Volume 386, Number 1, April IV 2002
|Page(s)||280 - 285|
|Section||Interstellar and circumstellar matter|
|Published online||15 April 2002|
Constraining the difference in convective blueshift between the components of α Centauri with precise radial velocities
Institut d'Astronomie et d'Astrophysique, Université Libre de Bruxelles, C.P. 226, Boulevard du Triomphe, 1050 Bruxelles, Belgium
2 Department of Astrophysical Sciences, Princeton University, Princeton NJ 08544-1001, USA
3 Department of Physics and Astronomy, San Francisco State University, CA 94132, USA
4 Department of Terrestrial Magnetism, Carnegie Institution of Washington, 5241 Broad Branch Road NW, Washington DC 20015-1305, USA
5 Anglo–Australian Observatory, PO Box 296, Epping, NSW 1710, Australia
6 Department of Astronomy, University of California, Berkeley, CA 94720, USA
7 Astrophysics Research Institute, Liverpool John Moores University, Twelve Quays House, Egerton Wharf Birkenhead CH41 1LD, UK
8 Rutherford Appleton Laboratory, Chilton, Didcot, Oxon, OX11 0QX, UK
9 Faculty of Sciences, University of Southern Queensland, Toowoomba, 4350, Australia
10 Observatoire de Genève, 1290 Sauvergny, Switzerland
11 Mount John University Observatory, Department of Physics and Astronomy, University of Canterbury, Orivate Bag 4800, Christchurch, New Zealand
Corresponding author: D. Pourbaix, email@example.com
Accepted: 20 February 2002
New radial velocities of α Cen A & B obtained in the framework the Anglo-Australian Planet Search programme as well as in the CORALIE programme are added to those by Endl et al. ([CITE]) to improve the precision of the orbital parameters. The resulting masses are and for A and B respectively. The factors limiting how accurately these masses can be derived from a combined visual-spectroscopic solution are investigated. The total effect of the convective blueshift and the gravitational redshift is also investigated and estimated to differ by m s-1 between the components. This suggests that the difference in convective blueshift between the components is much smaller than predicted from current hydrodynamical model atmosphere calculations.
Key words: stars: binaries: general / stars: individual: α Cen / methods: data analysis
© ESO, 2002
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