Cosmological voids with sizes >10 Mpc are the most under dense regions of the Universe in which to study galaxy evolution, with a galaxy population that is theorised to have assembled its mass via star formation only. Due to their isolation, void galaxies are thought to be pristine, and their evolution is likely governed by internal processes. By examining their properties, we can therefore gain a better understanding of the internal feedback processes that govern low mass galaxy evolution in an environment where galaxy-galaxy interactions are likely uncommon. Using the Galaxy and Mass Assembly (GAMA) dataset, we identify a sample of galaxies residing in cosmological voids to M_g=-18 out to z=0.1, with a population of void dwarf galaxies found at low redshifts (z<0.05). The majority of void galaxies are low mass, blue, star forming irregular or spiral galaxies with colours (g-i) < 0.8. However, a number of red, non star forming galaxies are identified, showing a fraction of void galaxies have undergone processes that have shut off their star formation. By comparing their properties with those of the field, we will establish if these red void galaxies are simply faded disks, or if other processes are responsible for quenching their star formation.