Coherent semiclassical states for loop quantum cosmology

Understand

The spatially flat Friedman-Robertson-Walker (FRW) cosmological model with a massless scalar field in loop quantum cosmology admits a description in terms of a completely solvable model.

• This has been used to prove that: i) the quantum bounce that replaces the big bang singularity is generic; ii) there is an upper bound on the energy density for all states and iii) semiclassical states at late times had to be semiclassical before the bounce.
• Here we consider a family of exact solutions to the theory, corresponding to generalized coherent Gaussian and squeezed states.
• We analyze the behavior of basic physical observables and impose restrictions on the states based on physical considerations.