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Astron. Astrophys. 350, 617-625 (1999)

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Solar-like oscillations of Procyon A: stellar models and time series simulations versus observations *

C. Barban 1, E. Michel 1, M. Martic 2, J. Schmitt 2, J.C. Lebrun 2, A. Baglin 3 and J.L. Bertaux 2

1 Observatoire de Paris, DASGAL, CNRS UMR 8633, 92195 Meudon, France
2 Service d'Aéronomie, CNRS, 91371 Verrières le Buisson, France
3 Observatoire de Paris, DESPA, CNRS UMR 8632, 92195 Meudon, France

Received 9 July 1999 / Accepted 30 August 1999


The aim of this paper is to discuss the possible stellar origin of the observed excess power presented in Martic et al. (1999) by comparing these observational data with theoretical predictions and numerical simulations. Stellar models are calculated for Procyon A with appropriate physics for this star and with the revised astrometric mass (1.46 [FORMULA] 0.04) [FORMULA] found by Girard (1998). For these models, we compute the expected oscillation spectra for [FORMULA]=0,1,2 modes including m[FORMULA]0 according to theoretical amplitude predictions. Time-series are then simulated, in the same conditions as the observations, and compared by Fourier analysis with the observed ones. We show that the characteristics of the signal are in good agreement with what should be expected for such observing runs and we emphasize the importance of obtaining multi-site observations for this star. We confirm the presence of a periodic pattern in the Fourier spectrum, this pattern being interpreted as the so-called large separation.

Key words: stars: oscillations – stars: individual: Procyon A

* Based on observations collected at the Observatoire de Haute-Provence (CNRS, France).

Send offprint requests to: Caroline.Barban@obspm.fr

© European Southern Observatory (ESO) 1999

Online publication: October 4, 1999