A procedure for modelling asymptotic g-mode pulsators: The case of γ Doradus stars

Details A procedure for modelling asymptotic g-mode pulsators: The case of γ Doradus stars A procedure for modelling asymptotic g-mode pulsators: The case of γ Doradus stars

Jun 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008an....329..541m&link_type=abstract

Astronomische Nachrichten, Vol.329, Issue 5, p.541

Statistics

Computation

3

Stars: Evolution, Stars: Interiors, Stars: Oscillations, Stars: Rotation, Stars: Fundamental Parameters

Scientific paper

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 γ Doradus star 9 Aurigae.

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