2015/10/31 by N. Farhangkhah · 1 citation
Physics and Astronomy · #Black Holes and Theoretical Physics #Black hole (networking) #Charge (physics) #Classical mechanics #Constant curvature #Cosmological constant #Cosmology and Gravitation Theories #Curvature #Electric charge #Event horizon #Geometry #Horizon #Mathematical physics #Naked singularity #Noncommutative and Quantum Gravity Theories #Physics #Quantum mechanics #Scalar curvature #Spacetime #gr-qc
paper · pdf · doi:10.1142/s0218271816500309
published as Int. J. Mod. Phys. Vol. 25, No. 2 (2016) 1650030 · 17 pages, 6 figures
arxiv created 2016/01/08 · openalex publication_date 2016/01/21 · arxiv updated 2018/04/12 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We find a class of charged black hole solutions in third-order Lovelock Gravity. To obtain this class of solutions, we are not confined to the usual assumption of maximal symmetry on the horizon and will consider the solution whose boundary is Einstein space with supplementary conditions on its Weyl tensor. The Weyl tensor of such exotic horizons exposes two chargelike parameter to the solution. These parameters in addition with the electric charge, cause different features in comparison with the charged solution with constant-curvature horizon. For this class of asymptotically (A)dS solutions, the electric charge dominates the behavior of the metric as [Formula: see text] goes to zero, and thus the central singularity is always timelike. We also compute the thermodynamic quantities for these solutions and will show that the first law of thermodynamics is satisfied. We also show that the extreme black holes with nonconstant-curvature horizons whose Ricci scalar are zero or a positive constant could exist depending on the value of the electric charge and chargelike parameters. Finally, we investigate the stability of the black holes by analyzing the behavior of free energy and heat capacity specially in the limits of small and large horizon radius. We will show that in contrast with charged solution with constant-curvature horizon, a phase transition occurs between very small and small black holes from a stable phase to an unstable one, while the large black holes show stability to both perturbative and nonperturbative fluctuations.