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Doppler Imaging of Non-radially Pulsating Stars

Published online by Cambridge University Press:  12 April 2016

S. Jankov ,
E. Janot-Pacheco  and
N.V. Leister
S. Jankov
Affiliation:
Astronomical Observatory Beograd, Volgina 7, 11050 Beograd, Yugoslavia
E. Janot-Pacheco
Affiliation:
Institute Astronômico e Geofísico, Universidade de São Paulo, C.P. 9638, 01065-970, São Paulo, SP, Brasil
N.V. Leister
Affiliation:
Institute Astronômico e Geofísico, Universidade de São Paulo, C.P. 9638, 01065-970, São Paulo, SP, Brasil

Abstract

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In addition to the common applications (temperature, magnetic field, abundance distributions) the Doppler Imaging technique can also be applied to non-radial stellar pulsations (NRP). Due to their rapid rotation, the Be stars are ideal candidates for Doppler Imaging. However, for the stars for which the periodic temporal line profile variability is produced by multiple mode NRP, the classical Doppler image in not an appropriate representation. When the corotating frequencies of existing pulsation modes are non-zero, the reference frame in which the resulting NRP is quasi-stationary cannot be defined. The technique can be applied “mode-by-mode”, which is illustrated in time-wavelength and Fourier frequency domain, using the time-resolved sequence of high resolution, high signal-to-noise ratio spectra of the Be star ζ Oph.

Type
3. Periodic Variations
Information
International Astronomical Union Colloquium , Volume 175: The Be Phenomenon in Early-Type Stars , 2000 , pp. 264 - 267
Copyright
Copyright © Astronomical Society of the Pacific 2000

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