  Modelling the propagation of supernova (SN) bubbles, in terms of energy,
momentum and spatial extent, is critical for simulations of galaxy evolution
which do not capture these scales. To date, small scale models of SN feedback
predict that the evolution of above-mentioned quantities can be solely
parameterised by average quantities of the surrounding gas, such as density.
However, most of these studies neglect the turbulent motions of this medium. In
this paper, we study the propagation and evolution of SNe in turbulent
environments. We confirm that the time evolution of injected energy and
momentum can be characterised by the average density. However, the details of
the density structure of the interstellar medium play a crucial role in the
spatial extent of the bubble, even at a given average density. We demonstrate
that spherically symmetric models of SN bubbles do not model well their spatial
extent, and therefore cannot not be used to design sub-grid models of SNe
feedback at galactic and cosmological scales.
