  About ten to 20 percent of massive stars may be kicked out of their natal
clusters before exploding as supernovae. These "runaway stars" might play a
crucial role in driving galactic outflows and enriching the circumgalactic
medium with metals. To study this effect, we carry out high resolution dwarf
galaxy simulations that include velocity kicks to massive O/B stars above 8
M$_{\odot}$. We consider two scenarios, one that adopts a power law velocity
distribution for kick velocities, resulting in more stars with high velocity
kicks, and a more moderate scenario with a Maxwellian velocity distribution. We
explicitly resolve the multi-phase interstellar medium (ISM), and include
non-equilibrium cooling and chemistry channels. We adopt a resolved feedback
scheme (\textsc{Griffin}) where we sample individual massive stars from an IMF.
We follow the lifetime of these stars and add their photoionising radiation,
their UV radiation field, and their photoelectric heating rate to the
surrounding gas. At the end of their lifetime we explode the massive population
as core collapse supernovae (CCSN). In the simulations with runaway massive
stars, we add additional (natal) velocity kicks that mimic two and three body
interactions that cannot be fully resolved in our simulations. We find that the
inclusion of runaway or walkaway star scenarios has an impact on mass, metal,
momentum and energy outflows as well as the respective loading factors. We find
an increase in mass, metal and momentum loading by a factor of 2-3, whereas we
find an increase in the mean energy loading by a factor of 5 in the runaway
case and a factor of 3 in the walkaway case. However, we find that the peak
values are increased by a factor of up to 10, independent of the adopted
velocity kick model. We conclude that the inclusion of runaway stars could have
a significant impact on the global outflow properties of dwarf galaxies.
