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Second-Order Rotational Effects on Observations of β Cephei Stars

Published online by Cambridge University Press:  12 April 2016

C. A. Engelbrecht (jr)
C. A. Engelbrecht (jr)*
Affiliation:
Department of Physics, University of South Africa, PO Box 392, Pretoria 0001, South Africa

Extract

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Practically all published models of β Cephei (β Cep) stars assume a spherical profile, despite the fact that many actual β Cep stars display high rotation velocities. As a result of the centrifugally altered profile of the surface of a rapidly rotating star, the surface area as well as the surface normal of an arbitrary element on the stellar surface will be modified. Numerical integration over the observed surface elements produces the observed luminosity and radial velocity of such a star. The effect of including the centrifugal distortion of a rotating model β Cep star on its observed characteristics was studied for inclination angles (i) of 0°, 22°.5, 45°, 67°.5 and 90° and equatorial rotation speeds of 0, 80, 160, 240, 320 and 400 km/s, for pulsation modes of order l = 0 to 4.

Type
Part 2. Poster Papers
Information
International Astronomical Union Colloquium , Volume 155: Astrophysical Applications of Stellar Pulsation , 1995 , pp. 313 - 314
Copyright
Copyright © Astronomical Society of the Pacific 1995

References

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