Editing No-hair theorem (section)

==Counterexamples==
Counterexamples in which the theorem fails are known in spacetime dimensions higher than four; in the presence of [[Non-abelian gauge theory|non-abelian]] [[Yang–Mills field]]s, non-abelian [[Proca action|Proca fields]], some [[minimal coupling|non-minimally coupled]] [[scalar fields]], or [[skyrmion]]s; or in some theories of gravity other than Einstein's general relativity. However, these exceptions are often unstable solutions and/or do not lead to conserved quantum numbers so that "The 'spirit' of the no-hair conjecture, however, seems to be maintained".<ref>{{cite arXiv |last=Mavromatos |first=N. E. |author-link=Nikolas Mavromatos |eprint=gr-qc/9606008v1 |title=Eluding the No-Hair Conjecture for Black Holes |date=1996 }}</ref> It has been proposed that "hairy" black holes may be considered to be bound states of hairless black holes and [[soliton]]s.

In 2004, the exact analytical solution of a (3+1)-dimensional spherically symmetric black hole with minimally coupled self-interacting scalar field was derived.<ref>{{cite journal |last=Zloshchastiev |first=Konstantin G. |journal=Phys. Rev. Lett. |volume=94 |pages=121101 |date=2005 |doi=10.1103/PhysRevLett.94.121101 |title=Coexistence of Black Holes and a Long-Range Scalar Field in Cosmology |issue=12 |bibcode=2005PhRvL..94l1101Z |arxiv = hep-th/0408163 |pmid=15903901|s2cid=22636577 }}</ref> This showed that, apart from mass, electrical charge and angular momentum, black holes can carry a finite [[Scalar field theory|scalar charge]] which might be a result of interaction with [[Inflation (cosmology)|cosmological]] scalar fields such as the [[inflaton]]. The solution is stable and does not possess any unphysical properties; however, the existence of a scalar field with the desired properties is only speculative.