recorded in the 1800-3800 cm −1 spectral region with a resolution of 0.017 cm −1 . The time profiles of the measured lines have maxima at 18-20 μs after a laser shot and display non-exponential decay with a decay time of 5-15 μs. This study reports 17 lines (uncertainty 0.0003-0.018 cm −1 ) of Cu I not previously observed. This results in seven newly-found levels and revised energy values for 11 known levels (uncertainty 0.01-0.03 cm −1 ). We also calculate transition probabilities and oscillator strengths for several transitions involving the reported Cu levels.

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“…(1) were used to calculate 4s 2 S − 4p 2 P o transition oscillator strengths and 4p 2 P o radiative lifetimes for Zn + for which a variety of experimental [10][11][12][13][14][15] and theoretical [3,5,17] results are available for comparison. The lifetime results are displayed in Table 2.…”

Section: One-electron Model For Zn +mentioning

confidence: 99%

The dipole polarisability of Zn+ and the highℓ Rydberg levels of Zn

Grib

Pavlov

1997

Z Phys D - Atoms, Molecules and Clusters

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An accurate 1-electron model of Zn + is developed and used to evaluate the long-range asymptotic form of the polarisation potential for an electron interacting with a Zn + 'core' up to terms of order r −8 . The static dipole polarisability of Zn + is calculated to be 16.7 au, in good agreement with an effective experimental value derived from observed zinc 4snf term values. Radiative lifetimes for 4p 1 2 , 3 2 resonance levels and several other excited levels of Zn + are also calculated. Energies of 4sn Rydberg levels of Zn for = 3 and 4 and n up to 26 are evaluated in first-and second-order perturbation theory; the 4snf energies are in accord with a recent measurement.

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Influence of core polarisation on oscillator strengths along the copper isoelectronic sequence

Cited by 80 publications

References 20 publications

Stellar laboratories

Stellar laboratories

Time-resolved FTIR emission spectroscopy of Cu in the 1800–3800 cm⁻¹region: transitions involving f and g states and oscillator strengths

The dipole polarisability of Zn+ and the highℓ Rydberg levels of Zn

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Influence of core polarisation on oscillator strengths along the copper isoelectronic sequence

Cited by 80 publications

References 20 publications

Stellar laboratories

Stellar laboratories

Time-resolved FTIR emission spectroscopy of Cu in the 1800–3800 cm−1region: transitions involving f and g states and oscillator strengths

The dipole polarisability of Zn+ and the highℓ Rydberg levels of Zn

Contact Info

Product

Resources

About

Time-resolved FTIR emission spectroscopy of Cu in the 1800–3800 cm⁻¹region: transitions involving f and g states and oscillator strengths