Propagation of scalar and tensor gravitational waves in Horndeski theory

Gravitational waves travel through the distributions of matter and dark energy during propagation. For this reason, gravitational waves emitted from binary compact objects serve as a useful tool especially to probe the nature of dark energy. The geometrical optics approximation is a conventional way of investigating wave propagation. However, the approximation becomes less accurate as the wavelength approaches the curvature radius of the background, which can occur in generic situations. In this paper, we suggest a formulation for higher-order corrections of the geometrical optics expansion, applied to Horndeski theory which accommodates many dark energy models. At the level of the background, assuming that the derivative of the scalar field is nonvanishing and timelike, we choose the time slices to coincide with the contours of the scalar field. This choice of the background time slices is advantageous as the sound cones of both scalar and tensor gravitational waves are upright with respect to the background time slices whenever the scalar field behaves as a perfect fluid. We then analyze the equations of motion for scalar and tensor components of gravitational waves at the leading and next-to-leading order in the geometrical optics expansion, deriving the evolution equations for their amplitudes under certain conditions. In particular, for generalized Brans-Dicke theories, we find a simple description of equations for gravitational waves in terms of an effective metric.

Figure 1

By choosing the time coordinate to set $\overline{\varphi }=\overline{\varphi }(t)$, we foliate the background spacetime by spacelike hypersurfaces with normal vectors having the same direction as the axis of the sound cone whenever the scalar field behaves as a perfect fluid. The sound cone is tilted with respect to the normal vector of other hypersurfaces even when the scalar field behaves as a perfect fluid.