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Astron. Astrophys. 317, 742-748 (1997)

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Line-profile variations of non-radial adiabatic pulsations of rotating stars

III. On the alleged misidentification of tesseral modes

J.H. Telting and C. Schrijvers

Astronomical Institute Anton Pannekoek, University of Amsterdam, and Center for High Energy Astrophysics, Kruislaan 403, 1098 SJ Amsterdam, Netherlands

Received 22 March 1996 / Accepted 3 June 1996


We use a model of a non-radially, adiabatically pulsating rotating star to generate time series of absorption line profiles. We analyse the spectral time series of a tesseral mode with pulsation parameters [FORMULA] =2 and m =-1, to obtain amplitude and phase diagrams as a function of position in the line profile. We investigate whether the phase diagrams can be used to identify the pulsation parameters [FORMULA] and [FORMULA] of this mode.

As opposed to the findings of Reid & Aerts (1993), we find that the effects of the Coriolis force do not hinder the identification of the degree [FORMULA] of the pulsation mode, but that the exact value of i = [FORMULA] that they used does. We show that for an inclination angle just slightly different from [FORMULA] the chances for an erroneous identification of the degree [FORMULA] of the [FORMULA] =2, m =-1 pulsation mode, by means of a spectroscopical phase diagram, are very small.

We also discuss the interpretation of observed line-profile variations in the Be star [FORMULA] Cen, where a tesseral mode with [FORMULA] =7 and m = [FORMULA] might be present.

Key words: stars: early-type, oscillations, rotation – line: profiles – stars individual: j Cen

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© European Southern Observatory (ESO) 1997

Online publication: July 8, 1998