Search arXiv⌕ Search

arXiv · 2609.40166

Axion corrections to photon superradiant scattering by Kerr black holes

Abstract

We study photon superradiant scattering by a Kerr black hole in the presence of an axion-photon coupling and investigate how this coupling modifies the electromagnetic amplification factor. We solve the coupled axion and electromagnetic equations in a fully relativistic framework. We distinguish two regimes according to the relation between the sourced axion frequency and the axion mass. In the radiative regime, the axion can propagate to spatial infinity and carry away energy, thereby suppressing photon amplification. In the subthreshold regime, the axion is confined by the mass barrier and exchanges energy with the black-hole horizon through quasibound-state excitations. In this regime, photon amplification can be either enhanced or suppressed, depending on whether the relevant axion modes satisfy the superradiance condition.

Explore related subjects

Keep this discovery

Explore connections, maps & timelines

BibTeXRIS

Zhi-Qing Zhu, Jun Zhang. 2026-09-30. Axion corrections to photon superradiant scattering by Kerr black holes. https://arxiv.org/abs/2609.40166

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

KEEP EXPLORING

Related papers

Primordial black hole formation in matter domination

We study Primordial Black Holes (PBHs) formed by the collapse of rare primordial fluctuations during an early period of Matter Domination. The collapse threshold strongly depends on the shape of the peaks, decreasing as they become flatter and hence rarer. In the extreme limit of a top-hat perturbation, Harada, Kohri, Sasaki, Terada, and Yoo have argued that the growth of velocity dispersion prevents the formation of black holes unless the initial peak is larger than $ζ_{\rm th} \sim ζ_{\rm rms}^{2/5}$. Including the shape distribution of the peaks, we find that for a realistic cosmic abundance of PBHs, the effective threshold is larger, $ζ_{\rm th} \sim ζ_{\rm rms }^{1/10}$. And this model requires $ζ_{\rm rms}\sim 10^{-1}$, which is much larger than the observed value at the CMB scales. Hence, PBH formation during Matter Domination is barely more efficient than Radiation Domination. We estimate the dimensionless spin parameter to be $a_{\rm rms} \sim ζ_{\rm rms}^{7/4}\ll 1$, slightly larger than PBHs formed in Radiation Domination.

gr-qc↗

Interaction of fluids described through relative motion and application to Bianchi type-I spacetimes

We study a model of two fluids with an interaction that depends on their relative motion. The interaction is described using the particle number density of each fluid measured in the rest frame of the other, providing a geometric interpretation of a class of interactions studied in relativistic multifluid theory. We derive the corresponding stress-energy tensor and show that its structure agrees with established results. In particular, the interaction introduces a dependence on the scalar product of the $4$-velocities, which can be expressed in terms of the relative speed of the fluid elements. Furthermore, the relative motion produces unequal pressures along and perpendicular to the direction of motion, together with an energy flux. As an application, we consider a Bianchi type-I universe dominated by one fluid, with the second fluid acting as a source of small anisotropy. We examine how the interaction influences the relative speed and the evolution of cosmological anisotropy. We identify conditions under which the anisotropy decays in the late-time limit, generalizing results for non-interacting fluids from the literature.

gr-qc↗

Perfect fluids revisited: an action principle approach

We revisit the variational principle for relativistic perfect fluids in a manifestly covariant formulation based on differential forms, with particular attention to the boundary data required for a well-posed action principle. For timelike flows, the formulation reproduces the standard formulation of Schutz and Brown. We then examine the extension obtained by replacing proper time normalization of the velocity with a nullity constraint, with the he Bi{\v c}{á}k-Kucha{\v r} null dust action emerging as a special case. Requiring the complete action to be invariant under local rescalings of the null flow vector imposes the condition that the energy density depend only on the entropy per particle. For this class of null flows, the conventional equilibrium condition, \textit{i.e.}, that the energy density is convex, fails at non-zero temperatures, therefore limiting the interpretation of the fluid as an ordinary thermodynamic system.

gr-qc↗