Volume 406, Number 3, August II 2003
|Page(s)||975 - 980|
|Section||Stellar structure and evolution|
|Published online||17 November 2003|
Elemental abundance analyses with DAO spectrograms*
XXVII. The superficially normal stars θ And (A2 IV), ϵ Del (B6 III), ϵ Aqr (A1.5 V), and ι And (B9 V)
Department of Mathematics and Computer Science, Faculty of Science & Letters, stanbul Kültür University, E5 Karayolu Üzeri, 34510, Şirinevler, stanbul, Turkey
2 Department of Physics, The Citadel, 171 Moultrie Street, Charleston, SC 29409, USA
3 Guest Investigator, Dominion Astrophysical Observatory, Herzberg Institute of Astrophysics, National Research Council of Canada, 5071 W. Saanich Road, Victoria, BC, V9E 2E7 Canada
4 Department of Astronomy and Space Sciences, stanbul University, 34452 University, stanbul, Turkey
5 Department of Physics, Brandon University, Brandon, MB R7A 6A9 Canada
Corresponding author: D. Kocer, firstname.lastname@example.org
Accepted: 24 April 2003
The superficially normal stars θ And (A2 V), ϵ Del (B6 III), ϵ Aqr (A1.5 V), and ι And (B9 V), which have rotationally broadened line profiles, are analyzed in a manner consistent with previous studies of this series using 2.4 Å mm-1 spectrograms obtained with CCD detectors and . Their variable radial velocities strongly suggest they are spectroscopic binaries. As no evidence is seen for lines of their companions they are analyzed as single stars. Their derived abundances are generally near solar. But those for θ And suggest that it is possibly a fast rotating Am star.
Key words: stars: abundances / stars: individual: θ And / stars: individual: ϵ Del / stars: individual: ϵ Aqr / stars: individual: ι And
© ESO, 2003
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