Kerr black holes with scalar hair.

By Carlos A. R. Herdeiro, Eugen Radu. Physical Review Letters, 2014

616 citations recorded by the source corpus.

We present a family of solutions of Einstein's gravity minimally coupled to a complex, massive scalar field, describing asymptotically flat, spinning black holes with scalar hair and a regular horizon. These hairy black holes (HBHs) are supported by rotation and have no static limit. Besides mass M and angular momentum J, they carry a conserved, continuous Noether charge Q measuring the scalar hair. HBHs branch off from the Kerr metric at the threshold of the superradiant instability and reduce to spinning boson stars in the limit of vanishing horizon area. They overlap with Kerr black holes for a set of (M, J) values. A single Killing vector field preserves the solutions, tangent to the null geodesic generators of the event horizon. HBHs can exhibit sharp physical differences when compared to the Kerr solution, such as J/M^{2}>1, a quadrupole moment larger than J^{2}/M, and a larger orbital angular velocity at the innermost stable circular orbit. Families of HBHs connected to the Kerr geometry should exist in scalar (and other) models with more general self-interactions.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/8ebd13c22580aa675768a0b239ab1b12f21ad46a

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Nuclear and High Energy Physics

Citations in the corpus

Born–Infeld inspired modifications of gravity (2017, background): “Finally there are apparent counterexamples of solutions with hair when adding the new ingredient of superradiance [205] (see [206] for a recent review), with related intensive searches for observational discriminations from the Kerr solution [98].”
Superradiance: Energy Extraction, Black-Hole Bombs and Implications for Astrophysics and Particle Physics (2015, methodology): “BH superradiance is also associated to the existence of new asymptotically flat, hairy BH solutions [12] and to phase transitions between spinning or charged black objects in asymptotically AdS spacetime [13, 14, 15] or in higher dimensions [16].”
Constraining the mass of dark photons and axion-like particles through black-hole superradiance (2018, background): “Note, however, that the stationary hairy black holes [36] that exist in this case above the superradiant threshold for a given azimuthal quantum number m, were recently found to be unstable against nonaxisymmetric perturbations with azimuthal number larger than m and in the superradiant regime [37],”
Numerical methods for finding stationary gravitational solutions (2015, methodology): “If we replace the AdS boundary of [41] by a Dirichlet boundary sourced by the mass of a scalar in Λ = 0, the solution of [41] survives and describes a hairy Kerr black hole [225].”
Testing black hole candidates with electromagnetic radiation (2015, methodology): “An important example of the violation of the no-hair theorem was presented in (Herdeiro & Radu, 2014), in which hairy BHs are possible by combining rotation with a harmonic time-dependence in the scalar field.”
Probing ultralight bosons with binary black holes (2018, background): “e Rabi frequency, we have (t) 1 (t0) 1 ˘ Mc(t) Mc(t0) ˘e 2A(t;t0) : (4.10) 20Exact solutions with (complex) scalar hair around spinning BHs have been studied numerically in the literature, see e.g. [122]. In principle, these quasi-stationary spacetimes can also have ˛1. 21For q .1, the virial theore”
Kerr black holes with Proca hair (2016, methodology): “Thus, following [1], we define the normalised Noether charge, q, as”
Black holes with scalar hair in light of the Event Horizon Telescope (2020, background): “For an inevitably incomplete list of important studies related to the construction and identification of observational signatures of HBHs in various theories of gravity or in the presence of various different types of matter fields, see for instance [5–54].”
Dynamical boson stars (2012, background): “(85) implies that the stress-energy tensor is independent of {t, φ}, and are generically known as Kerr BHs with scalar hair [257].”