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Published Online May 29, 2003
Science DOI: 10.1126/science.1084993

Reports

Submitted on March 27, 2003
Accepted on May 14, 2003

Asteroseismology of HD 129929: Core Overshooting and Nonrigid Rotation

C. Aerts 1*, A. Thoul 2, J. Daszynska 3, R. Scuflaire 2, C. Waelkens 1, M. A. Dupret 2, E. Niemczura 4, A. Noels 2

1 Instituut voor Sterrenkunde, Katholieke Universiteit Leuven, Celestijnenlaan 200 B, B-3001 Leuven, Belgium.
2 Institut d'Astrophysique et Géophysique, Université de Liège, allée du Six Août 17, B-4000 Liège, Belgium.
3 Instituut voor Sterrenkunde, Katholieke Universiteit Leuven, Celestijnenlaan 200 B, B-3001 Leuven, Belgium; Astronomical Institute of the Wroclaw University, ul. Kopernika 11, 51-622 Wroclaw, Poland.
4 Astronomical Institute of the Wroclaw University, ul. Kopernika 11, 51-622 Wroclaw, Poland.

* To whom correspondence should be addressed. E-mail: conny{at}ster.kuleuven.ac.be.

We have gathered and analyzed 1493 high-quality multicolor Geneva photometric data (obtained with the Swiss 0.7-meter telescope at La Silla Observatory, Chile) taken over 21 years of the B3V star HD 129929. We detect six frequencies, among which appear the effects of rotational splitting with a spacing of ~0.0121 cycles per day, implying that the star rotates very slowly. A nonadiabatic analysis of the oscillations allows us to constrain the metallicity of the star to Z {epsilon} [0.017,0.022], which agrees with a similar range derived from spectroscopic data. We provide evidence for the occurrence of core convective overshooting in the star, with {alpha}ov = 0.10 ± 0.05, and we rule out rigid rotation.




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Science. ISSN 0036-8075 (print), 1095-9203 (online)