 The first approach aims to reduce dependence on special initial conditions by introducing a phase of attractor dynamics. This phase of dynamical evolution “washes away” the traces of earlier states, in the sense that a probability distribution assigned over initial states converges towards an equilibrium distribution. Misner (1968) introduced a version of this approach (his “chaotic cosmology program”), proposing that free-streaming neutrinos could isotropize an initially anisotropic state. Inflationary cosmology was initially motivated by a similar idea: a “generic” or “random” initial state at the Planck time would be expected to be “chaotic”, far from a flat FLRW model. During an inflationary stage, arbitrary initial states are claimed to converge towards a state with the three features described above.