  The formation and evolution of galaxies have proved sensitive to the
inclusion of stellar feedback, which is therefore crucial to any successful
galaxy model. We present INFERNO, a new model for hydrodynamic simulations of
galaxies, which incorporates resolved stellar objects with star-by-star
calculations of when and where the injection of enriched material, momentum,
and energy takes place. INFERNO treats early stellar kinematics to include
phenomena such as walkaway and runaway stars. We employ this innovative model
on simulations of a dwarf galaxy and demonstrate that our physically motivated
stellar feedback model can drive vigorous galactic winds. This is quantified by
mass and metal loading factors in the range of $10-100$, and an energy loading
factor close to unity. Outflows are established close to the disc, are highly
multi-phase, spanning almost $8$ orders of magnitude in temperature, and with a
clear dichotomy between mass ejected in cold, slow-moving
($T\lesssim5\times10^4\,{\rm K}$, $v<100\,{\rm km\,s}^{-1}$) gas and energy
ejected in hot, fast-moving ($T>10^6\,{\rm K}$, $v>100\,{\rm km\,s}^{-1}$) gas.
In contrast to massive disc galaxies, we find a surprisingly weak impact of the
early stellar kinematics, with runaway stars having little to no effect on our
results, despite exploding in diffuse gas outside the dense star-forming gas,
as well as outside the galactic disc entirely. We demonstrate that this weak
impact in dwarf galaxies stems from a combination of strong feedback and a
porous interstellar medium, which obscure any unique signatures that runaway
stars provide.

Astrophysics of Galaxies