$\mathrm{\Psi }=\mathrm{W}{\mathrm{e}}^{\pm \mathrm{\Phi }}$ quantum cosmological solutions for Class A Bianchi Models

Abstract

We find solutions for quantum Class A Bianchi models of the form $\mathrm{\Psi }=\mathrm{W}{\mathrm{e}}^{\pm \mathrm{\Phi }}$ generalizing the results obtained by Moncrief and Ryan in standard quantum cosmology. For the II and IX Bianchi models there are other solutions ${\tilde{\mathrm{\Phi }}}_2$, ${\tilde{\mathrm{\Phi }}}_9$ to the Hamilton-Jacobi equation for which $\mathrm{\Psi }$ is necessarely zero, in contrast with solutions found in supersymmetric quantum cosmology.

15 pages, Latex

References in corpus (5)

• Supersymmetric minisuperspace with non-vanishing fermion number
• Supersymmetric Bianchi class A models
• Bianchi Cosmologies: New Variables and a Hidden Supersymmetry
• Super-Minisuperspace and New Variables
• No Quantum Super-Minisuperspace with $\Lambda \ne 0$

Cited by in corpus (6)

• Classical and Quantum Features of the Mixmaster Singularity
• Supersymmetric Quantum Mechanics for Bianchi Class A models
• Scalar potentials out of canonical quantum cosmology
• Inflation from Supersymmetric Quantum Cosmology
• Supersymmetric quantum cosmology for Bianchi class A models
• Time-dependent toroidal compactification proposals and the Bianchi type II model: classical and quantum solutions