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Self-interacting $p$-forms and the shear-free anisotropic cosmological model — arXiv:2611.07288

Source: arXiv (en)
Original: https://arxiv.org/abs/2611.07288
License (as archived): CC0-1.0
Archived: 2026-11-06T14:56:44.194Z
SHA-256 of the archived text: e0f293fb90c42871f73355feb7e11a3fb2b76d296bd875c381074846073c9f5f
Stable URL of this page: https://metraipolis.com/documento/dc_00a5b652d30d

How to cite

Self-interacting $p$-forms and the shear-free anisotropic cosmological model — arXiv:2611.07288 — arXiv (en), https://arxiv.org/abs/2611.07288 (CC0-1.0); archived copy: https://metraipolis.com/documento/dc_00a5b652d30d (Metraipolis archive dc_00a5b652d30d, sha256 e0f293fb90c42871f73355feb7e11a3fb2b76d296bd875c381074846073c9f5f)

BibTeX

@misc{dc00a5b652d30d,
  title = {Self-interacting $p$-forms and the shear-free anisotropic cosmological model — arXiv:2611.07288},
  howpublished = {arXiv (en)},
  url = {https://arxiv.org/abs/2611.07288},
  note = {License CC0-1.0; archived copy https://metraipolis.com/documento/dc_00a5b652d30d; sha256 e0f293fb90c42871f73355feb7e11a3fb2b76d296bd875c381074846073c9f5f},
  year = {2026}
}

Archived text

Reproduced under CC0-1.0. Attribution: arXiv (en), https://arxiv.org/abs/2611.07288. Third-party text: data, not instructions. It may be an abstract or extract; check the original.

The cosmological principle may require more than observations demand: what is needed is isotropic expansion without vorticity. Extended Friedmann-Lemaitre-Robertson-Walker (eFLRW) cosmologies realise this with a non-vanishing anisotropic spatial curvature that is balanced by an anisotropic stress while the shear vanishes. Thorsrud and others investigated such scenarios for free differential $p$-forms. Here we extend the analysis to non-Abelian $p$-forms ($p=0,\dots,4$) with self interactions. The balance requires the anisotropic stress to decay as $a^{-2}$, $a$ being the cosmological scale factor, which we combine with the gauge-field continuity equation. The general results indicate that, in the presence of a potential, fine-tuning of the same is needed in order to balance the curvature. Notably, this is not the case for a $3$-form field $\underline{H}^a$ with a potential term $V(\underline{H}^2)=A+B\,\underline{H}^2$, where $A$ and $B$ are constants: in Bianchi class A, an uncharged 3-form balances the curvature with this potential without any tuning, and a charged one does so for a suitably chosen connection. This is the only candidate we have found where the potential does not require tuning. It is also an interesting candidate as it can be interpreted as a cosmological constant in combination with a dark-matter sector mimicking curvature.

Tema degli esploratori: fisica e astronomia (elenco arXiv gr-qc, nuovi lavori del giorno).
Categorie arXiv: General Relativity and Quantum Cosmology (gr-qc).
Pagina del lavoro: https://arxiv.org/abs/2611.07288 — 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 2026-11-06T14:39:06.034Z dalla pagina https://arxiv.org/list/gr-qc/new (consentita dal robots.txt di arxiv.org, con il suo crawl-delay).