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Eternal Universes

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arxiv 2404.03016 v2 pith:J3YLUQGB submitted 2024-04-03 hep-th gr-qc

Damien A. Easson , Joseph E. Lesnefsky This is my paper · ORCID
classification hep-thgr-qc
keywords eternalbouncingcompleteenergyspacetimesuniversesamountbeginning
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We consider the possibility of a past and future eternal universe, constructing geodesically complete inflating, loitering, and bouncing spacetimes. We identify the constraints energy conditions in General Relativity place on the building of eternal cosmological models. Inflationary and bouncing behavior are shown to be essential ingredients in all significant examples. Non-trivial complete flat spacetimes are shown to violate the null energy condition (NEC) for at least some amount of time. Ignoring the intractable subtleties introduced by quantum considerations, such as rare tunneling events and Boltzmann brains, we demonstrate that these universes need not have had a beginning or an end.

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Cited by 4 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. Geodesic completeness of anisotropic cosmologies and the null energy condition

    gr-qc 2026-08 conditional novelty 7.0 of 10

    A Bianchi-I spacetime obeying the null energy condition and expanding in all directions at one time must have past-incomplete null geodesics.

  2. Obstructions to Minimal Regular Black Hole Cosmologies

    gr-qc 2026-06 conditional novelty 7.0 of 10

    Obstructions from matching conditions and completeness theorems prevent minimal regular black hole models from hosting unbounded FRW daughter cosmologies.

  3. Chaos in Horndeski cosmologies

    gr-qc 2025-09 conditional novelty 7.0 of 10

    In Bianchi IX cosmologies, ordinary scalar fields kill mixmaster chaos when their energy is not subleading, but a phantom scalar then produces eternal, chaotic, non-singular bounces.

  4. Cosmological Perturbations from a New Approach to Inflation

    astro-ph.CO 2025-01 conditional novelty 6.0 of 10

    A nearly static 'lingering' phase before inflation is unstable, and the growth of perturbations during that phase could seed the transition to inflation and leave observable curvature or transplanckian signatures.

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