On the seismic modelling of rotating B-type pulsators in the traditional approximation

TL;DR

This paper explores seismic modeling of rotating B-type pulsators using the traditional approximation, addressing the challenges of interpreting complex oscillation data from space telescopes like CoRoT and Kepler.

Contribution

It introduces oscillation computations incorporating the Coriolis force via the traditional approximation for B-type stars, highlighting the limitations of classical frequency matching.

Findings

Classical frequency matching has limited predictive power for high-order gravity modes.

Numerous modes of consecutive radial order are needed for effective seismic modeling.

The traditional approximation helps account for rotation effects in pulsation analysis.

Abstract

The CoRoT and Kepler data revolutionised our view on stellar pulsation. For massive stars, the space data revealed the simultaneous presence of low-amplitude low-order modes and dominant high-order gravity modes in several B-type pulsators. The interpretation of such a rich set of detected oscillations requires new tools. We present computations of oscillations for B-type pulsators taking into account the effects of the Coriolis force in the so-called traditional approximation. We discuss the limitations of classical frequency matching to tune these stars seismically and show that the predictive power is limited in the case of high-order gravity mode pulsators, except if numerous modes of consecutive radial order can be identified.