Spectrum and Energy Levels of Singly-Ionized Mercury (Hg II)

Sansonetti, Craig J.; Reader, Joseph

doi:10.1238/physica.regular.063a00219

Cited by 29 publications

(28 citation statements)

References 31 publications

(61 reference statements)

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“…The wavelengths for the λ4358 and the λ3984 lines were taken from , while the oscillator strengths are experimental values adopted from Benck et al (1989) for Hg  λ4358 (log g f = +0.34) and Dworetsky (1980) for Hg  λ3984 (log g f = −1.73). Note should be made that the log g f value of the Hg  λ3984 line adopted here is 0.2 dex lower than the theoretically calculated values of Proffitt et al (1999) (log g f = −1.529) and Sansonetti & Reader (2001) (log g f = −1.51). In our investigation the experimentally determined g f value was chosen since its experimental nature allows for an uncertainty to be attached, while the theoretically calculated value is of indeterminable uncertainty.…”

Section: Abundance Analysis and Line Datacontrasting

confidence: 63%

On the elemental abundance and isotopic mixture of mercury in HgMn stars

Dolk

Wahlgren

Hubrig

2003

A&A

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Abstract. Optical region spectra of 31 HgMn stars have been studied for the abundance and isotope mixture of mercury. In the course of the investigation the lines Hg  λ4358 and Hg  λλ3984,6149 have been studied, with abundances established for all three lines in several HgMn stars. The mercury isotope mixture has been determined from high resolution spectra of the λ3984 line. Possible signs of an ionization anomaly have been detected by the comparison of the abundance derived from the Hg  line and the Hg  lines in seven of the observed HgMn stars. A possible correlation of the mercury abundance with T eff has been detected. Possible signs of a weak anticorrelation of the manganese and mercury abundance in HgMn stars have been found, which could be interpreted as a sign of inhomogeneous surface distribution of these elements. For a number of the HgMn stars in this study the mercury abundance and isotope mixture are reported for the first time.

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Section: Abundance Analysis and Line Datacontrasting

confidence: 63%

On the elemental abundance and isotopic mixture of mercury in HgMn stars

Dolk

Wahlgren

Hubrig

2003

A&A

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“…The spectral resolution of the spectra and the effect of rotational broadening prevent us from detecting the signature of hyperfine splitting. Mercury abundance was derived using the line of HgII at 398.39 nm with the oscillator strength from Sansonetti & Reader (2001).…”

Section: Input Datamentioning

confidence: 99%

Looking for pulsations in HgMn stars through CoRoT lightcurves

Alecian¹,

Gebran

Auvergne

et al. 2009

A&A

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Context. HgMn chemically peculiar stars are among the quietest stars of the main-sequence. However, according to theoretical predictions, these stars could have pulsations related to the high overabundance of iron peak elements, which are produced by atomic diffusion in upper layers. Such pulsations have never been detected from ground-based observations. Aims. Our aim is to search for signatures of pulsation in HgMn stars using the high quality lightcurves provided by the CoRoT satellite. Methods. We identified three faint stars (V > 12), from a VLT-GIRAFFE multiobject spectrographic survey in a field planned for observation by CoRoT. They present the typical characteristics of HgMn stars. The three stars were observed by the CoRoT satellite during the long run (131 days) which started on 24 October 2007, with the exoplanets CCDs (Additional Programme). In the present work, we present the analysis of the ground-based spectra of these three stars and of the corresponding CoRoT lightcurves. Results. Two of these three HgMn candidates show low amplitude (less than 1.6 mmag) periodic variations (4.3 and 2.53 days respectively, with harmonics) which are compatible with periods predicted by theoretical models.

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“…The ionization energy of W + was found in Ref. [3] by means of the same method as here, using the scale factors for the 6s and 6p binding energies determined from the spectrum of Hg + analyzed by Sansonetti and Reader [22] and parametric fitting of the Hg 2+ levels from the ''Atomic Energy Levels'' compilation of C. Moore [23]. Another good reference point is provided by the analyses of Au + [24] and Au 2+ [25], where extensive and thorough parametric fitting was done and the IEs were accurately determined from high members of the Rydberg series.…”

Section: W 7+ (Ho-like) Through W 26+ (Cd-like)mentioning

confidence: 99%