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Derivation of the Rotational Frequency of Massive Stars from Seismic Studies

Published online by Cambridge University Press:  26 May 2016

C. Aerts ,
R. Scuflaire  and
A. Thoul
C. Aerts
Affiliation:
Institute of Astronomy, Celestijnenlaan 200B, B-3001 Leuven, Belgium
R. Scuflaire
Affiliation:
Institute of Astrophysics and Geophysics, 17 Allée du 6 Août, B-4000 Liège, Belgium
A. Thoul
Affiliation:
Institute of Astrophysics and Geophysics, 17 Allée du 6 Août, B-4000 Liège, Belgium

Abstract

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In this contribution we review the current status of the determination of the rotational frequency in non-radially pulsating B stars, i.e. β Cep stars and slowly pulsating B stars. Considerable progress is currently being made in the understanding of the non-radial oscillations of main-sequence B stars by means of high-temporal, high-spatial resolution spectroscopic time series. This has led to the detection of frequency multiplets, which are interpreted as rotationally splitted non-radial modes and which allow an accurate determination of the surface rotational frequency in some stars. We outline how our future goal, i.e. the derivation of the internal rotation frequency, can be achieved.

Type
Session 1 Observations of Rotating Stars
Information
Symposium - International Astronomical Union , Volume 215: Stellar Rotation , 2004 , pp. 199 - 204
Copyright
Copyright © Astronomical Society of the Pacific 2004 

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