EDP Sciences
Free Access
Volume 406, Number 3, August II 2003
Page(s) 975 - 980
Section Stellar atmospheres
DOI https://doi.org/10.1051/0004-6361:20030620

A&A 406, 975-980 (2003)
DOI: 10.1051/0004-6361:20030620

Elemental abundance analyses with DAO spectrograms

XXVII. The superficially normal stars  $\theta$ And (A2 IV), $\epsilon$ Del (B6 III), $\epsilon$ Aqr (A1.5 V), and $\iota$ And (B9 V)
D. Kocer1, S. J. Adelman2, 3, H. Caliskan4, A. F. Gulliver3, 5 and H. Gokmen Tektunali4

1  Department of Mathematics and Computer Science, Faculty of Science & Letters, $\dot{\rm I}$stanbul Kültür University, E5 Karayolu Üzeri, 34510, Sirinevler, $\dot{\rm I}$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, $\dot{\rm I}$stanbul University, 34452 University, $\dot{\rm I}$stanbul, Turkey
5  Department of Physics, Brandon University, Brandon, MB R7A 6A9 Canada

(Received 31 March 2003 / Accepted 24 April 2003 )

The superficially normal stars  $\theta$ And (A2 V), $\epsilon$ Del (B6 III), $\epsilon$ Aqr (A1.5 V), and  $\iota$ 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 $S/N \ge 200$. 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  $\theta$ And suggest that it is possibly a fast rotating Am star.

Key words: stars: abundances -- stars: individual: $\theta$ And -- stars: individual: $\epsilon$ Del -- stars: individual: $\epsilon$ Aqr -- stars: individual: $\iota$ And

Offprint request: D. Kocer, d.kocer@iku.edu.tr

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