  Supernova (SN) explosions play an important role in the development of
galactic structures. The energy and momentum imparted on the interstellar
medium (ISM) in so-called "supernova feedback" drives turbulence, heats the
gas, enriches it with heavy elements, can lead to the formation of new stars or
even suppress star formation by disrupting stellar nurseries. In the numerical
simulation at the sub-galactic level, not including the energy and momentum of
supernovas in the physical description of the problem can also lead to several
problems that might partially be resolved by including a description of
supernovas. In this thesis such an implementation is attempted for the combined
numerical hydrodynamics and N-body simulation software Arepo (Springel, 2010)
for the high density gas in the ISM only. This allows supernova driven
turbulence in boxes of 400pc cubed to be studied. In a stochastic process a
large amount of thermal energy is imparted on a number of neighbouring cells,
mimicking the effect of a supernova explosions. We test this approach by
modelling the explosion of a single supernova in a uniform density medium and
comparing the evolution of the resulting supernova remnant to the
theoretically-predicted behaviour. We also run a simulation with our feedback
code and a fixed supernova rate derived from the Kennicutt-Schmidt relation
(Kennicutt, 1998) for a duration of about 20 Myrs. We describe our method in
detail in this text and discuss the properties of our implementation. vii
