Volume 406, Number 1, July IV 2003
|Page(s)||273 - 280|
|Section||Stellar structure and evolution|
|Published online||17 November 2003|
Surface imaging of stellar non-radial pulsations
I. Inversions of simulated data
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
Corresponding author: S. V. Berdyugina, firstname.lastname@example.org
Accepted: 13 May 2003
We investigate capability of the stellar surface imaging technique for studying stellar non-radial pulsations on the basis of inversions of time series of variable line profiles without making assumptions on the specific shape of the pulsations. The inversion results in an image of the stellar surface in which sectoral and tesseral modes can be distinguished in many cases, and the pulsational degree and the azimuthal order can be determined. We find that sectoral and tesseral modes with (or any even number) can be successfully restored under various conditions (different inclinations of the rotational axis, surface temperature or velocity fluctuations due to pulsations). Tesseral modes with (or any odd number) do not show significant line profile variations at higher inclinations of the rotational axis, and, thus, no information can be recovered from line profiles. At lower inclinations, only the azimuthal order of such modes can be recovered. We conclude that stellar surface imaging is a useful technique for pulsation-mode identification.
Key words: stars: imaging / stars: oscillations
© ESO, 2003
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