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Massive stars are important metal factories in the Universe. They have shortand energetic lives, and many of them inevitably explode as a supernova andbecome a neutron star or black hole. In turn, the formation, evolution andexplosive deaths of massive stars impact the surrounding interstellar mediumand shape the evolution of their host galaxies. Yet the chemical and dynamicalevolution of a massive star, including the chemical yield of the ultimatesupernova and the remnant mass of the compact object, strongly depend on theinterior physics of the progenitor star. We currently lack empiricallycalibrated prescriptions for various physical processes at work within massivestars, but this is now being remedied by asteroseismology. The study of stellarstructure and evolution using stellar oscillations - asteroseismology - hasundergone a revolution in the last two decades thanks to high-precision timeseries photometry from space telescopes. In particular, the long-term lightcurves provided by the MOST, CoRoT, BRITE, Kepler/K2 and TESS missions providedinvaluable data sets in terms of photometric precision, duration and frequencyresolution to successfully apply asteroseismology to massive stars and probetheir interior physics. The observation and subsequent modelling of stellarpulsations in massive stars has revealed key missing ingredients in stellarstructure and evolution models of these stars. Thus asteroseismology has openeda new window into calibrating stellar physics within a highly degenerate partof the Hertzsprung-Russell diagram. In this review, I provide a historicaloverview of the progress made using ground-based and early space missions, anddiscuss more recent advances and breakthroughs in our understanding of massivestar interiors by means of asteroseismology with modern space telescopes.

Asteroseismology of high-mass stars: new insights of stellar interiors with space telescopes