More than fifty percent of the neutron-rich nuclei heavier than iron have their origin in the r-process that is believed to take place in the hot insides of core-collapse supernovae. These rapid neutron captures (r-process) involve many of the extreme neutron rich isotopes far from beta-stability where experimental knowledge of nuclear properties is rudimentary. This makes theoretical modeling of the atomic nucleus an important piece of the stellar nuclear abundance puzzle. In this paper I will examine the r-process from the perspective of a macroscopic-microscopic nuclear model developed by P. Möller et. al. based on the finite range liquid drop macroscopic model with a folded Yukawa-potential for the shell-correction(FRLDM). In the latest calculation using this model the possibility for triaxiality was implemented , a shape-degree of freedom never investigated on this scale(7206 nuclei) before.