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Latitude distribution of nonradial pulsations in rapidly rotating B stars

Published online by Cambridge University Press:  12 April 2016

S. Jankov ,
P. Mathias ,
A. Domiciano de Souza Jr. ,
K. Uytterhoeven  and
C. Aerts
S. Jankov
Affiliation:
Observatoire de la Côte d’Azur, UMR 6528, F-06304 Nice, France LUAN, UMR 6525, U.N.S.A., Parc Valrose, F-06108, Nice, France Astronomical Observatory, MNTRS 1940, 11050 Beograd, Serbia
P. Mathias
Affiliation:
Observatoire de la Côte d’Azur, UMR 6528, F-06304 Nice, France
A. Domiciano de Souza Jr.
Affiliation:
LUAN, UMR 6525, U.N.S.A., Parc Valrose, F-06108, Nice, France
K. Uytterhoeven
Affiliation:
Institute of Astronomy, Katholieke Universiteit Leuven, Celestijnenlaan 200B, B-3001 Leuven, Belgium
C. Aerts
Affiliation:
Institute of Astronomy, Katholieke Universiteit Leuven, Celestijnenlaan 200B, B-3001 Leuven, Belgium

Abstract

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We present a method for the analysis of latitude distribution associated with temperature and/or velocity perturbations of the stellar surface due to non-radial pulsation (NRP) modes in rapidly rotating B stars. The technique is applied together with Fourier Doppler Imaging (FDI) to high resolution and high signal-to-noise ratio spectroscopic observations of ϵ Per. The main advantage of this approach is that it decomposes complex multi-periodic line profile variations into single components, allowing the detailed analysis of each mode separately. We study the 10.6-d−1 frequency that is particularly important for modal analysis of non-radial pulsations in the star.

Type
Part 4. Early-type stars: B, A and F pulsators
Information
International Astronomical Union Colloquium , Volume 193: Variable Stars in the Local Group , 2004 , pp. 204 - 207
Copyright
Copyright © Astronomical Society of the Pacific 2004

References

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