Searcharxiv⌕ Search
Home/Archive/arXiv

arXiv · gr-qc/0206056

Quantum phase shift and neutrino oscillations in a stationary, weak gravitational field

Bernard Linet·Pierre Teyssandier
View original source ↗Read source document ↗Export metadata ↓

Abstract

A new method based on Synge's world function is developed for determining within the WKB approximation the gravitationally induced quantum phase shift of a particle propagating in a stationary spacetime. This method avoids any calculation of geodesics. A detailed treatment is given for relativistic particles within the weak field, linear approximation of any metric theory. The method is applied to the calculation of the oscillation terms governing the interference of neutrinos considered as a superposition of two eigenstates having different masses. It is shown that the neutrino oscillations are not sensitive to the gravitomagnetic components of the metric as long as the spin contributions can be ignored. Explicit calculations are performed when the source of the field is a spherical, homogeneous body. A comparison is made with previous results obtained in Schwarzschild spacetime.

Explore related subjects

gr-qcastro-phhep-ph

Keep this discovery

Explore connections, maps & timelines

BibTeXRIS

Bernard Linet, Pierre Teyssandier. 2011-08-09. Quantum phase shift and neutrino oscillations in a stationary, weak gravitational field. https://doi.org/10.1142/s0217732311036115

Cite the original work for its findings. Save a collection to share your selection of sources.

KEEP EXPLORING

Related papers

arXiv2026

Novel thermodynamic inequality for rotating AdS black holes

We propose a new thermodynamic inequality for stationary, asymptotically Anti-de Sitter rotating black holes, expressed in terms of their angular momentum, mass and thermodynamic volume as $ 4πJ^2/(3MV)<1 $. For the solutions considered, this inequality follows from the requirement that the thermodynamic identities admit a physical horizon with positive area. We examine Kerr(-Newman)-AdS, Kerr-Sen-AdS, pairwise-equal four-charge AdS black holes, charged rotating AdS black strings, and charged rotating AdS C-metrics, finding strong supporting evidence for the inequality across different horizon topologies. We then reformulate the inequality in terms of the underlying metric parameters and compare the resulting constraints with the corresponding regularity and horizon-existence conditions. This analysis shows that the proposed inequality has different physical content for different geometries. We further examine charged super-entropic black holes, for which the ultraspinning limit leads instead to a lower bound on the thermodynamic ratio. This result is consistent with the violation of the reverse isoperimetric inequality characteristic of super-entropic solutions. Moreover, when combined with the refined reverse isoperimetric inequality, the proposed bound ensures the physicality of the Kerr-AdS reference solution entering the refined bound and thereby yields the conventional reverse isoperimetric inequality. We also extend the proposed relation to higher dimensions and test it for singly spinning thin AdS black ring with nonspherical horizon topology, finding that the corresponding inequalities are satisfied throughout the thin-ring regime.

gr-qc↗
arXiv2026

Varying Newton constant, entropy and the black hole evaporation law

We assume that the Newton potential of a spherically symmetric body of mass $M$ is $V=-G(M)Mr^{-1}$, where the Newton constant $G$ may depend on $M$. We insert this assumption in the Schwarzschild solution. We discuss varying $G$ in the black hole thermodynamics and black hole evaporation law. We extend the Bekenstein-Hawking formula $\hbar GS=\frac{1}{4}A$, where $S$ is the entropy and $ A$ the area, to a varying $G$. It is shown that if $G(M)$ is of the form of a power-law $G\simeq M^{-Γ}$ then $G(M)S\simeq A$ is still preserved but the evaporation law substantially depends on the function $G(M)$.

gr-qc↗
arXiv2026

Relativistic mode sums for neutron-star tidal response

Time-dependent tidal interactions during the late inspiral of binary neutron stars encode valuable information about neutron-star structure, but systematically extending the familiar Newtonian mode-sum picture into full general relativity is nontrivial. In this paper, we develop a practical relativistic implementation of mode-sum tidal response for non-rotating neutron stars in Regge-Wheeler gauge. Using near-zone boundary conditions, we systematically define the interior tidal field, the relativistic overlap integrals, and the corresponding mode amplitudes. The good is that the dominant f-mode contribution is remarkably robust, reproducing the direct matching calculation to within $\sim 3$\% across the equations of state we consider. The bad is that the operator governing mode inner product is not positive definite on the full Regge-Wheeler-gauge function space, so the relativistic mode sum truncated at ${\cal{O}}(ω^2)$ is not expected to strictly converge to the direct matching solution. The subtle is that the tidal field inside the star is not unique, although this ambiguity has only a limited impact on the dominant f-mode response for the classes of extensions studied here. Our results establish the practical utility of relativistic mode-sum approximations, while making clear that their predictive power comes from a controlled low-mode description, rather than from a formally convergent strong-field expansion.

gr-qc↗