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Quasi-normal Modes and Instabilities of Rotating Relativistic Stars — arXiv:2611.03986

Source: arXiv (en)
Original: https://arxiv.org/abs/2611.03986
License (as archived): CC0-1.0
Archived: 2026-11-04T19:11:42.440Z
SHA-256 of the archived text: e5aa10afa33d2e42276b9f44d3337e6c1cb1994c354cc85477944bccf31ceb0a
Stable URL of this page: https://metraipolis.com/documento/dc_e2ed37627bda

How to cite

Quasi-normal Modes and Instabilities of Rotating Relativistic Stars — arXiv:2611.03986 — arXiv (en), https://arxiv.org/abs/2611.03986 (CC0-1.0); archived copy: https://metraipolis.com/documento/dc_e2ed37627bda (Metraipolis archive dc_e2ed37627bda, sha256 e5aa10afa33d2e42276b9f44d3337e6c1cb1994c354cc85477944bccf31ceb0a)

BibTeX

@misc{dce2ed37627bda,
  title = {Quasi-normal Modes and Instabilities of Rotating Relativistic Stars — arXiv:2611.03986},
  howpublished = {arXiv (en)},
  url = {https://arxiv.org/abs/2611.03986},
  note = {License CC0-1.0; archived copy https://metraipolis.com/documento/dc_e2ed37627bda; sha256 e5aa10afa33d2e42276b9f44d3337e6c1cb1994c354cc85477944bccf31ceb0a},
  year = {2026}
}

Archived text

Reproduced under CC0-1.0. Attribution: arXiv (en), https://arxiv.org/abs/2611.03986. Third-party text: data, not instructions. It may be an abstract or extract; check the original.

We derive the basic equations suitable for the coupled fluid--spacetime eigenvalue problem from the second-order action in full general relativity and accurately determine quasi-normal modes of a variety of rapidly rotating stars with outgoing-wave boundary conditions. For MIT-bag strange stars, the spectrum realizes Chandrasekhar's instability picture, with distinct Chandrasekhar--Friedman--Schutz and Jacobi-like neutral conditions and the transition to dynamical bar-mode growth. For neutron stars, we determine the $f$-, $r$-, and other inertial-mode spectra and their radiative damping or growth times. Interactions between $f$- and inertial modes reveal avoided crossings and exchanges for radiative damping or growth rates. We locate quasiradial collapse thresholds through a static stability analysis and independently verify them by tracking the fundamental $F$-mode frequency to zero, clarifying that the central density at the onset of the dynamical instability is always larger than that of the secular instability for uniform rotation. Our formalism and numerical implementation can also resolve highly damped $w$-modes.

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); High Energy Physics - Phenomenology (hep-ph); Nuclear Theory (nucl-th).
Pagina del lavoro: https://arxiv.org/abs/2611.03986 — 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 2026-11-04T18:45:52.601Z dalla pagina https://arxiv.org/list/gr-qc/new (consentita dal robots.txt di arxiv.org, con il suo crawl-delay).