Black Holes Grow a Fur Coat on the Fly express

Original: "Scalarization and descalarization in hyperbolic encounters of black holes"
arXiv:2606.30865 · 2026-06-29 · CC BY 4.0 · 1 min
When black holes approach each other at tremendous speed, a scalar field temporarily emerges around them.

Two black holes race past each other like Formula 1 cars on opposite lanes. In standard general relativity, they remain 'bald'—no extra fields appear around them. But if you add a scalar field to the equations (something like an invisible fog permeating space), the rules change.

The authors numerically simulated such encounters in a theory where gravity interacts with a scalar field in a special way. Initially, they set a barely noticeable field around the holes, like a light haze. Then they saw that during a close flyby, this haze can suddenly thicken. For a brief moment, a scalar fur coat appears — an effect physicists dubbed dynamical scalarization.

Interestingly, this trick works for both positive and negative coupling constants of the field to curvature: it all depends on the spin of the holes.

The most interesting part happens after the flyby. If during the encounter the black holes exchange angular momentum, their spin can change. Sometimes so much that one of the holes permanently acquires scalar 'hair' or, conversely, loses it. This permanent effect was dubbed spin (de)scalarization by the researchers.

The scalar field around a black hole can be imagined as an invisible 'fur coat' that appears only for certain values of mass and spin, like an animal changing its coat with the seasons.

In Robert Wilson's novel 'Spin', a mysterious barrier alters the properties of space — similar to how a scalar field manifests itself only under extreme gravitational conditions.

Scientists
John Archibald WheelerJacob BekensteinFritz ZwickyKarl SchwarzschildStephen HawkingSubrahmanyan Chandrasekhar
Concepts
spontaneous scalarization scalar hair black hole black hole tidal deformability scalar perturbations no-hair theorem ringdown binary stellar evolution modified gravity singularities hills mechanism stellar evolution Hawking area theorem event horizon stability hawking radiation mechanism photon sphere spiral critical collapse naked singularity spin parameter horizon area bubble collision