Cosmic rays below $10\,\mathrm{GeV}$ are important for the dynamics of the interstellar medium. However, modelling of their propagation around potential sources such as supernova remnants is complicated due to their dynamical backreaction. Due to their overdensity close to the acceleration site they produce turbulence upon which scatter, thereby confining themselves in these regions. This highly non-linear problem can be approached by numerically solving the coupled transport equations of cosmic rays and magnetic turbulence. In this work we will focus on supernovae exploding in those phases of the interstellar medium, where these effects are the most relevant, the warm ionised and warm neutral medium. Interestingly we find, that the self-generated turbulence of low energy cosmic rays suppresses the diffusion coefficient by up to two orders of magnitude for several tens of kiloyears. This results in a non negligible grammage accumulated around the source and has to be accounted for in cosmic ray precision fitting.