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Comparison of Different Methods for Determining Atmospheric Parameters of A and F Stars

Published online by Cambridge University Press:  12 April 2016

B. Smalley  and
M.M. Dworetsky
B. Smalley
Affiliation:
Department of Physics & Astronomy, University College London, Gower Street, London WC1E 6BT, United Kingdom
M.M. Dworetsky
Affiliation:
Department of Physics & Astronomy, University College London, Gower Street, London WC1E 6BT, United Kingdom

Abstract

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The atmospheric parameters of metallic-lined (Am) stars have been the subject of much debate. Using spectrophotometric flux fitting, Lane & Lester (1984) obtained values of Teff and log g for several classical Am stars that were systematically lower than those obtained by Dworetsky & Moon (1986), who used empirically calibrated uvbyß photometry. We have used the standard procedures of photometry, spectrophotometry and hydrogen-line profile fitting to determine the atmospheric parameters of many A and F stars, including several Am stars. Modifications to the standard techniques have been used to allow for the effects of cooler companion stars in the determination of such parameters. It is found that spectrophotometric methods give results for Teff and log g that are highly sensitive to the adopted metal abundance. This explains the anomalous results of Lane & Lester.

Type
I. General Properties of CP Stars
Information
International Astronomical Union Colloquium , Volume 138: Peculiar versus Normal Phenomena in A-Type and Related Stars , 1993 , pp. 182 - 186
Copyright
Copyright © Astronomical Society of the Pacific 1993

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