Search arXiv⌕ Search

arXiv · 2610.38746

Bosonic Dark Matter Cores Can Screen Scalar-Tensor Gravity

Abstract

We examine the observational viability of scalarized fermion-boson stars (FBSs) in massless Damour-Esposito-Farèse gravity, using the MPA1 nuclear equation of state and a self-interacting complex scalar field playing the role of an ultralight bosonic dark matter model. Constraining stellar models within a multi-messenger-motivated mass-radius window, we obtain three main results: First, bosonic dark matter acts as a catalyst for spontaneous scalarization. Second, energetically favored configurations are scalarized FBSs featuring bosonic dark matter cores that reconcile strongly coupled regimes with radius bounds. Third, dark matter cores tend to suppress scalar charges, which mimics the effect of a massive gravitational scalar field and could contribute to evade observational constraints. Additionally, the exclusive prediction of scalarized FBSs at high masses suggests a way to test this theoretical scenario.

Explore related subjects

Keep this discovery

Explore connections, maps & timelines

BibTeXRIS

Jorge Castelo Mourelle, Saeed Fakhry, Néstor Ortiz. 2026-10-28. Bosonic Dark Matter Cores Can Screen Scalar-Tensor Gravity. https://arxiv.org/abs/2610.38746

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

KEEP EXPLORING

Related papers

Self-force in hyperbolic black hole encounters

Self-force methods can be applied in calculations of the scatter angle in two-body hyperbolic encounters, working order by order in the mass ratio (assumed small) but with no recourse to a weak-field approximation. This, in turn, can inform ongoing efforts to construct an accurate description of the general-relativistic binary dynamics via an effective-one-body description or other approaches. Existing self-force methods are to a large extent specialised to bound, inspiral orbits. Here we derive the first-order conservative self-force correction to the scattering angle, show its agreement with recent post-Minkowsian results, and develop a technique for (numerical) self-force calculations that can efficiently tackle scatter orbits. In the method, the metric perturbation is reconstructed from a Hertz potential that satisfies (mode-by-mode) a certain inhomogeneous version of the Teukolsky equation. The crucial ingredient in this formulation are certain jump conditions that the (multipole modes of the) Hertz potential must satisfy along the worldline of the small body's orbit. We present a closed-form expression for these jumps, for an arbitrary geodesic orbit in Schwarzschild spacetime. To begin developing the numerical infrastructure, a scalar-field evolution code on a Schwarzschild background (in 1+1D) is developed. Following this, results for the conservative scalar self-force corrections to the scatter angle are calculated. We continue by constructing a Teukolsky evolution code on a Schwarzschild background. This produces numerically unstable solutions due to unphysical homogeneous solutions of the Teukolsky equation at the horizon and null infinity being seeded by numerical error. This can be resolved by a change of variables to a Regge-Wheeler-like field. We then present a full numerical implementation of this method for circular and scatter orbits in Schwarzschild.

gr-qc↗

Quasinormal Ringing of de Sitter Braneworlds

Compared with the Poincaré braneworld, the de Sitter (dS) braneworld aligns more closely with the present universe characterized by a small but finite cosmological constant; to explore the quasinormal ringing properties within the dS brane scenario, we investigate gravitational perturbations in both thin and thick dS brane configurations. Analysis of the perturbation equations reveals that the effective potential along the extra dimension exhibits the shape of a Pöschl-Teller potential, asymptotically approaching a constant value (mass gap) at infinity, and in particular this mass gap can be reduced. Analytical calculations further indicate that the gravitational perturbations, apart from the zero mode, possess a series of discrete, purely imaginary quasinormal modes in the late stages, implying that these perturbations decay without oscillation over time; the analytical findings also demonstrate that the brane structure primarily determines the distribution of the quasinormal spectrum while preserving the purely imaginary nature of the quasinormal frequencies. Subsequently, we further simulate the gravitational wave signal by numerically evolving the perturbation equations, which yields late-stage results consistent with the analytical predictions. Interestingly, these quasinormal modes carry information about the cosmological constant on the brane, which provides a potential new pathway for the study of cosmology in the dS brane scenario.

gr-qc↗

Beyond quasinormal modes: a complete mode decomposition of black hole perturbations

We show that retarded Green's functions of black hole spacetimes can be expressed as a convergent mode sum everywhere in spacetime. At late times a quasinormal mode sum converges, while at early times a Matsubara (or, Euclidean) mode sum converges. The two regions are separated by a lightcone which scatters from the black hole potential. The Matsubara sum is a Fourier series on the Euclidean thermal circle associated to the early time region. We illustrate our results for Pöschl-Teller, BTZ, and Schwarzschild. In the case of Schwarzschild, we express the branch cut contribution as a convergent sum of de Sitter quasinormal modes as $Λ\to 0^+$, and exploit recent exact solutions to the Heun connection problem. In each case we analytically show convergence by studying the asymptotics of residue sums and also provide numerical demonstrations.

gr-qc↗