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Spin-induced Scalar Clouds around Kerr-Newman Black Holes
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Recent studies have demonstrated that a scalar field non-minimally coupled to the electromagnetic field can experience a spin-induced tachyonic instability near Kerr-Newman black holes, potentially driving the formation of scalar clouds. In this paper, we construct such scalar clouds for both fundamental and excited modes, detailing their existence domains and wave functions. Our results indicate that a sufficiently strong coupling between the scalar and electromagnetic fields is essential for sustaining scalar clouds. Within the strong coupling regime, black holes that rotate either too slowly or too rapidly are unable to support scalar clouds. Furthermore, we observe that scalar cloud wave functions are concentrated near the black hole's poles. These findings provide a foundation for future investigations of spin-induced scalarized Kerr-Newman black holes.
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Spin-induced Scalarized Black Holes in Einstein-Maxwell-scalar Models
Spin-induced scalarized Kerr-Newman black holes are constructed numerically for negative coupling, and they coexist with stable, entropically favored Kerr-Newman black holes.
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