Issue |
A&A
Volume 406, Number 1, July IV 2003
|
|
---|---|---|
Page(s) | 281 - 285 | |
Section | Stellar structure and evolution | |
DOI | https://doi.org/10.1051/0004-6361:20030747 | |
Published online | 17 November 2003 |
Surface imaging of stellar non-radial pulsations*
II. The β Cephei star ω1 Sco
1
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, sveta@astro.phys.ethz.ch
Received:
10
February
2003
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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