# Obstructions towards a generalization of no-hair theorems: I. Scalar clouds around Kerr black holes

## TL;DR

This paper demonstrates that the integral method used in no-hair theorems fails for rotating black holes with scalar fields, providing a heuristic explanation for the existence of scalar hair around Kerr black holes, and highlights challenges in extending no-hair theorems.

## Contribution

It reveals the limitations of the integral method for no-hair theorems in rotating spacetimes and supports the existence of scalar hair around Kerr black holes through numerical analysis.

## Key findings

- Negative contribution due to rotation allows scalar hair existence.
- Integral vanishes only when no hair is present in non-rotating cases.
- Numerical solutions confirm scalar field eigenvalues in Kerr backgrounds.

## Abstract

We show that the integral method used to prove the no-hair theorem for Black Holes (BH's) in spherically symmetric and static spacetimes within the framework of general relativity with matter composed by a complex-valued scalar-field does not lead to a straightforward conclusion about the absence of hair in the stationary and rotating (axisymmetric) scenario. We argue that such a failure can be used to justify in a simple and heuristic way the existence of non-trivial boson clouds or hair found numerically by Herdeiro and Radu [1,2] and analytically by Hod in the test field limit [3-5]. This is due to the presence of a contribution that is negative when rotation exists which allows for an integral to vanish even when a non-trivial boson hair is present. The presence of such a negative contribution that depends on the rotation properties of the BH is perfectly correlated with the eigenvalue problem associated with the boson-field equation. Conversely, when the rotation is absent the integral turns to be composed only by non negative (i.e. positive semidefinite) terms and thus the only way it can vanish is when the hair is completely absent. This analysis poses serious challenges and obstructions towards the elaboration of no-hair theorems for more general spacetimes endowed with a BH region even when including matter fields that obey the energy conditions. Thus rotating boson stars, if collapsed, may lead indeed to a new type of rotating BH, like the ones found in [1,2]. In order to achieve this analysis we solve numerically the eigenvalue problem for the boson field in the Kerr-BH background by imposing rigorous regularity conditions at the BH horizon for the non-extremal case ($0<a<M$) which include the near extremal one in the limit $M\rightarrow a$, as well as the small BH limit $M\rightarrow a\rightarrow 0$.