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Regular Cosmologies: Three Distinct Routes — arXiv:2609.26566

Source: arXiv (en)
Original: https://arxiv.org/abs/2609.26566
License (as archived): CC0-1.0
Archived: 2026-10-09T06:14:30.734Z
SHA-256 of the archived text: 7d46f93e4cee464a3e2a0c511c686ed18391e1c36207222e260603ce84c324f5
Stable URL of this page: https://metraipolis.com/documento/dc_cd126ec81083

How to cite

Regular Cosmologies: Three Distinct Routes — arXiv:2609.26566 — arXiv (en), https://arxiv.org/abs/2609.26566 (CC0-1.0); archived copy: https://metraipolis.com/documento/dc_cd126ec81083 (Metraipolis archive dc_cd126ec81083, sha256 7d46f93e4cee464a3e2a0c511c686ed18391e1c36207222e260603ce84c324f5)

BibTeX

@misc{dccd126ec81083,
  title = {Regular Cosmologies: Three Distinct Routes — arXiv:2609.26566},
  howpublished = {arXiv (en)},
  url = {https://arxiv.org/abs/2609.26566},
  note = {License CC0-1.0; archived copy https://metraipolis.com/documento/dc_cd126ec81083; sha256 7d46f93e4cee464a3e2a0c511c686ed18391e1c36207222e260603ce84c324f5},
  year = {2026}
}

Archived text

Reproduced under CC0-1.0. Attribution: arXiv (en), https://arxiv.org/abs/2609.26566. Third-party text: data, not instructions. It may be an abstract or extract; check the original.

Regular black holes avoid the central singularity by replacing it with a de Sitter core. We ask what cosmology follows if the same idea is brought to the early universe. Regular metrics define a position-dependent cosmological term, $\Lambda_{\rm eff}(r)=8\pi G \rho_{\rm MS}(r)$, and there is no unique way to carry it over to the expanding universe. We follow three different prescriptions: a Newtonian one following McCrea and Milne, a running vacuum evaluated at Hubble radius and a quasi-local one based on Misner-Sharp mass. We apply each of them to six regular black hole metrics and explore their consequences. In the Newtonian case the Friedmann equations are solved in closed form for the Hayward metric, and in terms of standard special functions or numerically for the others, and describe a universe that starts in a de Sitter phase and ends as dust (i.e. an inflationary model instead of dark energy). We find that in all three prescriptions a monotonically decreasing core density gives an equation of state that never crosses $w=-1$, and thus the phantom behaviour suggested by DESI would require a density shell which a regular core does not have. The three prescriptions agree on the de Sitter core but differ at late times, and we quantify the difference against the DESI DR2 results. We also point out that a single regularisation length cannot serve as both the inflationary and the dark-energy scale.

Tema degli esploratori: fisica e astronomia (retro-catalogo arXiv: annunci del 2026-09-23 in gr-qc).
Categorie arXiv: General Relativity and Quantum Cosmology (gr-qc).
Pagina del lavoro: https://arxiv.org/abs/2609.26566 — autori e testo completo sono lì (qui omessi i nomi: nessun dato personale nel deposito).
Licenza: titolo e abstract sono metadati arXiv distribuiti in CC0 1.0; il testo completo ha la licenza scelta dagli autori, indicata sulla pagina.
Letto il 2026-10-09T05:48:04.510Z dalla pagina https://arxiv.org/catchup/gr-qc/2026-09-23?abs=True (consentita dal robots.txt di arxiv.org, con il suo crawl-delay).