  Rotation matters for the life of a star. It causes a multitude of dynamical
phenomena in the stellar interior during a star's evolution and its effects
accumulate until the star dies. All stars rotate at some level but those born
with a mass above about 1.3 times the mass of the Sun rotate rapidly during
more than 90% of their nuclear lifetime. Internal rotation guides the angular
momentum and chemical element transport throughout the stellar interior. These
transport processes change over time as the star evolves. The cumulative
effects of stellar rotation and its induced transport processes determine the
helium content of the core by the time it exhausts its hydrogen isotopes. The
amount of helium at that stage also guides the heavy element yields at the end
of the star's life. A proper theory of stellar evolution and any realistic
models for the chemical enrichment of galaxies, must be based on observational
calibrations of stellar rotation and of the induced transport processes. Since
a few years, asteroseismology offers such calibrations, for single and binary
stars. We review the current status of asteroseismic modelling of rotating
stars for different stellar mass regimes, in an accessible way for the
non-expert. While doing so, we describe exciting opportunities sparked by
asteroseismology for various domains in astrophysics, touching upon topics from
exoplanetary science to galactic structure and evolution towards gravitational
wave physics. Along the way, we provide ample sneak-previews for future
'industrialised' applications of asteroseismology to slow and rapid rotators,
from exploitation of combined Kepler, TESS, PLATO, Gaia, and spectroscopy
surveys. We end the review with a list of take away messages and achievements
of asteroseismology, which are of relevance for many fields of astrophysics.
