R-Andromedae and the Method of Wavelength Coincidence Statistics

Cowley, C. R.; Hensberge, H.

doi:10.1086/158702

Cited by 18 publications

(15 citation statements)

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“…A subset of the measurements, excluding lines longer than 1 micron were then subjected to analysis by wavelength coincidence statistics (WCS, cf. Cowley & Hensberge 1981). The spectra of Br II and V II were found in this survey.…”

Section: Introductionmentioning

confidence: 62%

Abundances of vanadium and bromine in 3 Centauri A

Cowley¹,

Wahlgren²

2006

A&A

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Section: Introductionmentioning

confidence: 62%

Abundances of vanadium and bromine in 3 Centauri A

Cowley¹,

Wahlgren²

2006

A&A

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“…Several methods were used to establish the zero point of the stellar atomic lines. Most commonly, a radial velocity scan was performed, using wavelength coincidence statistics (Cowley & Hensberge 1981) for the atomic species expected to be strongly present. The radial velocity of the star was taken to be that which gave the most highly significant results.…”

Section: Wavelength Determination and Accuracymentioning

confidence: 99%

The calcium isotopic anomaly in magnetic CP stars

Cowley

Hubrig

2005

A&A

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Abstract. Chemically peculiar stars in the magnetic sequence can show the same isotopic anomaly in calcium previously discovered for mercury-manganese stars in the non-magnetic sequence. In extreme cases, the dominant isotope is the exotic 48 Ca.Measurements of Ca  lines arising from 3d−4p transitions reveal the anomaly by showing shifts up to 0.2 Å for the extreme cases -too large to be measurement errors. We report measurements of miscellaneous objects, including two metal-poor stars, two apparently normal F-stars, an Am-star, and the N-star U Ant. Demonstrable anomalies are apparent only for the Ap stars.The largest shifts are found in rapidly oscillating Ap stars and in one weakly magnetic Ap star, HD 133792. We note the possible relevance of these shifts for the GAIA mission.

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“…Thus 0.05 corresponds to the 95 per cent confidence level, which is often taken as the threshold of significance. Cowley & Hensberge (1981) give a detailed summary of the method of WCS. Current techniques are somewhat more versatile than those used at that time because digitized stellar intensities are available.…”

Section: Wavelength Identificationsmentioning

confidence: 99%

Abundances in Przybylski's star

Cowley¹,

Ryabchikova²,

Kupka³

et al. 2000

Monthly Notices of the Royal Astronomical Society

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We have derived abundances for 54 elements in the extreme roAp star HD 101065. ESO spectra with a resolution of about 80 000, and S/N of 200 or more were employed. The adopted model has Teff=6600 K, and log(g)=4.2. Because of the increased line opacity and consequent low gas pressure, convection plays no significant role in the temperature structure. Lighter elemental abundances through the iron group scatter about standard abundance distribution (SAD) (solar) values. Iron and nickel are about one order of magnitude deficient while cobalt is enhanced by 1.5 dex. Heavier elements, including the lanthanides, generally follow the solar pattern but enhanced by 3 to 4 dex. Odd‐Z elements are generally less abundant than their even‐Z neighbours. With a few exceptions (e.g. Yb), the abundance pattern among the heavy elements is remarkably coherent, and resembles a displaced solar distribution.

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R-Andromedae and the Method of Wavelength Coincidence Statistics

Cited by 18 publications

References 0 publications

Abundances of vanadium and bromine in 3 Centauri A

Abundances of vanadium and bromine in 3 Centauri A

The calcium isotopic anomaly in magnetic CP stars

Abundances in Przybylski's star

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