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Astron. Astrophys. 317, 723-741 (1997)

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

II. The diagnostic value of amplitude and phase diagrams derived from time series of spectra

John H. Telting and Coen Schrijvers

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

Received 14 March 1996 / Accepted 3 June 1996


We discuss the possibilities to derive the pulsation parameters [FORMULA] and m of non-radially pulsating rotating stars from spectroscopic observations. We model the line-profile variations caused by the oscillatory velocity field and temperature variations at the surface of the star. In our description of the velocity field of the pulsations, we use the expressions for linear adiabatic pulsations, and include terms that account for the Coriolis force. For various stellar and pulsational parameters we generate time series of spectra, and analyse the phase and amplitude diagrams resulting from a Fourier analysis of the time series.

We find that for stars with [FORMULA] larger than approximately five times the half-width (HWHM) of the intrinsic profile, one can derive both the degree [FORMULA] and the order [FORMULA] from the phase diagrams of the line-profile variations. We present linear relations between observable phase differences and the parameters [FORMULA] and [FORMULA]. These relations can be used to identify pulsation modes. This method works for spheroidal and toroidal, sectoral and tesseral modes; it is possible to derive values of [FORMULA] and values of [FORMULA]. The method is also applicable to multi-periodic multi-mode pulsations.

We apply the method to analyse spectroscopic data sets of [FORMULA] Oph and [FORMULA] Per, and present values of [FORMULA] of the pulsation modes in these stars. We use harmonic phase diagrams to constrain values of [FORMULA] of some of these modes.

We argue that the presence of the complex pattern of frequencies in the periodogram of the line-profile variations of [FORMULA] Per, is consistent with the expectations for profile variations which are dominated by the oscillatory velocity field, rather than the oscillatory temperature variations.

Key words: line: profiles – stars: oscillations; rotation – stars: variable: ffi Sct – stars individual: i Oph , ffl Per

© European Southern Observatory (ESO) 1997

Online publication: July 8, 1998