  We present numerical simulations of a 15 solar mass star in a suite of
idealised environments in order to quantify the amount of energy transmitted to
the interstellar medium (ISM). We include models of stellar winds, UV
photoionisation and the subsequent supernova based on theoretical models and
observations of stellar evolution. The system is simulated in 3D using
RAMSES-RT, an Adaptive Mesh Refinement Radiation Hydrodynamics code. We find
that stellar winds have a negligible impact on the system owing to their
relatively low luminosity compared to the other processes. The main impact of
photoionisation is to reduce the density of the medium into which the supernova
explodes, reducing the rate of radiative cooling of the subsequent supernova.
Finally, we present a grid of models quantifying the energy and momentum of the
system that can be used to motivate simulations of feedback in the ISM unable
to fully resolve the processes discussed in this work.
