[en] Mode identification is one of the first and main problems we encounter in trying to develop the complete potential of asteroseismology. In the particular case of {g}-mode pulsators, this is still an unsolved problem, from both the observational and theoretical points of view. Nevertheless, in recent years, some observational and theoretical efforts have been made to find a solution. In this work we use the latest theoretical and computational tools to understand asymptotic {g}-mode pulsators: 1) the Frequency Ratio Method, and 2) Time Dependent Convection. With these tools, a self-consistent procedure for mode identification and modelling of these {g}-mode pulsators can be constructed. This procedure is illustrated using observational information available for the gamma Doradus star 9 Aurigae.
Disciplines :
Space science, astronomy & astrophysics
Author, co-author :
Moya, A.; Instituto de Astrofísica de Andalucía -CSIC, Cno. Bajo de Huetor, 18008, Granada, Spain
Suárez, J. C.; Instituto de Astrofísica de Andalucía -CSIC, Cno. Bajo de Huetor, 18008, Granada, Spain
Martín-Ruiz, S.; Instituto de Astrofísica de Andalucía -CSIC, Cno. Bajo de Huetor, 18008, Granada, Spain
Amado, P. J.; Instituto de Astrofísica de Andalucía -CSIC, Cno. Bajo de Huetor, 18008, Granada, Spain
Rodríguez-López, C.; Instituto de Astrofísica de Andalucía -CSIC, Cno. Bajo de Huetor, 18008, Granada, Spain