Geodesics of the schwarzschild black hole

Black holes are best known with their strong gravitational field from which even light can not escape. They are sometimes called spacetime singularities. There are observational evidence of existence of black holes. The simplest and the best known one is the Schwarzschild black hole which has a static spherically symmetric gravitational field, uncharged and not rotating. However, there are still some ambiguities inherited in the solution of the Schwarzschild black hole. To get a better understanding of them one can look at how particles and light behave around the black hole, i.e. their geodesics. In this thesis we studied geodesics of the Schwarzschild black hole inside and outside of the event horizon. First, derivation of the Schwarzschild metric is done using Cartan's structural equations. Then, it is verified that the geodesic of a particle in free spacetime is a straight line.Afterwards, we have looked at geodesics of the Schwarzschild black hole. By calculating the equations for the geodesics of both - the particle and light - in two cases (angular momentum is zero and nonzero) we defined a potential and drew its graph and identified the orbits around the black hole. Then, we examined consistency of the graphs with our equations.Lastly, by comparing the defined potential with the Newtonian potential, we designated how particles and light behave differently around the black hole.