Effect of scalar field mass on gravitating charged scalar solitons and black holes in a cavity

Ponglertsakul, Supakchai; Winstanley, Elizabeth

doi:10.1016/j.physletb.2016.10.073

Cited by 28 publications

(45 citation statements)

References 12 publications

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“…If the system has electric charge, we can also have static black hole bomb systems [2][3][4][5][6][7][8][9][10][11][12][13][14][15][16][17][18][19]. All we need is a complex scalar field with charge q scattering a Reissner-Nordström black hole with chemical potential µ that is placed inside a box that reflects the scalar waves.…”

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confidence: 99%

Evading no-hair theorems: Hairy black holes in a Minkowski box

Dias

Masachs

2018

Phys. Rev. D

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We find hairy black holes of Einstein-Maxwell theory with a complex scalar field that is confined inside a box in a Minkowski background. These regular hairy black holes are asymptotically flat and thus the presence of the box or mirror allows to evade well-known no-hair theorems. We also find the Israel surface stress tensor that the confining box must have to obey the energy conditions. In the zero horizon radius limit, these hairy black holes reduce to a regular asymptotically flat hairy soliton. We find our solutions using perturbation theory. At leading order, a hairy black hole can be seen as a Reissner-Nordstrom black hole placed on top of a hairy soliton with the same chemical potential (so that the system is in thermodynamic equilibrium). The hairy black holes merge with the Reissner-Nordstrom black hole family at the onset of the superradiant instability. When they co-exist, for a given energy and electric charge, hairy black holes have higher entropy than caged Reissner-Nordstrom black holes. Therefore, our hairy black holes are the natural candidates for the endpoint of charged superradiance in the Reissner-Nordstrom black hole mirror system. * Electronic address: ojcd1r13@soton.ac.uk † Electronic address: rmg1e15@soton.ac.uk

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confidence: 99%

Evading no-hair theorems: Hairy black holes in a Minkowski box

Dias

Masachs

2018

Phys. Rev. D

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“…Including charged scalars, boson stars and hairy black holes in a cavity were considered in [21][22][23][24], which showed that the phase structure of the gravity system in a cavity is strikingly similar to that of holographic superconductors in the AdS gravity. The stabilities of solitons, stars and black holes in a cavity were also studied in [25][26][27][28][29][30][31][32]. It was found that the nonlinear dynamical evolution of a charged black hole in a cavity could end in a quasi-local hairy black hole.…”

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Thermodynamics and phase transition of a nonlinear electrodynamics black hole in a cavity

Wang

Yang

2019

J. High Energ. Phys.

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We discuss the thermodynamics of a general nonlinear electrodynamics (NLED) asymptotically flat black hole enclosed in a finite spherical cavity. A canonical ensemble is considered, which means that the temperature and the charge on the wall of the cavity are fixed. After the free energy is obtained by computing the Euclidean action, it shows that the first law of thermodynamics is satisfied at the locally stationary points of the free energy. Focusing on a Born-Infeld (BI) black hole in a cavity, the phase structure and transition in various regions of the parameter space are investigated. In the region where the BI electrodynamics has weak nonlinearities, Hawking-Pagelike and van der Waals-like phase transitions occur, and a tricritical point appears. In the region where the BI electrodynamics has strong enough nonlinearities, only Hawking-Page-like phase transitions occur. The phase diagram of the BI black hole in a cavity can have dissimilarity from that of a BI black hole using asymptotically anti-de Sitter boundary conditions. The dissimilarity may stem from a lack of an appropriate reference state with the same charge and temperature for the BI-AdS black hole.

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“…Our compact theorem therefore reveals the interesting fact that, as opposed to stationary scalar fields [12,13,[27][28][29][30][31], static self-gravitating scalar fields whose nonlinear selfinteraction potential V (ψ 2 ) is a monotonically increasing function of its argument cannot form spatially regular asymptotically flat boson stars.…”

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confidence: 99%