Charged black holes in quartic quasi-topological gravity

Ghanaatian, M.; Naeimipour, F.; Bazrafshan, A.; Abkar, M.

doi:10.1103/physrevd.97.104054

Cited by 11 publications

(14 citation statements)

References 56 publications

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“…Also, by writing metric (8) in the form of the reference background metric, the ADM (Arnowitt-Deser-Misner) energy of the black hole per unit volume V n−1 is obtained at the limit r → ∞ as [32]…”

Section: Thermodynamics Of the Solutionsmentioning

confidence: 99%

“…After obtaining the conserved and thermodynamic quantities, we want to check out the first law of thermodynamics for the solutions. By using the equations (27), (32), (33) and (25), we first obtain m-smarr formula as…”

Section: Thermodynamics Of the Solutionsmentioning

confidence: 99%

“…There is also a review of quartic quasi-topological black holes in the presence of the nonlinear electromagnetic Born-Infeld field in [30]. Also, quasi-topological gravity has been investigated in Lifshitz spacetime for general value z in [31] and for z = 1 in [32]. Now, we are eager to construct lifshitz black hole solutions with the third order quasi-topological gravity in the presence of a power-law Maxwell field.…”

Section: Introductionmentioning

confidence: 99%

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Third order quasitopological black hole with a power-law Maxwell nonlinear source

et al. 2019

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In this paper, we construct a new class of solutions for five dimensional third order quasitopological black holes coupled to a power-law Maxwell nonlinear electrodynamics. To have real solutions, we should establish condition µ < − λ 2 3 and to have finite solutions at infinity, the parameter of power-law Maxwell theory "s" should obey 1 2 < s ≤ 2. Power-law Maxwell lagrangian is successful to set conformal invariance in higher dimensions. Also, this theory can reduce the divergence of the electrical field at the origin that is caused in linear Maxwell theory. As the value of parameter "s" increases, this divergence reduces more. In asymptotically anti-de sitter spacetimes, these obtained solutions lead to a black hole with two horizons for small values of s and q. Also, solutions for s = 2 have different behaviors with respect to the ones for other values of s. For negative and small values of parameter µ, these solutions can describe a black hole with two horizons. An other important tip is that this black hole has thermal stability just for anti-de sitter solutions if its temperature is positive.

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Section: Thermodynamics Of the Solutionsmentioning

confidence: 99%

Section: Thermodynamics Of the Solutionsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Third order quasitopological black hole with a power-law Maxwell nonlinear source

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“…which are the electromagnetic fields of linear Maxwell theory [19] plus some leading order nonlinear correction terms. To find the gauge potential A t , we should solve the equation F tr + ∂ r A t = 0 that leads to…”

Section: Quartic Quasitopological Black Hole Solutionsmentioning

confidence: 99%

Physical and thermodynamic properties of quartic quasitopological black holes and rotating black branes with a nonlinear source

et al. 2019

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In this paper, we find the solutions of quartic quasitopological black holes and branes coupled to logarithmic and exponential forms of nonlinear electrodynamics. These solutions have an essential singularity at r = 0. Depending on the value of charge parameter q, we have an extreme black hole/brane, a black hole/brane with two horizons or a naked singularity. For small values of parameter q, the solutions lead to a black hole/brane with two horizons. The values of the horizons are independent of the values of quasitopological parameters and depend only on the values of q, dimensions n, nonlinear parameter β and mass parameter. Also, the solutions are not thermally stable for dS and flat spacetimes. However, AdS solutions are stable for r+ > r+ ext which the temperature is zero for r+ = r+ ext . The value of r+ ext also depends on the values of parameters q, β, n and m. As the value of r+ ext decreases, the region of stability becomes larger. We also use HPEM metric to probe GTD formalism for our solutions. This metric is successful to predict the divergences of the scalar curvature exactly at the phase transition points. For large values of parameter Ξ, the black hole/brane has a transition to a stable state and stays stable.

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“…respectively where we have used the substitution f (r) = N 2 (r)g(r). Equation (12) shows that the function N (r) should be a constant, and so we choose N (r) = 1 which yields to f (r) = g(r). Using N = 1 in (13), we reach to the equationμ…”

Section: Construction Of (N + 1)-dimensional Quintic Quasitopologmentioning

confidence: 99%

Thermodynamics of static solutions in ( n+1 )-dimensional quintic quasitopological gravity

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Based on the fact that some important theories like string and M-theories predict spacetime with higher dimensions, so, in this paper, we aim to construct a theory of quintic quasitopological gravity in higher dimensions (n ≥ 5). This (n + 1)-dimensional quintic quasitopological gravity can also lead to the most second-order linearized field equations in the spherically symmetric spacetimes. These equations can not be solved exactly and so, we obtain a new class of (n + 1)-dimensional static solutions with numeric methods. For large values of mass parameter m, these solutions yield to black holes with two horizons in AdS and flat spacetimes. For dS solutions, there are two values, mext and mcri, which yield to a black hole with three horizons for mext < m < mcri. We also calculate thermodynamic quantities for this black hole such as entropy and temperature and check the first law of thermodynamics. Finally, we analyze thermal stability of the (n + 1)-dimensional static black hole at the horizon r+. Unlike dS solutions, AdS ones have thermal stability for each values of k, but flat solutions are stable with just k = 1.

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Charged black holes in quartic quasi-topological gravity

Cited by 11 publications

References 56 publications

Third order quasitopological black hole with a power-law Maxwell nonlinear source

Third order quasitopological black hole with a power-law Maxwell nonlinear source

Physical and thermodynamic properties of quartic quasitopological black holes and rotating black branes with a nonlinear source

Thermodynamics of static solutions in ( n+1 )-dimensional quintic quasitopological gravity

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