Seismic modelling of the rotating, slowly pulsating B-type star HD 21071

Abstract

Interpretation of the oscillation spectrum of the slowly pulsating B-type star HD21071 is presented. We show that non-rotating models cannot account for the two highest amplitude frequencies and taking into account the effects of rotation is necessary. Rotating seismic models are constructed using various chemical compositions, opacity data, core overshooting parameters and rotational velocities. There are prospects for seismic modelling of SPB stars, even if no asymptotic pattern is observed in their oscillation spectra, provided an unambiguous mode identification is doable and the effects of rotation are properly included.

13 pages, 9 figures, 4 tables, accepted in MNRAS

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• Seismic modeling of a very young SPB star -- KIC8264293
• Analysis of high-resolution FEROS spectroscopy for a sample of variable B-type stars assembled from TESS photometry
• Mode coupling coefficients between the convective core and radiative envelope of $\gamma$Doradus and slowly pulsating B stars
• On the diversity of mixing and helium core masses of B-type dwarfs from gravity-mode asteroseismology