Volume 406, Number 1, July IV 2003
|Page(s)||281 - 285|
|Section||Stellar structure and evolution|
|Published online||17 November 2003|
Surface imaging of stellar non-radial pulsations*
II. The β Cephei star ω1 Sco
Astronomy Division, University of Oulu, PO Box 3000, 90401 Oulu, Finland
2 Institute of Astronomy, ETHZ, 8092 Zurich, Switzerland
3 Nordic Optical Telescope, Apartado 474, 38700 S/C de La Palma, Canarias, Spain
4 Astrophysical Institute Potsdam, An der Sternwarte 16, 14482 Potsdam, Germany
5 Astronomical Institute Anton Pannekoek, University of Amsterdam, Kruislaan 403, 1098 SJ Amsterdam, The Netherlands
Corresponding author: S. V. Berdyugina, firstname.lastname@example.org
Accepted: 13 May 2003
We apply the surface imaging technique to high-resolution spectra of the rapidly rotating β Cep-type star ω1 Sco which shows strong line-profile variations in the λ 4552, 4567, 4574 Å triplet. These variations have been interpreted in terms of non-radial pulsations by Telting & Schrijvers (1998). Their analysis of the spectral time series with traditional Fourier transforms resulted in one significant frequency, suggesting that the profile variations are due to only one dominant pulsation mode. Here we apply a spectral inversion technique to the same time series of the profiles. Assuming only temperature fluctuations due to pulsations, we obtain an image of the dominant pulsation mode. We estimate the pulsation degree from the image, put constraints on the azimuthal number of the mode, and study the latitudinal distribution of the pulsation pattern. In addition to the known dominant mode we find traces of a second pulsation mode.
Key words: stars: oscillations / stars: imaging / stars: early-type / stars: individual: ω1 Sco
© ESO, 2003
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