Isotopic abundances of HG in mercury stars inferred from the HG II line at 3984 A

White, R. E.; Vaughan, A. H.; Preston, George W.; Swings, Jean-Pierre

doi:10.1086/154157

Cited by 57 publications

(40 citation statements)

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“…The relative abundances of iron-peak elements vary from star to star, but Mn is generally overabundant up to 3 dex. Abnormal variations in the relative isotopic abundances of Hg and Pt from star to star have been detected a few decades ago (e.g., White et al 1976;Dworetsky & Vaughan 1973). Hg and Pt lines in many HgMn stars are shifted with respect to the centroids of the terrestrial Hg and Pt lines.…”

Section: Introductionmentioning

confidence: 99%

The Ca II infrared triplet as indicator of anomalous Ca isotopic mixture in HgMn stars

Castelli

Hubrig

2004

A&A

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Abstract.For the first time we present observational evidence for an anomalous isotopic structure of Ca  in mercury-manganese (HgMn) stars. The centroid wavelengths of Ca  infrared triplet lines in a number of stars have been found redshifted with respect to the centroids of the terrestrial Ca  lines. The record holder is the star HD 175640 for which the measured wavelength is consistent with Ca  being present in the atmosphere entirely in form of the heaviest stable isotope 48 Ca. This is a very striking result as 48 Ca makes up only 0.187% of the terrestrial Ca mixture.

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Section: Introductionmentioning

confidence: 99%

The Ca II infrared triplet as indicator of anomalous Ca isotopic mixture in HgMn stars

Castelli

Hubrig

2004

A&A

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“…Firstly noted by White et al (1976), the anti-correlation existing between q and T eff was confirmed by Smith (1997). Referring to Fig.…”

Section: Mercurymentioning

confidence: 71%

“…The profile of Hg λ3984 Å can be a blend of seven stable isotopes of mercury (A = 196, 198, 199, 200, 201, 202, 204) of which those with odd isotope numbers are further split into hyperfine components (Dworetsky et al 1970). It is commonly accepted that the isotopic mixture can be characterized according to the q parameter formalism introduced by White et al (1976). In this formalism q ranges from 0, corresponding to the terrestrial mixture, to 4 for pure 204 Hg.…”

Section: Mercurymentioning

confidence: 99%

HD 191110 a SB2 system with HgMn and Hg components

Catanzaro¹,

Leone²,

Leto

2003

A&A

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Abstract. In this paper we present the first quantitative abundance analysis of the SB2 system with HgMn and Hg components HD 191110. Time-resolved (R = 14 000) spectroscopic observations of this system have been obtained during September and October 2002 at the Catania Astrophysical Observatory. Combining these observations with spectra (R = 50 000-110 000) taken from the CFHT archive, we refined the orbital period of this system (P = 9.34661 ± 0.00002 d) and then we recalculated the fundamental parameters characterizing its orbit. From the fit of the H β profiles, obtained at different orbital phases, we determined the effective temperatures and surface gravities of each component and the light ratio: T A eff = 11 000 K, log g A = 3.60, T B eff = 10 700 K, log g B = 3.90, L A /L B = 1.20. Regarding the chemical composition, both components have solar abundances of sulfur, titanium and iron; magnesium and silicon are slightly underabundant; platinum and yttrium are overabundant. Manganese lines have been detected only in the spectrum of the primary. As to rare-earths, two lines of Nd have been identified in the secondary's spectrum. Other lines we identified in our spectra belong to P, Cr, Ni, Sr, Zr and Au. We also discuss the isotopic structure of the Hg λ3983.9 Å line.

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“…As a result of atomic structure there was shown to be a relationship between the shift in the center of gravity of specific spectral lines of Pt ii and Hg ii with isotope composition. The q-formalism was introduced by White et al (1976), quantifying the shift for the line Hg ii λ3984. The q-formalism was useful for many years and is still a useful indicator of the Hg isotopic composition for low to medium resolution spectroscopy.…”

Section: Isotopic Anomaliesmentioning

confidence: 99%

Observations of nonmagnetic CP stars: crossing boundaries

Wahlgren¹

2004

Proc. IAU

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Abstract.Observations of chemically peculiar (CP) stars have been conducted for decades and have revealed a variety of spectrum anomalies, most prominent among them are line enhancements of heavy elements. The earlier observations were limited to the optical region and the use of less sensitive detectors, yet are responsible for much of our current characterization of the CP star phenomenon. More recent observations embrace a wider expanse of the electromagnetic spectrum and employ more sensitive detectors that continue to unveil new levels of spectrum peculiarity. The traditional criteria used to distinguish normal from peculiar stars have become blurred, thus in some sense replacing the concept of peculiarity with one of continuity. This presentation will address the observations of the traditional nonmagnetic CP star groups over the past decade, paying particular attention to new avenues of research that have a bearing upon the interpretation of the atmospheres of CP stars and the origins of this phenomenon.

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Isotopic abundances of HG in mercury stars inferred from the HG II line at 3984 A

Cited by 57 publications

References 0 publications

The Ca II infrared triplet as indicator of anomalous Ca isotopic mixture in HgMn stars

The Ca II infrared triplet as indicator of anomalous Ca isotopic mixture in HgMn stars

HD 191110 a SB2 system with HgMn and Hg components

Observations of nonmagnetic CP stars: crossing boundaries

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