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Pulsation of Rotating Magnetic Stars

Published online by Cambridge University Press:  15 February 2018

H. Shibahashi  and
M. Takata
H. Shibahashi
Affiliation:
Department of Astronomy, University of Tokyo, Japan
M. Takata
Affiliation:
Department of Astronomy, University of Tokyo, Japan

Extract

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Recently, one of the rapidly oscillating Ap stars, HR 3831, has been found to have an equally split frequency septuplet, though its oscillation seems to be essentially an axisymmetric dipole mode with respect to the magnetic axis which is oblique to the rotation axis (Kurtz et al. 1992; Kurtz 1992). In order to explain this fine structure, we investigate oscillations of obliquely rotating magnetic stars by taking account of the perturbations due to the magnetic fields and the rotation. We suppose that the star is rigidly rotating and that the magnetic field is a dipole field and its axis is oblique to the rotation axis. We treat the effects of the rotation and of the magnetic field as perturbations. In doing so, we suppose that the rotation of the star is slow enough so that the effect of the rotation on oscillations is smaller than that of the magnetic field.

Type
Stellar Seismology
Information
International Astronomical Union Colloquium , Volume 139: New Perspectives on Stellar Pulsation and Pulsating Variable Stars , 1993 , pp. 134
Copyright
Copyright © Cambridge University Press 1993

References

Kurtz, D. W. 1992, MNRAS, in press.Google Scholar
Kurtz, D. W., Kanaan, A., and Martinez, P. 1992, MNRAS, in press.Google Scholar
Shibahashi, H., and Takata, M. 1992, in Inside the Stars, Proc IAU Colloq. No. 137, ed. W.W. Weiss & A. Baglin, Astron. Soc. of Pacific Conf. Series, in press.Google Scholar