On the relationship between the mercury-manganese stars and the metallic-lined stars

Adelman, Saul J.; Adelman, A. S.; Pintado, O. I.

doi:10.1051/0004-6361:20021475

Cited by 51 publications

(62 citation statements)

References 25 publications

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“…He-weak stars lie on the main sequence and have T eff approximately between 14 000 and 20 000 K. Since observational abundance determinations are much less prevalent for He-weak stars than for HgMn stars, we will only focus on the abundances of 3 Cen A given in Adelman & Pintado (2000).…”

Section: He-weak Starsmentioning

confidence: 99%

Radiative accelerations in stellar atmospheres

Hui-Bon-Hoa

Leblanc

Hauschildt

et al. 2002

A&A

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Abstract. We present calculations of radiative accelerations obtained with the general purpose model atmosphere code PHOENIX. The accelerations are computed simultaneously for all the elements He-Ga; Kr-Nb; Ba; La, using the opacity sampling method. The calculations are mainly performed with the LTE approximation. Tests are made to evaluate the influence of non-LTE effects and the validity of the radiative flux obtained through the diffusion approximation. It is shown that the abundances supported in the atmospheres of HgMn and He-weak stars are generally consistent with those observed.

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Section: He-weak Starsmentioning

confidence: 99%

Radiative accelerations in stellar atmospheres

Hui-Bon-Hoa

Leblanc

Hauschildt

et al. 2002

A&A

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“…BRH show that this variation occurs because of helium-rich and helium-poor areas on the stellar surface, which they have mapped using Doppler imaging. Interestingly, BRH identify 3 He, found in other helium-weak stars such as the highly unusual phosphorus-gallium star 3 Cen A (Castelli et al 1997;Adelman & Pintado 2000).…”

Section: Introductionmentioning

confidence: 94%

Lanthanides and other spectral oddities in a Centauri

Cowley

Hubrig

González

2010

A&A

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Context. There is considerable interest in the helium variable a Cen as a bridge between helium-weak and helium-strong CP stars.Aims. We investigate Ce iii and other possible lanthanides in the spectrum the of hottest chemically peculiar (CP) star in which these elements have been found. A Kr ii line appears within a broad absorption which we suggest may be due to a high-level transition in C ii.Methods. Wavelengths and equivalent widths are measured on high-resolution UVES spectra, analyzed, and their phase-variations investigated.Results. New, robust identifications of Ce iii and Kr ii are demonstrated. Nd iii is likely present. A broad absorption near λ4619 is present at all phases of a Cen, and in some other early B stars. Conclusions. The presence of lanthanides in a Cen strengthens the view that this star is a significant link between the cooler CP stars and the hotter helium-peculiar stars. Broad absorptions in a Cen are not well explained.

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“…Elements beyond the iron peak when observed are overabundant. When we have performed statistically sufficient additional abundance analyses of HgMn stars, we will again perform a correlation of abundance analysis (see, e.g., Adelman et al 2001Adelman et al or 2003.…”

Section: The Abundance Analysesmentioning

confidence: 99%

Elemental abundance analyses with DAO spectrograms

Adelman

Caliskan

Gulliver

et al. 2006

A&A

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We performed elemental abundances analyses of the mercury-manganese (HgMn) stars 53 Tau, β Tau, and γ Crv consistent with previous studies of similar stars in this series. The derived v sin i values for the last two stars are 59 and 32 km s −1 , respectively, both of which are greater than those of HgMn stars previously studied. For 53 Tau this analysis using selected wavelength regions replaces one performed with coadded photographic spectra. A stricter upper limit is placed on any Hg II λ3984 line. The abundances of β Tau are usually greater than those of γ Crv. But the later star has a Hg II λ3984 line which the former lacks. Our analysis of υ Her, which was performed with spectrograms obtained with CCD detectors, is extended by using additional spectrograms to increase the range of wavelengths covered longward of λ4800. Minor changes in the derived abundances result.

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On the relationship between the mercury-manganese stars and the metallic-lined stars

Cited by 51 publications

References 25 publications

Radiative accelerations in stellar atmospheres

Radiative accelerations in stellar atmospheres

Lanthanides and other spectral oddities in a Centauri

Elemental abundance analyses with DAO spectrograms

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