Abstract:Recently, several methods have been proposed to regularize a D→4 limit of Einstein–Gauss–Bonnet (EGB), leading to nontrivial gravitational dynamics in 4D. We present an exact nonsingular black hole solution in the 4D EGB gravity coupled to non-linear electrodynamics and analyze their thermodynamic properties to calculate precise expressions for the black hole mass, temperature, and entropy. Because of the magnetic charge, the thermodynamic quantities are corrected, and the Hawking–Page phase transition is achi… Show more
“…Here, A = 4πr 2 + is the black hole event horizon area, and A 0 is a constant with the area units. This equation generalizes the Hawking-Bekenstein area formula [79] by a supplementary logarithmic term and third in the above expression is due to magnetic charge g. Notice that, in limit α → 0, we obtain the entropy of the Hayward black hole [24]. Here, it is interesting to note that entropy of nonsingular-AdS EGB black holes does not depend explicitly on the pressure P of the system, but the horizon radius r + of the black hole depends on pressure P ; hence the pressure of the black hole affects its entropy.…”
Section: ∂T ∂Rsupporting
confidence: 55%
“…is the Lagrangian density of the NED, which for the nonsingular black hole solutions we are interested in, is given as [24,55]…”
Section: IImentioning
confidence: 99%
“…Here, we want to obtain the static spherically symmetric black hole solutions of Eq. ( 1), hence we consider the following metric [24,55]…”
Section: IImentioning
confidence: 99%
“…Nevertheless, several researchers attracted to analyse this 4D EGB theory, in particular, the spherically symmetric black hole solution obtained by Glavan and Lin [17] was extended to include charge [20], a nonstatic Vaidya-like radiating black hole in Ref. [21,22], black holes coupled with NED [23][24][25], with cloud of string background [26]. The black hole stability and quasinormal modes are also widely discussed [27][28][29][30][31][32], and the rotating counter of the black holes obtained [33,34].…”
The EGB is an outcome of quadratic curvature corrections to the Einstein-Hilbert gravity action in the form of a Gauss-Bonnet (GB) term in D > 4 dimensions, and EGB gravity is topologically invariant in 4D. Several ways have been proposed for regularizing the D → 4 limit of EGB for non-trivial gravitational dynamics in 4D. Motivated by the importance of AdS/CFT, we obtain an exact static spherically symmetric nonsingular black hole in 4D EGB gravity coupled to the nonlinear electrodynamics (NED) in an AdS spacetime. We interpret the negative cosmological constant Λ as the positive pressure, via P = −Λ/8π, of the system's thermodynamic properties of the nonsingular black hole with an AdS background. We find that for P < Pc, the black holes with CP > 0 are stable to thermal fluctuations and unstable otherwise. We also analyzed the Gibbs free energy to find that the small globally unstable black holes undergo a phase transition to the large globally stable black holes. Further, we study the P − V criticality of the system and then calculate the critical exponents to find that our system behaves like Van der Walls fluid.
“…Here, A = 4πr 2 + is the black hole event horizon area, and A 0 is a constant with the area units. This equation generalizes the Hawking-Bekenstein area formula [79] by a supplementary logarithmic term and third in the above expression is due to magnetic charge g. Notice that, in limit α → 0, we obtain the entropy of the Hayward black hole [24]. Here, it is interesting to note that entropy of nonsingular-AdS EGB black holes does not depend explicitly on the pressure P of the system, but the horizon radius r + of the black hole depends on pressure P ; hence the pressure of the black hole affects its entropy.…”
Section: ∂T ∂Rsupporting
confidence: 55%
“…is the Lagrangian density of the NED, which for the nonsingular black hole solutions we are interested in, is given as [24,55]…”
Section: IImentioning
confidence: 99%
“…Here, we want to obtain the static spherically symmetric black hole solutions of Eq. ( 1), hence we consider the following metric [24,55]…”
Section: IImentioning
confidence: 99%
“…Nevertheless, several researchers attracted to analyse this 4D EGB theory, in particular, the spherically symmetric black hole solution obtained by Glavan and Lin [17] was extended to include charge [20], a nonstatic Vaidya-like radiating black hole in Ref. [21,22], black holes coupled with NED [23][24][25], with cloud of string background [26]. The black hole stability and quasinormal modes are also widely discussed [27][28][29][30][31][32], and the rotating counter of the black holes obtained [33,34].…”
The EGB is an outcome of quadratic curvature corrections to the Einstein-Hilbert gravity action in the form of a Gauss-Bonnet (GB) term in D > 4 dimensions, and EGB gravity is topologically invariant in 4D. Several ways have been proposed for regularizing the D → 4 limit of EGB for non-trivial gravitational dynamics in 4D. Motivated by the importance of AdS/CFT, we obtain an exact static spherically symmetric nonsingular black hole in 4D EGB gravity coupled to the nonlinear electrodynamics (NED) in an AdS spacetime. We interpret the negative cosmological constant Λ as the positive pressure, via P = −Λ/8π, of the system's thermodynamic properties of the nonsingular black hole with an AdS background. We find that for P < Pc, the black holes with CP > 0 are stable to thermal fluctuations and unstable otherwise. We also analyzed the Gibbs free energy to find that the small globally unstable black holes undergo a phase transition to the large globally stable black holes. Further, we study the P − V criticality of the system and then calculate the critical exponents to find that our system behaves like Van der Walls fluid.
“…Recently, the investigation on the shadows has been extended to regular black holes as well, including rotating Bardeen and Hayward black holes [23][24][25][26]. In history, regular black holes are proposed to resolve the singularity problem in classical general relativity.…”
We investigate the shadow cast by a sort of new regular black holes which are characterized by an asymptotically Minkowski core and the Sub-Planckian curvature. Firstly, we extend the metric with spherical symmetry to the one of rotating Kerr-like black holes and derive the null geodesics with circular orbit near the horizon of the black hole, and then plot the shadow of black holes with different values of the deviation parameter. It is found that the size of the shadow shrinks with the increase of the deviation parameter, while the shape of the shadow becomes more deformed. In particular, by comparing with the shadow of Bardeen black hole and Hayward black hole with the same values of parameters, we find that in general the shadow of black holes with Minkowski core has a larger deformation than that with de Sitter core, which potentially provides a strategy to distinguish these two sorts of regular black holes with different cores by astronomical observation in future.
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