Elemental abundance analyses with DAO spectrograms - XXIII. The superficially normal stars 28 And (A7 III) and 99 Her (F7 V)

Adelman, Saul J.; Caliskan, H.; Kocer, D.; Çay, İpek H.; Tektunali, H. G.

doi:10.1046/j.1365-8711.2000.03577.x

Cited by 21 publications

(11 citation statements)

References 33 publications

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“…We used the abundances of non-variable F-and A-type stars published by Adelman et al (1997Adelman et al ( , 2000, Erspamer & North (2003) and Hill (1995), to generate a typical abundance pattern for stars of similar spectral types. From a direct comparison, we showed that the mean abundance pattern of our sample of δ Scuti stars and of the non-variable F-and A-type stars are comparable.…”

Section: Discussionmentioning

confidence: 99%

Abundance analysis of seven δ Scuti stars

Fossati

Kolenberg

Reegen

et al. 2008

A&A

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Context. The current knowledge of the abundance pattern in δ Scuti stars is based on the analysis of just a few field stars. Aims. We aim to determine the general chemical properties of the atmospheres of δ Scuti stars based on a statistically relevant sample of stars and will investigate whether the abundance pattern is close to solar, an assumption generally made for pulsation models. Methods. We have analysed high-resolution, high signal-to-noise ratio spectra of seven field δ Scuti stars. We derived the fundamental parameters and the photospheric abundances and compared them to a similar sample of cluster δ Scuti stars. Results. With the use of a t-test we demonstrated that there is no difference between the two samples, which allows us to merge them, resulting in a sample of fifteen δ Scuti stars. We did not find any substantial difference between the abundance pattern of our sample of δ Scuti stars and a sample of normal early A-and late F-type stars. One field star in our sample, HD 124953, is most likely a pulsating Am star.

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Section: Discussionmentioning

confidence: 99%

Abundance analysis of seven δ Scuti stars

Fossati

Kolenberg

Reegen

et al. 2008

A&A

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“…Clearly, up to about 10 500 K abundances increase with temperature, which immediately calls for another investigation: is there a similar trend for normal stars and/or is this trend artificially caused by incorrect model atmospheres and spectrum reduction techniques? For this purpose we compiled Cr and Fe abundances for normal, superficially-normal, Am and δ Scuti-type stars with low rotational velocities (v e sin i < 50 km s −1 ) from papers by Varenne & Monier (1999, Hyades A and F stars), Hill & Landstreet (1993), Mittermayer & Weiss (2003), and from numerous papers by Adelman and co-workers: Adelman (1991, 1994, 1996, Adelman & Davis Philip (1992), Adelman et al (1997Adelman et al ( , 2000Adelman et al ( , 2001, , Adelman & Albayrak (1998), Pintado & Adelman (2003), and Kocer et al (2003).…”

Section: Spectroscopic Signature Of Roap Starsmentioning

confidence: 99%

The spectroscopic signature of roAp stars

Ryabchikova¹,

Nesvacil

Weiß³

et al. 2004

A&A

117

162

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Abstract.To reliably determine the spectroscopic signature of rapidly oscillating chemically peculiar (roAp) stars it is also necessary to investigate a sample of non pulsating chemically peculiar (noAp) as well as presumably "normal" stars. We describe in this study the sample of spectroscopically investigated stars and comment on the techniques used for the analysis. In particular we discuss ionization disequilibria of rare earths in roAp stars that distinguish them from noAp stars. In the light of the recently discovered pulsation of β CrB we see arguments that all magnetic CP2 stars up to a transition temperature of about 8100 K may be pulsating.

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“…The reasoning applied to E s is the same here as it is for example (5). In a procedure that is intermediate between this example and example (5), values of f s + E s and f are compared without subtraction (see, for example, Adelman et al 2000). Examples of this kind of analysis are given by Klochkova & Panchuk (1987, 1990).…”

Section: ) Differential Analysis (Relative To the Sun)mentioning

confidence: 99%

Statistical cataloging of archival data for luminosity class IV–V stars

Taylor

2003

A&A

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Abstract. This paper describes the derivation of an updated statistical catalog of metallicities. The stars for which those metallicities apply are of spectral types F, G, and K, and are on or near the main sequence. The input data for the catalog are values of [Fe/H] published before 2002 February and derived from lines of weak and moderate strength. The analyses used to derive the data have been based on one-dimensional LTE model atmospheres. Initial adjustments which are applied to the data include corrections to a uniform temperature scale which is given in a companion paper (see Taylor 2003). After correction, the data are subjected to a statistical analysis. For each of 941 stars considered, the results of that analysis include a mean value of [Fe/H], an rms error, an associated number of degrees of freedom, and one or more identification numbers for source papers. The catalog of these results supersedes an earlier version given by Taylor (1994b).

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Elemental abundance analyses with DAO spectrograms - XXIII. The superficially normal stars 28 And (A7 III) and 99 Her (F7 V)

Cited by 21 publications

References 33 publications

Abundance analysis of seven δ Scuti stars

Abundance analysis of seven δ Scuti stars

The spectroscopic signature of roAp stars

Statistical cataloging of archival data for luminosity class IV–V stars

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