In the theory of planetary formation, the process of how sub-µm to mm dust aggregates in protoplanetary discs grow into planetesimals is still poorly understood. A solution to overcome the fragmentation and radial drift barriers is to consider grain porosity (Garcia 2018). We have implemented a porosity evolution model in the SPH code Phantom based on Garcia (2018) and Garcia & Gonzalez (2020), with new destructive effects. With a disc model that reproduces observations, we show that porosity help grain growth as expected, allowing them to reach larger sizes. When fragmentation, bouncing and compaction are taken into account, it is still possible to form a thin disc of large dust in the mid-plane, with correct filling factors and sizes according to observations, something that can not be reproduced with compact grains.