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Tidal deformability of white dwarfs in Eddington-inspired Born-Infeld gravity — arXiv:2610.19629

Source: arXiv (en)
Original: https://arxiv.org/abs/2610.19629
License (as archived): CC0-1.0
Archived: 2026-10-15T14:59:02.749Z
SHA-256 of the archived text: a3e7c6ca32eda848cc0cd49063bde1e1000f66772c853654e4d2a1e088a4afb1
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How to cite

Tidal deformability of white dwarfs in Eddington-inspired Born-Infeld gravity — arXiv:2610.19629 — arXiv (en), https://arxiv.org/abs/2610.19629 (CC0-1.0); archived copy: https://metraipolis.com/documento/dc_3ca8d2a0bbcf (Metraipolis archive dc_3ca8d2a0bbcf, sha256 a3e7c6ca32eda848cc0cd49063bde1e1000f66772c853654e4d2a1e088a4afb1)

BibTeX

@misc{dc3ca8d2a0bbcf,
  title = {Tidal deformability of white dwarfs in Eddington-inspired Born-Infeld gravity — arXiv:2610.19629},
  howpublished = {arXiv (en)},
  url = {https://arxiv.org/abs/2610.19629},
  note = {License CC0-1.0; archived copy https://metraipolis.com/documento/dc_3ca8d2a0bbcf; sha256 a3e7c6ca32eda848cc0cd49063bde1e1000f66772c853654e4d2a1e088a4afb1},
  year = {2026}
}

Archived text

Reproduced under CC0-1.0. Attribution: arXiv (en), https://arxiv.org/abs/2610.19629. Third-party text: data, not instructions. It may be an abstract or extract; check the original.

We compute the static quadrupole Love number $k_2$ and the dimensionless tidal deformability $\Lambda$ of cold white dwarfs in Eddington-inspired Born-Infeld (EiBI) gravity. Matter couples to the physical metric while perturbation equations are solved in an auxiliary metric, so the physical tidal field near the surface depends on derivatives of the equation of state. This dependence is regular for a surface polytropic index $1<\Gamma_{\rm env}<3/2$, but not for the $\Gamma = 5/3$ Chandrasekhar equation of state. The mechanism, an algebraic map between the metric that carries perturbations and the metric that matter feels, is common to Palatini-type theories, so the same type of surface condition should apply to tidal calculations in this wider class. We use thermodynamically consistent envelopes that exactly reach zero enthalpy. At five masses from \(0.6\) to \(1.3\,\Msun\) and five sampled Born-Infeld couplings \(\kappa\), with $|\kappa|\le5\times10^6\,\mathrm{m^2}$, the EiBI-GR differences are approximately linear in $\kappa$. The largest absolute fractional shifts are \(3.89\times 10^{-5}\) in the stellar radius $R$, \(4.09\times 10^{-5}\) in $k_2$, and \(2.36\times 10^{-4}\) in $\Lambda$. Across nine envelope models, half the spread of each quantity relative to the baseline envelope is at most \(0.0186\) in $R$ and \(0.0857\) in \(k_2\), but only \(3.02\times 10^{-5}\) in \(\Lambda\) as the changes in \(k_2\) and \(R^5\) largely cancel. A high-precision calculation shows that the envelope dependence of the EiBI-GR difference in \(\Lambda\) is small. Half the spread of this difference ranges from \(1.067\times 10^{-12}\) to \(6.208\times 10^{-11}\) over the 20 nonzero mass-coupling points.

Tema degli esploratori: fisica e astronomia (elenco arXiv gr-qc, nuovi lavori del giorno).
Categorie arXiv: General Relativity and Quantum Cosmology (gr-qc) ; High Energy Physics - Theory (hep-th).
Pagina del lavoro: https://arxiv.org/abs/2610.19629 — 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 2026-10-15T14:04:38.502Z dalla pagina https://arxiv.org/list/gr-qc/new (consentita dal robots.txt di arxiv.org, con il suo crawl-delay).