## What is/are Hole Thermodynamics?

Hole Thermodynamics - We consider few such applications including dynamics of cosmological (anti)scalar background, non-variational deduction of the field equations, scalar and black-hole thermodynamics and the reshaping of the Einstein equations into the Klein-Gordon equation in thermodynamic Killing space.^{[1]}

## Black Hole Thermodynamics

It has been known that the Schwarzschild–de Sitter (Sch–dS) black hole may not be in thermal equilibrium and also be found to be thermodynamically unstable in the standard black hole thermodynamics.^{[1]}Moreover, we investigate the generalized second law of black hole thermodynamics (GSL) in Rényi statistics by considering the black hole as a working substance in heat engine.

^{[2]}From the free energy, we have done a systematic study of the 3D black hole thermodynamics and present, among our results, an indication of restoration of conformal symmetry for high temperatures.

^{[3]}Through the Smarr mass formula, it has been demonstrated that the first law of black hole thermodynamics remains valid for either of the new rainbow black hole solutions.

^{[4]}By introducing the general construction of Landau functional of the van der Waals system and charged AdS black hole system, we have preliminarily realized the Landau continuous phase transition theory in black hole thermodynamics.

^{[5]}Furthermore, we discuss the implications of our approach, regarding the the second and third laws of black hole thermodynamics.

^{[6]}We show that these results are compatible with the results obtained from classical black hole thermodynamics.

^{[7]}We obtain the modified first law of black hole thermodynamics in the presence of logarithmic corrections.

^{[8]}Causality and the generalized laws of black hole thermodynamics imply a bound, known as the Bekenstein-Hod universal bound, on the information emission rate of a perturbed system.

^{[9]}Moreover, the first law of black hole thermodynamics modified due to quantum corrections.

^{[10]}Keywords— Hawking radiation, Bardeen black hole, black hole thermodynamics, Hawking temperature.

^{[11]}The Smarr law, the first and the second law of black hole thermodynamics are discussed.

^{[12]}We utilize the general form of first law of black hole thermodynamics and compute different thermodynamic quantities.

^{[13]}In the extended phase space, by interpreting the cosmological constant as the thermodynamic pressure, we derive the thermodynamical quantities by the first law of black hole thermodynamics and obtain the equation of state.

^{[14]}Expressions for temperature, electric and magnetic potential were obtained and they satisfy the first law of the extended black hole thermodynamics, where a negative cosmological constant is associated with thermodynamic pressure.

^{[15]}This paper investigates whether the framework of fractional quantum mechanics can broaden our perspective of black hole thermodynamics.

^{[16]}Based in these experiments a modified Schwarzschild metric was obtained in order to calculate a quantum corrections in Schwarzschild black hole thermodynamics and tunneling probability.

^{[17]}We then extend our analysis to black hole thermodynamics.

^{[18]}Then, through calculation of the Smarr mass formula, we have shown that the first law of black hole thermodynamics remain valid for all of the new dilatonic black holes.

^{[19]}It has been known that in the presence of a scalar hair there would be a distinct additional contribution to the first law of black hole thermodynamics.

^{[20]}The black hole thermodynamics, entropy, shadow, energy emission rate, and quasinormal modes of black holes are investigated.

^{[21]}Not only is a classical black hole metric sought, but also agreement with the laws of black hole thermodynamics.

^{[22]}It turns out the first and second laws of black hole thermodynamics and the weak cosmic censorship conjecture are valid in high-dimensional hairy space-time.

^{[23]}Our results indicate that there may be a connection between the black hole thermodynamics and the boundary condition imposed on the black hole.

^{[24]}We analyze the generalized uncertainty principle (GUP) impact onto the nonextensive black hole thermodynamics by using R\'enyi entropy.

^{[25]}The first law of black hole thermodynamics is given and the Smarr relation is verified.

^{[26]}The first law of black hole thermodynamics in the presence of a cosmological constant Λ can be generalized by introducing a term containing the variation δΛ.

^{[27]}In presence of thermal fluctuations, we then derive various corrected thermodynamic potentials and also discuss the validity of first law of black hole thermodynamics for Bardeen black hole.

^{[28]}We explore a link between AdS black hole thermodynamics and the deflection angle variation.

^{[29]}Using concomitantly the Generalized Second Law of black hole thermodynamics and the holographic Bekenstein entropy bound embellished by Loop Quantum Gravity corrections to quantum black hole entropy, we show that the boundary cross sectional area of the postmerger remnant formed from the compact binary merger in gravitational wave detection experiments like GW150914, is bounded from below.

^{[30]}The current special issue was born out of the need to have a collection of original articles which provide novel investigations in the aforementioned topics, which not only highlight the important recent developments, but also open up new fields for future research in extended black hole thermodynamics.

^{[31]}Then, we study the Schwarzschild black hole thermodynamics by following NEUP.

^{[32]}Our results indicate that the first law of black hole thermodynamics might be valid for the Einstein-Maxwell theory with some quantum corrections in the effective region.

^{[33]}Based on the results of black hole thermodynamics, it is shown that this boundary may be lying at a level of the energy scales much lower than the Planck.

^{[34]}The results may offer new perspectives on the study of black hole thermodynamics.

^{[35]}In the extended phase space, it firstly shows that the first law of black hole thermodynamics is always true in our case.

^{[36]}Understanding the entanglement of radiation in quantum field theory has been a long-standing challenge, with implications ranging from black hole thermodynamics to quantum information.

^{[37]}Although the entropy of black holes in any diffeomorphism invariant theory of gravity can be expressed as the Wald entropy, the issue of whether the entropy always obeys the second law of black hole thermodynamics remains open.

^{[38]}According to the cosmic censorship conjecture, it is impossible for nature to have a physical singularity without a horizon because if it were to arise in any formalism, for instance as an extremal black hole (Kerr or Reissner-Nordstrom) then the surface gravity κ = 0, which is a strict violation of the third law of black hole thermodynamics.

^{[39]}Black hole thermodynamics suggests that, in order to describe the physics of distant observers, one may model a black hole as a standard quantum system with density of states set by the BekensteinHawking entropy SBH.

^{[40]}An implicit relation between the black hole carge $Q$ and other parameters is implied by combining the expression of the black hole mass with the first law of black hole thermodynamics.

^{[41]}The resulting thermodynamic variables are shown to satisfy the first law of black hole thermodynamics.

^{[42]}The grand canonical partition function that follows from the AdS3/CFT2 correspondence describes BPS and nearBPS black hole thermodynamics.

^{[43]}We discuss the Swampland Distance Conjecture in the framework of black hole thermodynamics.

^{[44]}This paper aims specifically at answering two contemporary requirements of a quantum theory of gravity, shown by using Loop Quantum Gravity (LQG) theory on the mathematics of black hole thermodynamics by (i) to quantise known classical General Relativistic formulations of black holes using LQG; and (ii) using LQG microstate spacelike sections (holonomies) on established quantum formulations of general relativity like Generalised Uncertainty Principle, to advocate for background independence in the mathematics of black hole horizon as the next step towards a viable quantum theory of gravity.

^{[45]}We show how these expressions suggest that conical defects emerging from a black hole can be considered as true hair – a new charge that the black hole can carry – and discuss the impact of conical deficits on black hole thermodynamics from this ‘chemical’ perspective.

^{[46]}So exploring the Van der Waals transition is potentially valuable for studying holographic properties of charged black hole thermodynamics.

^{[47]}The thermodynamical quantities like Hawking temperature, entropy and specific heat capacity at constant charge are found and we show that the resulting quantities satisfy the first law of black hole thermodynamics.

^{[48]}Within our approximation, our construction allows us to write down a completely local version of the second law of black hole thermodynamics, in the presence of the higher derivative corrections considered here.

^{[49]}From the near-horizon analysis, its microscopic entropy, according to the Kerr/CFT correspondence, is found and the second law of black hole thermodynamics is discussed.

^{[50]}

## hole thermodynamics remain

Through the Smarr mass formula, it has been demonstrated that the first law of black hole thermodynamics remains valid for either of the new rainbow black hole solutions.^{[1]}Then, through calculation of the Smarr mass formula, we have shown that the first law of black hole thermodynamics remain valid for all of the new dilatonic black holes.

^{[2]}Although the entropy of black holes in any diffeomorphism invariant theory of gravity can be expressed as the Wald entropy, the issue of whether the entropy always obeys the second law of black hole thermodynamics remains open.

^{[3]}