Speaker
Description
Effective quantum gravity models often specify corrections to homogeneous cosmological evolution, leaving open how these corrections extend to cosmological perturbations. I will present a framework for constructing scalar and tensor perturbations around a given modified FLRW background. Here, spatial covariance and a Birkhoff-type vacuum requirement constrain its extension to inhomogeneous geometries. For a specified matter realization and class of local actions, the resulting response to curvature and anisotropy determines the quadratic perturbation action and the corresponding Mukhanov–Sasaki equations. As an example, I will consider an effective model motivated by loop quantum gravity with a canonical inflaton and discuss its propagation properties, stability conditions, and general-relativistic limit.