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How to interpret LPV in roAp stars

Published online by Cambridge University Press:  02 March 2005

H. Shibahashi ,
D.W. Kurtz ,
E. Kambe  and
D.O. Gough
H. Shibahashi
Affiliation:
Department of Astronomy, University of Tokyo, Tokyo 113-0033, Japan email: shibahashi@astron.s.u-tokyo.ac.jp
D.W. Kurtz
Affiliation:
Centre for Astrophysics, University of Central Lancashire, Preston PR1 2HE, UK
E. Kambe
Affiliation:
Department of Earth and Ocean Sciences, National Defense Academy, Yokosuka, Kanagawa 239-8686, Japan
D.O. Gough
Affiliation:
Institute of Astronomy, Madingley Road, Cambridge, CB3 0HA, UK
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Abstract

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Recent spectroscopic observations of roAp stars with high spectral resolution and high time resolution show line profile variations (LPV) which seem to be similar to those seen in rapidly rotating B-type line-profile variables. At first glance these line profile variations seem to be in disagreement with the mode identification based on the photometric observations. We propose an interpretation according to which the observed line profile variations are a manifestation of a shock wave in the high atmosphere near the magnetic polar regions, and show that the line profile variations can be still understood in the framework of the oscillation mode being consistent with the photometric observations.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Keywords

Stars: chemically peculiarstars: oscillationsstars: variables: otherline: profiles
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2004 , Issue IAUS224 , July 2004 , pp. 829 - 834
Copyright
© 2004 International Astronomical Union