Gravitational waves from inspiralling compact binaries will provide tests of alternative theories of gravity, such as the general class of scalar-tensor theories. We derive the scalar-tensor equations of motion for non-spinning compact objects, including black holes and neutron stars, to order (v/c)^5 beyond Newtonian order. We use the DIRE (Direct Integration of the Relaxed Einstein Equations) formalism [1] adapted to scalar-tensor theory, coupled with Eardley's scheme [2] for incorporating compact, quasi- stationary, self-gravitating bodies. We find that to this order of the PN approximation, binary black hole behavior in this class of theories is indistinguishable from that predicted by general relativity

This talk has two parts. In the first part I will briefly review Gravitational Waves: phenomenology, sources, detectors, and data analysis and in the second part I will present my current work

[1] A. G. Wiseman and C. M. Will, Phys. Rev. D 54, 4813 (1996); M. E. Pati and C. M. Will, Phys. Rev. D 62, 124015 (2000); ibid. 65, 104008 (2002)

[2] D. M. Eardley, Astrophys. J. Lett. 196, L59 (1975

IPM Larak Building, School of Astronomy