The self-force approach is a method to describe the motion of a small body in a curved spacetime beyond the geodesic approximation. In this approach, the motion of a small body is corrected to the geodesic motion including the back-reaction of its own gravitational field (ie "gravitational self-force") order by order in the mass ratio. The self-force approach will play a crucial role to model the gravitational-wave signal from large-mass-ratio compact binaries (stellar compact objects inspiral into super massive black holes), which is a main source of the future space-based gravitational-wave detectors (LISA). This talk will describe the orbital motion beyond geodesic approximation in the self-force approach. I will overview the self-force approach in the two-body problem in general relativity, and show recent results that characterize post-geodesic effects to the conservative dynamics in the two-body system. I will then discuss their connection for the results from other approach (post-Newtonian and Numerical Relativity methods) to the two-body systems.