TL;DR
This paper demonstrates that rotating black holes can support extremely short-range scalar configurations, challenging the traditional 'no short hair' theorem which applies only to spherically symmetric static black holes.
Contribution
It provides analytical evidence that the 'no short hair' theorem does not hold for rotating black holes, showing they can have very short scalar 'hair' in their exterior regions.
Findings
Rotating black holes can support short scalar 'clouds'.
The Klein-Gordon-Kerr-Newman wave equation was solved analytically.
Short scalar configurations exist in the regime of large scalar masses.
Abstract
The elegant `no short hair' theorem states that, if a spherically-symmetric static black hole has hair, then this hair must extend beyond 3/2 the horizon radius. In the present paper we provide evidence for the failure of this theorem beyond the regime of spherically-symmetric static black holes. In particular, we show that rotating black holes can support extremely short-range stationary scalar configurations (linearized scalar `clouds') in their exterior regions. To that end, we solve analytically the Klein-Gordon-Kerr-Newman wave equation for a linearized massive scalar field in the regime of large scalar masses.
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