期刊
ASTRONOMY & ASTROPHYSICS
卷 542, 期 -, 页码 -出版社
EDP SCIENCES S A
DOI: 10.1051/0004-6361/201118548
关键词
stars: oscillations; stars: early-type; stars: individual: HD 50230; techniques: photometric
资金
- Fund for Scientific Research of Flanders (FWO), Belgium
- Research Council of K.U. Leuven, Belgium
- Fonds National de la Recherche Scientifique (FNRS), Belgium
- Royal Observatory of Belgium
- Observatoire de Geneve, Switzerland
- Thuringer Landessternwarte Tautenburg, Germany
- European Research Council under the European Community [227224 (PROSPERITY)]
- Belgian PRODEX Office [C90309]
- National Science Foundation of the United States [NSF PHY05-51164]
Context. B-type stars are promising targets for asteroseismic modelling, since their frequency spectrum is relatively simple. Aims. We deduce and summarise observational constraints for the hybrid pulsator, HD 50230, earlier reported to have deviations from a uniform period spacing of its gravity modes. The combination of spectra and a high-quality light curve measured by the CoRoT satellite allow a combined approach to fix the position of HD 50230 in the HR diagram. Methods. To describe the observed pulsations, classical Fourier analysis was combined with short-time Fourier transformations and frequency spacing analysis techniques. Visual spectra were used to constrain the projected rotation rate of the star and the fundamental parameters of the target. In a first approximation, the combined information was used to interpret multiplets and spacings to infer the true surface rotation rate and a rough estimate of the inclination angle. Results. We identify HD 50230 as a spectroscopic binary and characterise the two components. We detect the simultaneous presence of high-order g modes and low-order p and g-modes in the CoRoT light curve, but were unable to link them to line profile variations in the spectroscopic time series. We extract the relevant information from the frequency spectrum, which can be used for seismic modelling, and explore possible interpretations of the pressure mode spectrum.
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