Products of thermodynamic parameters of the generalized charged rotating black hole and the Reissner–Nordström black hole with a global monopole (original) (raw)
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2016
We investigate the thermodynamics of Kerr-Newman-Kasuya black hole and the Reissner-Nordstrom black hole with a global monopole on inner and outer horizons. Products of surface gravities, surface temperatures, Komar energies, electromagnetic potentials, angular velocities, areas, entropies, horizon radii and the irreducible masses at the Cauchy and the event horizons are calculated. It is observed that the product of surface gravities, surface temperature product and product of Komar energies, electromagnetic potentials and angular velocities at horizons are not universal quantities for these black holes. Products of areas and entropies at horizons are independent of masses of black holes. Heat capacity is calculated for the generalized charged rotating black hole and phase transition is observed, under certain conditions on r. ?E
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Journal of Physics: Conference Series
In this paper we calculate the Hawking temperature of a black hole described by the Kerr-Newman metric, starting from the surface gravity, the area of the event horizon and the angular velocity of the black hole. To do this we apply the laws of black hole thermodynamics: we first set the energy conservation through a relationship between the mass M, the charge Q and the angular momentum J, then we implement the Hawking's theorem of areas by setting an upper bound to the energy and we get finally the surface gravity of the black hole. In addition, we study the relationship between the black hole parameters (mass M, angular momentum J, electric charge Q) and the Hawking temperature.
Thermodynamic analysis of Kerr-Newman black holes Thermodynamic analysis of Kerr-Newman black holes
Journal of Physics: Conference Series, 2019
In this paper we calculate the Hawking temperature of a black hole described by the Kerr-Newman metric, starting from the surface gravity, the area of the event horizon and the angular velocity of the black hole. To do this we apply the laws of black hole thermodynamics: we first set the energy conservation through a relationship between the mass M, the charge Q and the angular momentum J, then we implement the Hawking's theorem of areas by setting an upper bound to the energy and we get finally the surface gravity of the black hole. In addition, we study the relationship between the black hole parameters (mass M, angular momentum J, electric charge Q) and the Hawking temperature. 1. Introduction In 1974 Hawking [1,2] predicted that the curvature of space-time at the event horizon of a black hole is sufficient to excite photons from vacuum and cause a continuous flow of them, known as Hawking radiation. The continuous process causes the black hole to lose energy with the consequent decrease of its mass, until after a while and the hole disappears completely. Hawking predicted that this radiation has a well-defined temperature proportional to the superficial gravity in its horizon of events. In 2009 V. Pankovic [3], presents a simplified method for describing and calculating the basic characteristics, dynamics (horizons) and thermodynamics of a Kerr-Newman black hole. His method was based on principles of classical mechanics, electrodynamics, thermodynamics, statistics, non-relativistic quantum mechanics and on the elementary form of the general principle of relativistic equivalence; which represented results already proposed in the theory of quantum gravity. In 2010 F. Belgiorno and his colleagues [4], created an optical analogue of the event horizon of a black hole, the results of which coincide with Stephen Hawking's quantum predictions for radiation emitted by a black hole evaporating. If the result of Franco Belgiorno and his colleagues is confirmed, it would be the first observation of Hawking radiation. This paper presents a simplified method for estimating Hawking temperature and evaporation time of Kerr-Newman black holes. The relationship between the hole parameters (mass M, angular momentum J, electric charge Q) and this time is also studied.
Thermodynamics of accelerating and rotating black holes
Astrophysics and Space Science, 2013
Thermodynamics of a large family of black holes from electrovacuum solutions of Einstein's equations is studied. This family includes rotating and nonaccelerating black holes with NUT charge, and rotating and accelerating black holes. The surface gravity, Hawking temperature and the area laws for these black holes are presented. The first law of thermodynamics is also given. An interesting outcome of our analysis is the restriction obtained on the magnitude of acceleration for these black holes.
Thermodynamics of charged, rotating, and accelerating black holes
Journal of High Energy Physics
We show how to obtain a consistent thermodynamic description of accelerating asymptotically AdS black holes, extending our previous results by including charge and rotation. We find that the key ingredient of consistent thermodynamics is to ensure that the system is not over-constrained by including the possibility of varying the ‘string’ tensions that are responsible for the acceleration of the black hole, yielding a first law of full cohomogeneity. The first law assumes the standard form, with the entropy given by one quarter of the horizon area and other quantities identified by standard methods. In particular we compute the mass in two independent ways: through a Euclidean action calculation and by the method of conformal completion. The ambiguity in the choice of the normalization of the timelike Killing vector can be fixed by explicit coordinate transformation (in the case of rotation) to the standard AdS form or by holographic methods (in the case of charge). This resolves a ...
Thermodynamics of Extended Gravity Black Holes
Thermodynamics of extended gravity static spherically symmetric black hole solutions is investigated. The energy issue is discussed making use of the derivation of Clausius relation from equations of motion, evaluating the black hole entropy by the Wald method and computing the related Hawking temperature.
Geometro-thermodynamics of tidal charged black holes
European Physical Journal C, 2011
Tidal charged spherically symmetric vacuum brane black holes are characterized by their mass m and tidal charge q, an imprint of the five-dimensional Weyl curvature. For q>0 they are formally identical to the Reissner–Nordström black hole of general relativity. We study the thermodynamics and thermodynamic geometries of tidal charged black holes and discuss similarities and differences as compared to the Reissner–Nordströ m black hole. As a similarity, we show that (for q>0) the heat capacity of the tidal charged black hole diverges on a set of measure zero of the parameter space, nevertheless both the regularity of the Ruppeiner metric and a Poincaré stability analysis show no phase transition at those points. The thermodynamic state spaces being different indicates that the underlying statistical models could be different. We find that the q
Thermodynamic Product Relations for Generalized Regular Black Hole
Advances in High Energy Physics, 2016
We derive thermodynamic product relations for four-parametric regular black hole (BH) solutions of the Einstein equations coupled with a nonlinear electrodynamics source. The four parameters can be described by the mass (m), charge (q), dipole moment (α), and quadrupole moment (β), respectively. We study its complete thermodynamics. We compute different thermodynamic products, that is, area product, BH temperature product, specific heat product, and Komar energy product, respectively. Furthermore, we show some complicated function of horizon areas that is indeedmass-independentand could turn out to beuniversal.
Thermodynamic Analysis of Non-Linear Reissner-Nordström Black Holes
Universe, 2015
In the present article we study the Inverse Electrodynamics Model. This model is a gauge and parity invariant non-linear Electrodynamics theory, which respects the conformal invariance of standard Electrodynamics. This modified Electrodynamics model, when minimally coupled to General Relativity, is compatible with static and spherically symmetric Reissner-Nordström-like black-hole solutions. However, these black-hole solutions present more complex thermodynamic properties than their Reissner-Nordström black-hole solutions counterparts in standard Electrodynamics. In particular, in the Inverse Model a new stability region, with both the heat capacity and the free energy negative, arises. Moreover, unlike the scenario in standard Electrodynamics, a sole transition phase is possible for a suitable choice in the set of parameters of these solutions.
2018
F. B. Lustosa1,∗ M. E. X. Guimarães1,† Cristine N. Ferreira2,‡ and J. L. Neto3§ 1. Instituto de F́ısica, Universidade Federal Fluminense, Av. Gal. Milton Tavares de Souza, s/n Campus da Praia Vermelha 24210-346 Niterói, RJ, Brazil 2. Núcleo de Estudos em F́ısica, Instituto Federal de Educação, Ciência e Tecnologia Fluminense, Rua Dr. Siqueira 273, Campos dos Goytacazes, 28030-130 RJ, Brazil and 3. Instituto de F́ısica, Universidade Federal do Rio de Janeiro, Caixa Postal 68528 Rio de Janeiro 21941-972, RJ, Brazil