DeWitt boundary condition in one-loop quantum cosmology
arXiv:2303.05430 · doi:10.3390/universe9040187
Abstract
DeWitt's suggestion that the wave function of the universe should vanish at the classical big-bang singularity is here considered within the framework of one-loop quantum cosmology. For pure gravity at one loop about a flat four-dimensional background bounded by a 3-sphere, three choices of boundary conditions are considered: vanishing of the linearized magnetic curvature when only transverse-traceless gravitational modes are quantized; a one-parameter family of mixed boundary conditions for gravitational and ghost modes; diffeomorphism invariant boundary conditions for metric perturbations and ghost modes. A positive zeta(0) value in these cases ensures that, when the 3-sphere boundary approaches zero, the resulting one-loop wave function approaches zero. This property may be interpreted by saying that, in the limit of small three-geometry, the resulting one-loop wave function describes a singularity-free universe. This property holds for one-loop functional integrals, which are not necessarily equivalent to solutions of the quantum constraint equations.
arXiv commentIn the final version, the presentation has been improved
References in corpus (11)
- Gauge theories on manifolds with boundary
- Quantum cosmology and late-time singularities
- Lack of strong ellipticity in Euclidean quantum gravity
- Holographic quantization of gravity in a black hole background
- Foliation, jet bundle and quantization of Einstein gravity
- Non-Local Boundary Conditions in Euclidean Quantum Gravity
- Spectral asymptotics of Euclidean quantum gravity with diff-invariant boundary conditions
- Mixed Boundary Conditions in Euclidean Quantum Gravity
- DeWitt boundary condition is consistent in Hořava-Lifshitz quantum gravity
- New Kernels in Quantum Gravity
- A Non-Singular One-Loop Wave Function of the Universe From a New Eigenvalue Asymptotics in Quantum Gravity