Elemental abundance analyses with DAO spectrograms: XXX. The middle B through early A stars ξ2 Ceti (B9 III), 21 Aquilae (B8 II‐III), ι Aquilae (B5 III), and ι Delphini (A2V)

Adelman, Saul J.; Westbrook, P.C.; Gulliver, A. F.

doi:10.1002/asna.201011347

Cited by 5 publications

(2 citation statements)

References 43 publications

(32 reference statements)

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“…Corresponding author: kyuce@ankara.edu.tr forts to upgrade and make more consistent the analyses continue (see, e. g., Adelman et al 2010Adelman et al , 2011. Adding stars increases the value of the complete set of derived abundances.…”

Section: Introductionmentioning

confidence: 99%

Elemental abundance analyses with DAO spectrograms: XXXII. HR 6455 (A3 III), δ Aqr (A3 V), η Lep (F2 V), and 1 Boo (A1 V)

et al. 2011

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We examine the sharp-lined stars HR 6455 (A3 III, v sin i = 8.7 km s −1 ) and η Lep (F2 V, v sin i = 13.5 km s −1 ) as well as δ Aqr (A3 V, v sin i = 81 km s −1 ) and 1 Boo (A1 V, v sin i = 59 km s −1 ) to increase the number consistently analyzed A and F stars using high dispersion and high S/N (≥200) spectrograms obtained with CCD detectors at the long Coudé camera of the 1.22-m telescope of the Dominion Astrophysical Observatory. Such studies contribute to understanding systematic abundance differences between normal and non-magnetic main-sequence band chemically peculiar A and early F stars. LTE fine analyses of HR 6455, δ Aqr, and 1 Boo using Kurucz's ATLAS suite programs show the same general elemental abundance trends with differences in the metal richness. Light and iron-peak element abundances are generally solar or overabundant while heavy element and rare earth element abundances are overabundant. HR 6455 is an evolved Am star while δ Aqr and 1 Boo show the phenomenon to different extents. Most derived abundances of η Lep are solar.

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Section: Introductionmentioning

confidence: 99%

Elemental abundance analyses with DAO spectrograms: XXXII. HR 6455 (A3 III), δ Aqr (A3 V), η Lep (F2 V), and 1 Boo (A1 V)

et al. 2011

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“…As for literature sources, for Am stars, most of the abundances were taken from Yüce & Adelman (2014) with reference to Ghazaryan et al (2018). Data for other CP types were collected from studies of individual stars or small groupings of stars (Alonso et al 2003;Bailey et al 2014;Folsom et al 2008Folsom et al , 2007Takada-Hidai et al 1986;Cidale et al 2007;Adelman 1989;Adelman et al 2001;Adelman 1994aAdelman , 1988bAdelman & Albayrak 1998;Adelman et al 2006;Adelman 1988aAdelman , 1992Ryabchikova et al 1996;Adelman et al 1997Adelman et al , 1999Adelman 1999;Yüce et al 2011;Adelman 1994b;Adelman et al 2011Adelman et al , 2010. Several elements are well studied and secure, but data for others is sparse.…”

Section: Modelsmentioning

confidence: 99%

Chemically Peculiar Stars in Integrated Light Stellar Population Models and Local Group Galaxies

Worthey¹,

Xiang²

2022

Preprint

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Integrated-light models that incorporate common types of chemically peculiar (CP) stars are assembled using synthetic spectra. Selected spectral features encode significant age information for populations with ages ∼50 Myr < age <∼2 Gyr. Due to the alleviation of template mismatch, the inclusion of CP star features in model spectra improves the accuracy of recovered stellar population parameters, but we are not able to show that new or unique age information can be extracted from the weak CP features compared to continuum fitting and strong-feature strengths, at least at the present state of the art. An age-extraction routine that recovers 2-and 3-burst age structures is employed to analyze the spectra of local group galaxies. NGC 224 (M 31) has a stellar population too old for the types of CP stars we examine. NGC 221 (M 32) also shows no CP spectral features. It appears to contain a component at age ∼1 Gyr at 1% by mass in addition to its dominant 4.7 Gyr population. Unlike SDSS galaxy spectrum averages, NGC 205 (M 110) contains no features due to HgMn stars. This excludes the age range associated with HgMn production, and its near-nuclear spectrum is best fit by a 68±2 Myr population superimposed on an older population with a 1.85±0.1 Gyr component. Both NGC 205 and NGC 221 have an ancient component whose mass is not easy to constrain given the overwhelming light-dominance of the younger populations.

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Elemental Abundance Analyses with DAO Spectrograms. XXXIV. A Three-Dimensional Graphical Examination of the Elemental Abundances of the Mercury-Manganese and Metallic-Line Stars

Yüce

Adelman

2014

Publications of the Astronomical Society of the Pacific

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Detailed analyses of high-dispersion, high signal-to-noise spectra enable astronomers to infer many stellar properties. We study nonmagnetic normal and chemically peculiar B, A, and F stars to understand the details of their optical region abundances via graphical techniques using two kinds of figures for 32 elements. By characterizing the anomalies of the mercury-manganese (HgMn) and the metallic-line (Am) stars, we provide major theoretical tests. We confirmed the known Hg dichotomy between HgMn stars, which are greatly overabundant, and the Am stars with normal abundances. Further P, Ga, Xe, Pt, and Au values were only overabundant for some HgMn stars, and lines of the rare earth elements, such as Sm and Eu, were seen only in some Am and normal stars. These observations might be due in some cases to changes in the major ionization state of atoms in the relevant stellar atmosphere. That some HgMn stars with large Ga overabundances have positions close in the H-R diagram to HgMn stars that lack Ga II lines in the optical region suggests a dichotomy similar to Hg with a boundary close to, but not identical, to that for Hg. The spread of the abundance anomalies for a given element tends to be smaller among the Am stars than among the HgMn stars. Star-to-star differences are superimposed upon abundance trends.

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Elemental abundance analyses with DAO spectrograms: XXX. The middle B through early A stars ξ² Ceti (B9 III), 21 Aquilae (B8 II‐III), ι Aquilae (B5 III), and ι Delphini (A2V)

Cited by 5 publications

References 43 publications

Elemental abundance analyses with DAO spectrograms: XXXII. HR 6455 (A3 III), δ Aqr (A3 V), η Lep (F2 V), and 1 Boo (A1 V)

Elemental abundance analyses with DAO spectrograms: XXXII. HR 6455 (A3 III), δ Aqr (A3 V), η Lep (F2 V), and 1 Boo (A1 V)

Chemically Peculiar Stars in Integrated Light Stellar Population Models and Local Group Galaxies

Elemental Abundance Analyses with DAO Spectrograms. XXXIV. A Three-Dimensional Graphical Examination of the Elemental Abundances of the Mercury-Manganese and Metallic-Line Stars

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