Sommaire:

Asteroseismology has opened a window on the internal physics of thousands of stars, by relating their pulsations to their internal physics. Seismic modelling requires good models and a reliable matching of the measured frequencies to the oscillation geometries. In upper main-sequence stars, that often rotate rapidly, this matching is challenging as both the structure and the oscillations are impacted by the centrifugal and Coriolis forces.

In this talk, I will describe the models we use, the mode geometries that emerge in rapidly rotating stars, and their differences with slow rotators. I will present recent progress, based on either perturbative treatments or complete calculations of rotation : line-profile variations of rapid rotators, cluster dating through delta Scuti stars, machine-learning techniques applied to mode identification and inversion techniques. Each of these facets is part of a bigger picture that is becoming clearer every day.

Pour plus d'informations, merci de contacter Morin J.