It is shown that, for a de Sitter Universe, the Hartle–Hawking (HH) wave function can be obtained in a simple way starting from the Friedmann–Lemaitre–Robertson–Walker (FLRW) line element of cosmological equations. An oscillator having imaginary time is indeed derived starting from the Hamiltonian obtaining the HH condition. This proposes again some crucial matter on the meaning of complex time in cosmology. In order to overcome such difficulties, we propose an interpretation of the HH framework based on de Sitter Projective Holography.
Hartle-Hawking boundary conditions as Nucleation by de Sitter Vacuum
Feleppa F.;
2019-01-01
Abstract
It is shown that, for a de Sitter Universe, the Hartle–Hawking (HH) wave function can be obtained in a simple way starting from the Friedmann–Lemaitre–Robertson–Walker (FLRW) line element of cosmological equations. An oscillator having imaginary time is indeed derived starting from the Hamiltonian obtaining the HH condition. This proposes again some crucial matter on the meaning of complex time in cosmology. In order to overcome such difficulties, we propose an interpretation of the HH framework based on de Sitter Projective Holography.File in questo prodotto:
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