scholarly journals Phase transition and thermodynamic geometry off(R)AdS black holes in the grand canonical ensemble

2016 ◽  
Vol 93 (12) ◽  
Author(s):  
Gu-Qiang Li ◽  
Jie-Xiong Mo
Keyword(s):  
Phase Transition ◽  
Black Holes ◽  
Canonical Ensemble ◽  
Grand Canonical Ensemble ◽  
Ads Black Holes ◽  
Thermodynamic Geometry ◽  
Grand Canonical

scholarly journals Critical behaviors and phase transitions of black holes in higher order gravities and extended phase spaces

2017 ◽  
Vol 26 (03) ◽  
pp. 1750017 ◽  
Author(s):  
Zeinab Sherkatghanad ◽  
Behrouz Mirza ◽  
Zahra Mirzaiyan ◽  
Seyed Ali Hosseini Mansoori
Keyword(s):  
Black Holes ◽  
Phase Transitions ◽  
Canonical Ensemble ◽  
Grand Canonical Ensemble ◽  
Lovelock Gravity ◽  
Third Order ◽  
Extended Phase ◽  
The Third ◽  
Ads Black Holes ◽  
Grand Canonical

We consider the critical behaviors and phase transitions of Gauss–Bonnet–Born–Infeld-AdS black holes (GB–BI-AdS) for [Formula: see text] and the extended phase space. We assume the cosmological constant, [Formula: see text], the coupling coefficient [Formula: see text], and the BI parameter [Formula: see text] to be thermodynamic pressures of the system. Having made these assumptions, the critical behaviors are then studied in the two canonical and grand canonical ensembles. We find “reentrant and triple point phase transitions” (RPT-TP) and “multiple reentrant phase transitions” (multiple RPT) with increasing pressure of the system for specific values of the coupling coefficient [Formula: see text] in the canonical ensemble. Also, we observe a reentrant phase transition (RPT) of GB–BI-AdS black holes in the grand canonical ensemble and for [Formula: see text]. These calculations are then expanded to the critical behavior of Born–Infeld-AdS (BI-AdS) black holes in the third-order of Lovelock gravity and in the grand canonical ensemble to find a van der Waals (vdW) behavior for [Formula: see text] and a RPT for [Formula: see text] for specific values of potential [Formula: see text] in the grand canonical ensemble. Furthermore, we obtain a similar behavior for the limit of [Formula: see text], i.e. charged-AdS black holes in the third-order of the Lovelock gravity. Thus, it is shown that the critical behaviors of these black holes are independent of the parameter [Formula: see text] in the grand canonical ensemble.

Extended phase space and thermodynamic geometry of topological Born–Infeld-dilaton black holes

2016 ◽  
Vol 25 (06) ◽  
pp. 1650062 ◽  
Author(s):  
A. Sheykhi ◽  
S. Hajkhalili
Keyword(s):  
Phase Transition ◽  
Black Holes ◽  
Canonical Ensemble ◽  
Nonlinear Electrodynamics ◽  
Dilaton Field ◽  
Extended Phase ◽  
Thermodynamic Geometry ◽  
Transition Points ◽  
The Stability ◽  
Grand Canonical

We consider an [Formula: see text]-dimensional topological black holes of Einstein-dilaton gravity in the presence of Born–Infeld nonlinear electrodynamics. We investigate the thermal stability in the grand canonical ensemble and show that depending on the values of the parameters, these types of black holes can experience an instable phase and with changing of the metric parameters, the stability can be influenced. Also, we study the phase transition of these black holes via thermodynamic geometry approach and show that two types of phase transition can be occurred. Finally, we extend thermodynamical space by considering dilaton field as an extensive thermodynamic parameter and check the phase transition points.

scholarly journals Thermal stability of black holes with arbitrary hairs

2018 ◽  
Vol 33 (05) ◽  
pp. 1850031 ◽  
Author(s):  
Aloke Kumar Sinha
Keyword(s):  
Thermal Stability ◽  
Black Holes ◽  
Loop Quantum Gravity ◽  
Canonical Ensemble ◽  
Grand Canonical Ensemble ◽  
Stability Criteria ◽  
Spacetime Geometry ◽  
Rotating Black Holes ◽  
Grand Canonical ◽  
Thermal Stability Of

We have derived the criteria for thermal stability of charged rotating black holes, for horizon areas that are large relative to the Planck area (in these dimensions). In this paper, we generalized it for black holes with arbitrary hairs. The derivation uses results of loop quantum gravity and equilibrium statistical mechanics of the grand canonical ensemble and there is no explicit use of classical spacetime geometry at all in this analysis. The assumption is that the mass of the black hole is a function of its horizon area and all the hairs. Our stability criteria are then tested in detail against some specific black holes, whose metrics provide us with explicit relations for the dependence of the mass on the area and other hairs of the black holes. This enables us to predict which of these black holes are expected to be thermally unstable under Hawking radiation.

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