A review of recent asteroseismology results from the KU Leuven team

Thanks to recent high-precision time-series photometry from space missions, asteroseismology of massive stars has undergone a revolution in the last decade. The high-radial order g-mode pulsation frequencies of slowly pulsating B stars, and the low-radial order p- and g-mode pulsation frequencies of beta Cephei stars provide a window inside the deep interiors of stars with masses between 3 and 25 solar masses. In this review of the recent asteroseismology results from the Institute of Astronomy at KU Leuven, I discuss how asteroseismology using Kepler space photometry reveals a diverse range of envelope mixing efficiencies, and allows the direct measurement of the size, shape and temperature gradient of the core boundary mixing region in slowly pulsating B stars. Furthermore, new TESS mission photometry allows us to extend asteroseismology to massive stars and study the interior rotation profiles of beta Cephei stars, as well as determine their precise masses and ages using forward asteroseismic modelling. Armed with new techniques and results, asteroseismology is now providing detailed and valuable constraints of the deep interiors of massive stars for future generations of stellar and galactic evolution codes.