Strong gravity in the immediate vicinity of compact objects (e.g., black holes, neutron stars) necessitates inclusion of general relativistic effects. Traditionally, pseudo-Newtonian potential representations of gravity were favored to simulate the fluid motion in this region since that reduced the calculation complexity. However, with the advent of easily implementable, reliable numerical algorithms and computer hardware, more and more research groups are shifting towards the numerical solutions of general relativistic fluid dynamics equations. In this chapter, we report our progress on the development of such simulation tool and present results of sub-Keplerian accretion flow onto black holes.