Black holes with toroidal horizons in ( $$d+1$$ d + 1 )-dimensional space-time

Sharifian, Elham; Mirza, Behrouz; Mirzaiyan, Zahra

doi:10.1007/s10714-017-2313-9

Cited by 2 publications

(2 citation statements)

References 51 publications

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“…70 Furthermore, the mass parameter µ and the conserved mass M are related via µ = 2M/π. 70 The Bekenstein-Hawking entropy S still satisfies the area law…”

Section: Solutions With Flat Horizon Structurementioning

confidence: 99%

Charged slowly rotating toroidal black holes in the (1 + 3)-dimensional Einstein-power-Maxwell theory

Panotopoulos

Rincón

2019

Int. J. Mod. Phys. D

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In this work we find charged slowly rotating solutions in the four-dimensional Einsteinpower-Maxwell non-linear electrodynamics assuming a negative cosmological constant. By solving the system of coupled field equations explicitly we obtain an approximate analytical solution in the small rotation limit. The solution obtained is characterized by a flat horizon structure, and it corresponds to a toroidal black hole. The Smarr's formula, the thermodynamics and the invariants Ricci scalar and Kretschmann scalar are briefly discussed. September 5,2018 1:0 WSPC/INSTRUCTION FILE Toroidal˙Black˙Hole˙IV 2 BHs do exist in Nature and they merge. In the light of this development the socalled quasinormal modes ω = ω R + iω I , with a non-vanishing imaginary part, have become very relevant, since they do not depend on the initial conditions, and they thus carry unique information on the few BH parameters. 12-14 Therefore it becomes clear that BHs are exciting objects that link together several areas of research, from gravity, to astrophysics, to quantum physics, to thermodynamics and statistical physics, and they have become an excellent laboratory to study and understand various aspects of classical and quantum gravity.Soon after the formulation of GR, the Schwarzschild 15 as well as the Reissner-Nordström 16 solutions were obtained, characterized by the mass and the electric charge, respectively, and much later the Kerr solution 17 for rotating BHs was found. The theoretical paradigm of the no-hair theorem, 18 according to which BHs are uniquely characterized by its mass, electric and/or magnetic charge and angular momentum (although counter examples do exist. See e.g. the recent reviews 19, 20 on hairy BHs), the Smarr's formula, 21,22 and the area law of the BH entropy, 5, 6 are valid in GR coupled to Maxwell's linear electrodynamics in (1+3) dimensions. There are, however, good theoretical reasons to consider alternative theories of gravity, or non-linear electrodynamics or extra dimensions. In all of these cases some of the previous conditions are modified or violated.Kaluza-Klein theories, 23, 24 supergravity 25 and Superstring/M Theory 26, 27 have pushed forward the idea that extra spatial dimensions may exist. In more than four dimensions higher order curvature terms are natural in Lovelock theory, 28 and also higher order curvature corrections appear in the low-energy effective equations of Superstring Theory. 29 Furthermore, gravity in (1+2) dimensions is special and has attracted a lot of attention due to the deep connection to a Yang-Mills theory with the Chern-Simons term only, 30-32 and also due to its mathematical simplicity as there are no propagating degrees of freedom. What is more, the current cosmic acceleration 33, 34 and the cosmological constant problem 35 have forced us to explore other possibilities modifying the gravitational theory, and studying e.g. f (R) theories of gravity 36, 37 or scalar-tensor theories of gravity 38 or brane models. 39 In addition, non-linear electrodynamics has attracted a lot...

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“…70 Furthermore, the mass parameter µ and the conserved mass M are related via µ = 2M/π. 70 The Bekenstein-Hawking entropy S still satisfies the area law…”

Section: Solutions With Flat Horizon Structurementioning

confidence: 99%

Charged slowly rotating toroidal black holes in the (1 + 3)-dimensional Einstein-power-Maxwell theory

Panotopoulos

Rincón

2019

Int. J. Mod. Phys. D

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“…[82], the concept of the torus-like black hole was first introduced. This work has inspired many studies of the torus-like black hole, including the statistical entropy [83], the weak cosmic censorship conjecture [84,85], the tunneling radiation [86], heat engine [87], the dBB quantization [88], and other aspects [89][90][91]. Unlike previous studies, the topology of this space-time is S × S × M 2 .…”

Section: Introductionmentioning

confidence: 99%

Joule–Thomson expansion of the torus-like black hole

Liang

Lin

2021

Eur. Phys. J. Plus

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In this paper, we study the Joule-Thomson expansion of the torus-like black hole in extended phase space, where the cosmological constant is determined by the pressure. It is noteworthy that the torus-like black hole has a horizon of toroidal topology, rather than a horizon of spherical topology. We study both the inversion and isenthalpic curves of the torus-like black holes in the T − P plane and find that their intersection coincides with the inversion point that distinguishes the heat in the cooling process. Compared to the Van der Waals fluid, the inversion curves of torus-like black holes do not end at any point and only lower inversion curves are available. Most importantly, we find that the P − V diagram of the torus-like black hole has no inflection point, i.e., the torus-like black hole is always thermally stable. Therefore, the torus-like black hole has no critical point and critical temperature, and there is no ratio between the minimum inversion temperature and the critical temperature.

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Black holes with toroidal horizons in ( $$d+1$$ d + 1 )-dimensional space-time

Cited by 2 publications

References 51 publications

Charged slowly rotating toroidal black holes in the (1 + 3)-dimensional Einstein-power-Maxwell theory

Charged slowly rotating toroidal black holes in the (1 + 3)-dimensional Einstein-power-Maxwell theory

Joule–Thomson expansion of the torus-like black hole

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