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Composition $g$-modes and $f$-modes of neutron stars with gravitationally coupled dark matter: degeneracy with the symmetry energy — arXiv:2610.10007

Source: arXiv (en)
Original: https://arxiv.org/abs/2610.10007
License (as archived): CC0-1.0
Archived: 2026-10-08T14:11:39.231Z
SHA-256 of the archived text: 301c6db913e438fb24c9e9a76798269f77373f835ecb0a0f46f2dc0c699fdd6f
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How to cite

Composition $g$-modes and $f$-modes of neutron stars with gravitationally coupled dark matter: degeneracy with the symmetry energy — arXiv:2610.10007 — arXiv (en), https://arxiv.org/abs/2610.10007 (CC0-1.0); archived copy: https://metraipolis.com/documento/dc_ea5da0800bdb (Metraipolis archive dc_ea5da0800bdb, sha256 301c6db913e438fb24c9e9a76798269f77373f835ecb0a0f46f2dc0c699fdd6f)

BibTeX

@misc{dcea5da0800bdb,
  title = {Composition $g$-modes and $f$-modes of neutron stars with gravitationally coupled dark matter: degeneracy with the symmetry energy — arXiv:2610.10007},
  howpublished = {arXiv (en)},
  url = {https://arxiv.org/abs/2610.10007},
  note = {License CC0-1.0; archived copy https://metraipolis.com/documento/dc_ea5da0800bdb; sha256 301c6db913e438fb24c9e9a76798269f77373f835ecb0a0f46f2dc0c699fdd6f},
  year = {2026}
}

Archived text

Reproduced under CC0-1.0. Attribution: arXiv (en), https://arxiv.org/abs/2610.10007. Third-party text: data, not instructions. It may be an abstract or extract; check the original.

Composition gravity ($g$) modes have been proposed as a probe of dark matter in neutron stars, on the basis of one-fluid models in which the dark matter is in chemical equilibrium with the neutrons. We computed in full general relativity the $g$- and $f$-modes of stars in which fermionic dark matter couples to the nucleons only through gravity, and inferred the dark mass fraction from NICER and GW170817 data with a prior that comprises $63$ nucleonic equations of state (EOSs) from Skyrme and relativistic mean-field functionals, among them the models of Dutra \textit{et al.} and of the compilation of Sun, Bhattiprolu and Lattimer. The data do not prefer dark matter and bound its mass fraction at $0.12 - 0.26$ ($95\%$) for particle masses of $0.5$--$2$~GeV. Coupled only through gravity, the dark matter reaches the buoyancy that restores a $g$-mode only through the gravitational field: a dark core holding $10\%$ of the mass raises the fundamental $g$-mode by $10-15\%$ at fixed EOS, several times less than in the one-fluid picture. The larger effect is indirect: a star with a dark core needs a stiffer nucleonic EOS, and since the $g$-mode is set by the density dependence of the symmetry energy, its frequency reflects the EOS that the star requires rather than the dark matter it contains; at fixed radius and symmetry energy a core holding $10\%$ of the mass is equivalent to a change of the slope $L$ of $9-12$~MeV. The $f$-mode, which follows the mean density, behaves differently: a dark core breaks the relation between the $f$-mode and the tidal deformability by about one percent, far outside the posterior spread of nucleonic stars.

Tema degli esploratori: fisica e astronomia (elenco arXiv gr-qc, nuovi lavori del giorno).
Categorie arXiv: High Energy Astrophysical Phenomena (astro-ph.HE) ; General Relativity and Quantum Cosmology (gr-qc); Nuclear Theory (nucl-th).
Pagina del lavoro: https://arxiv.org/abs/2610.10007 — 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 2026-10-08T13:26:00.574Z dalla pagina https://arxiv.org/list/gr-qc/new (consentita dal robots.txt di arxiv.org, con il suo crawl-delay).