Frequency regularities of acoustic modes and multi-colour mode identification in rapidly rotating stars
1 Institut d’Astrophysique et Géophysique de l’Université de Liège, Allée du 6 Août 17, 4000, Liège, Belgium
2 School of Physics and Astronomy, University of Birmingham, Edgbaston, Birmingham, B15 2TT, UK
3 LESIA, Observatoire de Paris, PSL Research University, CNRS, Sorbonne Universités, UPMC Univ. Paris 06, Univ. Paris Diderot, Sorbonne Paris Cité, 5 place Jules Janssen, 92195 Meudon, France
4 Université de Toulouse, UPS-OMP, IRAP, 31028 Toulouse, France
5 CNRS, IRAP, 14 avenue Édouard Belin, 31400 Toulouse, France
6 GEPI, Observatoire de Paris-Meudon, CNRS, Université Paris Diderot, 92125 Meudon Cedex, France
7 High Altitude Observatory, National Center for Atmospheric Research, Boulder, CO 80307, USA
Received: 8 February 2013
Accepted: 27 January 2017
Context. Mode identification has remained a major obstacle in the interpretation of pulsation spectra in rapidly rotating stars. This has motivated recent work on calculating realistic multi-colour mode visibilities in this type of star.
Aims. We would like to test mode identification methods and seismic diagnostics in rapidly rotating stars, using oscillation spectra that are based on these new theoretical predictions.
Methods. We investigate the auto-correlation function and Fourier transform of theoretically calculated frequency spectra, in which modes are selected according to their visibilities. Given that intrinsic mode amplitudes are determined by non-linear saturation and cannot currently be theoretically predicted, we experimented with various ad-hoc prescriptions for setting the mode amplitudes, including using random values. Furthermore, we analyse the ratios between mode amplitudes observed in different photometric bands to see up to what extent they can identify modes.
Results. When non-random intrinsic mode amplitudes are used, our results show that it is possible to extract a mean value for the large frequency separation or half its value and, sometimes, twice the rotation rate, from the auto-correlation of the frequency spectra. Furthermore, the Fourier transforms are mostly sensitive to the large frequency separation or half its value. The combination of the two methods may therefore measure and distinguish the two types of separations. When the intrinsic mode amplitudes include random factors, which seems more representative of real stars, the results are far less favourable. It is only when the large separation or half its value coincides with twice the rotation rate, that it might be possible to detect the signature of a frequency regularity. We also find that amplitude ratios are a good way of grouping together modes with similar characteristics. By analysing the frequencies of these groups, it is possible to constrain mode identification, as well as determine the large frequency separation and the rotation rate.
Key words: stars: oscillations / stars: rotation / stars: interiors / stars: variables:δScuti
© ESO, 2017