Video and Audio Data

arasitic black holes. The swallowing of a fuzzy dark matter soliton. Time evolution of BH mass (top panel), scalar field (bottom left), and energy flux (bottom right). Initial boson star mass is 15 times heavier than initial black hole mass. Initial boson star size is 600 times larger than black hole radius. arXiv:2207.09469v1.

Piercing of boson stars by a black hole (I). A black hole of unit mass colliding with a boson star of mass 0.53. The collision happens at 50% the speed of light. arXiv:2206.00021.

Piercing of boson stars by a black hole (II). A black hole of unit mass colliding with a boson star of mass 0.53. The collision happens at 50% the speed of light. Right panel: a black hole of mass 0.1 colliding with a boson star of mass 0.53. The collision happens at 50% the speed of light. arXiv:2206.00021.

High energy black hole collisions. The collision of two boosted black holes (v=0.75c in the center of mass frame), with a finite impact parameter in asymptotically flat spacetime. About 24% of the center of mass frame can be released as radiation, for this collision. The final hole is nearly maximally spinning. The intensity of the color refers to the amplitude of the gravitational waves as measured by Ψ₄. arXiv:0907.1252.

Black hole bombs I: Scalar fields. The time evolution of a massive scalar field around a highly spinning black holes. The scalar field is initially in a bound state, and continues to be for thousands of orbital periods. Colors depict field intensity. arXiv:1212.0551.

Black hole bombs II: Vector fields. The time evolution of a massive vector field around a highly spinning black holes. The vector field is initially a generic gaussian. Colors depict field intensity. arXiv:1212.0551.

Black hole collisions in de Sitter spacetime. Two black holes of sufficiently large mass in de Sitter spacetime would, upon merger, give rise to too large a black hole to fit in its cosmological horizon, resulting in a naked singularity. We here test such a configuration. Even though the initial separation is very small, we find that the holes move away from each other, with a proper separation increasing as the simulation progresses. arXiv:1204.2019.

Bursts of light from axion clouds (I). The evolution of an axion Phi of mass mu=0.2 and of the electromagnetic scalar E²-B² in the background of a Kerr BH (a=0.5). The initial axion configuration describes a cloud around a spinning black hole, grown by superradiance.

When superradiance is turned off and the initial amplitude of the axion is small, any vector perturbation dies off quickly. arXiv:1811.04950.

Bursts of light from axion clouds (II). When superradiance is turned off and the initial amplitude of the axion is large, an instability is triggered and gives rise to a EM burst. arXiv:1811.04950.

Bursts of light from axion clouds (III). When superradiant growth is included, even a small initial axion amplitude eventually grows large and triggers EM bursts, blasts of laser-like electromagnetic radiation. This blasts lowers the axion to sub-critical values, until superradiance dominates again. arXiv:1811.04950.

Turbulent accretion disk around a supermassive black hole (I). The turbulent gas flow stochastically excites the quasinormal modes of the central black hole which leads to gravitational wave emission.

Turbulent accretion disk around a supermassive black hole (II). See description above.