Description
During the main sequence the convective cores of massive stars act as engines that drive their evolution, but direct inference of core masses is challenging. Moreover, estimates are subject to unconstrained convective boundary mixing (CBM) processes owing to largely uncalibrated prescriptions in 1D stellar evolution models. The uncertain chemical and angular momentum transport mechanisms can lead to unwieldy interior mixing and rotation profiles, thus making it difficult to predict a massive star's evolutionary fate. However, thanks to ongoing space missions and our development of modern asteroseismic modelling techniques for massive stars, we are now able to deduce precise convective core masses and robustly measure (non-rigid) radial rotation profiles in main-sequence stars that span a wide range in mass and age within the HR diagram. In this talk, I will provide an introduction to asteroseismology of massive stars for the non-expert and highlight recent modern advances in forward asteroseismic modelling of such stars. The combination of space photometry, high-resolution spectroscopy, and Gaia astrometry for massive stars allows precise measurements of masses, core masses, and ages to better than 10-20% precision. Asteroseismic modelling of gravity-mode period spacing patterns and rotational multiplets also allow CBM, as well as the near-core and envelope rotation profiles to be inferred, thus providing important anchor points for calibrating angular momentum transport processes. Finally, the inclusion of magnetic fields in forward asteroseismic modelling also allows the strength and geometry of such fields and their impact on CBM to be probed through magneto-asteroseismology.
