Volume 425, Number 1, October I 2004
|Page(s)||171 - 177|
|Section||Stellar structure and evolution|
|Published online||10 September 2004|
Department of Astronomy, Sejong University, Seoul, 143-747, Korea e-mail: email@example.com; firstname.lastname@example.org
2 Odessa Astronomical Observatory, Odessa National University, Park Shevchenko, Odessa, 65014, Ukraine e-mail: email@example.com; firstname.lastname@example.org
3 Deceased (Institute of Astronomy, Russian Academy of Sciences, Pyatnitskaya ul. 48, Moscow, 109017, Russia)
4 The W. J. McDonald Observatory, University of Texas, Austin, TX 78712, USA e-mail: email@example.com
5 Department of Earth Science Education, Chonbuk National University, Chonju 561-756, Korea e-mail: firstname.lastname@example.org
Accepted: 25 May 2004
We report the results of abundance determinations for the components of the SB2 star HD 153720 from high resolution () echelle high signal-to-noise spectra of the wavelength region 3595-10 260 Å taken with the 2.7 m telescope of the McDonald Observatory We found the values of the atmospheric parameters of the primary to be effective temperature = 7425 K and surface gravity = 4.0 cgs, and of the secondary to be = 7125 K and = 3.9 cgs. The microturbulent velocity is = 2.7 for both components, and the projected rotational velocity is = 15 also for both components. The abundances of about 20 elements were determined with the method of spectrum synthesis. The components of HD 153720 are metallic-line stars. Possible inconsistencies between old and new measurements of radial velocities may be explained by the existence of third body in this system. A review of recent high resolution spectral observations of eight A4-F1 binaries shows that only one of these systems can be classified as normal.
Key words: stars: abundances / stars: atmospheres / stars: evolution / stars: chemically peculiar / stars: binaries: spectroscopic / stars: individual: HD 153720
© ESO, 2004
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