On the behavior of the Cii 4267.261, 6578.052 and 6582.882 Å lines in chemically peculiar and standard stars☆

Catanzaro, G.; Leone, F.

doi:10.1016/s1384-1076(02)00174-4

Cited by 2 publications

(1 citation statement)

References 9 publications

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“…Carbon, nitrogen and oxygen -Three lines of C are useful in the visible range to infer carbon abundance (see for example Catanzaro & Leone 2002), namely: the multiplet at Fig. 3.…”

Section: Abundance Analysismentioning

confidence: 99%

Balmer lines as T$\mathsf{_{eff}}$ and log g indicators for non-solar composition atmospheres

Catanzaro

Leone

Dall³

2004

A&A

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Abstract.Although the importance of a correct abundance assumption in the determination of effective temperature and surface gravity of a star has been demonstrated in the literature, this determination is often still extremely simplified, neglecting the effects of non-solar chemical abundances. In this paper we show how the modeling of the profiles of H δ and H γ , commonly used as T eff and log g indicators, is affected when the chemical composition is far from the standard one. As a target for our study we selected the chemically peculiar star HR 6000. Comparing the observed and synthetic profiles of H δ and H γ we obtained T eff = 12 950 K and log g = 4.05; the atmospheric model has been computed with a metal opacity scale evaluated for [M/H] = −0.5 and He/H = 0. A number of FeII lines have been used to infer the rotational velocity (v e sin i = 0 km s −1 ) and the heliocentric radial velocity (RV = 0.67 km s −1 ). By requiring that the abundance of iron is independent of the 96 measured equivalent widths, we determined the microturubulence velocity (ξ = 0 km s −1 ). The abundance pattern coming from our study is similar to the one inferred from UV lines by Castelli et al. (1985), with the exception of O, Al, Si, Sc and Ni. Possible causes for these descrepancies are discussed. With respect to the Sun, we found the iron peak elements to be normal or overabundant and the light elements, with the exception of Na and P, to be extremely underabundant. We find that HR 6000 is one of the most He-underabundant among the chemically peculiar stars.

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“…Carbon, nitrogen and oxygen -Three lines of C are useful in the visible range to infer carbon abundance (see for example Catanzaro & Leone 2002), namely: the multiplet at Fig. 3.…”

Section: Abundance Analysismentioning

confidence: 99%

Balmer lines as T$\mathsf{_{eff}}$ and log g indicators for non-solar composition atmospheres

Catanzaro

Leone

Dall³

2004

A&A

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The Surface Composition of Six Newly Discovered Chemically Peculiar Stars. Comparison to the HgMn Stars mu Lep and beta Scl and the Superficially Normal B Star nu Cap

Monier,

Niemczura,

Kurtz

et al. 2023

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We report on a detailed abundance study of six bright, mostly southern, slowly rotating late B-stars: HD 1279 (B8III), HD 99803 (B9V), HD 123445 (B9V), HD 147550 (B9V), HD 171961 (B8III), and HD 202671 (B5II/III), hitherto reported as normal stars. We compare them to the two classical HgMn stars μ Lep and β Scl, and to the superficially normal star ν Cap. In the spectra of the six stars, the Hg ii line at 3984 Å line is clearly seen and numerous lines of P, Ti, Mn, Fe, Ga, Sr, Y, and Zr appear to be strong absorbers. A comparison of newly acquired and archival spectra of these objects with a grid of synthetic spectra for selected unblended lines reveals large overabundances of P, Ti, Cr, Mn, Sr, Y, Zr, Ba, Pt, and Hg, and underabundances of He, Mg, Sc, and Ni. The effective temperatures, surface gravities, low projected rotational velocities, and the peculiar abundance patterns of the six investigated stars show that they are new chemically peculiar stars, mostly new HgMn stars, and are reclassified as such. The evolutionary status of these stars has been inferred, and their ages and masses estimated. The two most massive objects, HD 1279 and HD 202671, might have evolved away from the main sequence recently, the other stars are main-sequence objects. HD 99803A is a sharp lined HgMn star with grazing eclipses. From TESS and MASCARA photometry, we determine an orbital period of P orb = 26.12022 ± 0.00004 day.

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On the behavior of the Cii 4267.261, 6578.052 and 6582.882 Å lines in chemically peculiar and standard stars☆

Cited by 2 publications

References 9 publications

Balmer lines as T$\mathsf{_{eff}}$ and log g indicators for non-solar composition atmospheres

Balmer lines as T$\mathsf{_{eff}}$ and log g indicators for non-solar composition atmospheres

The Surface Composition of Six Newly Discovered Chemically Peculiar Stars. Comparison to the HgMn Stars mu Lep and beta Scl and the Superficially Normal B Star nu Cap

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