A possible thermodynamic origin of the spacetime minimum length

2020 ◽  
Vol 29 (14) ◽  
pp. 2043022
Author(s):  
Ting-Ping Liu ◽  
Jin Pu ◽  
Yan Han ◽  
Qing-Quan Jiang
Keyword(s):  
Black Hole ◽  
Quantum Gravity ◽  
Generalized Uncertainty Principle ◽  
Black Hole Thermodynamics ◽  
Minimum Length ◽  
Black Hole Evaporation ◽  
The Third ◽  
Third Law Of Thermodynamics ◽  
Third Law ◽  
Classical Gravity

In this paper, by applying the generalized uncertainty principle (GUP) at the final stage of black hole evaporation, we have proposed a thermodynamic explanation for the minimal scale of quantum gravity, i.e. it may stem from the basic requirements of the third law of thermodynamics for quantum gravitation system. At the same time, we have interestingly found that the third law of black hole thermodynamics acts as a supervisor in quantum gravity spacetime to ensure the causality of the spacetime as that does in classical gravity.

scholarly journals BLACK HOLES AND THE THIRD LAW OF THERMODYNAMICS

2004 ◽  
Vol 13 (04) ◽  
pp. 739-770 ◽  
Author(s):  
F. BELGIORNO ◽  
M. MARTELLINI
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Second Law Of Thermodynamics ◽  
Temperature Limit ◽  
Black Hole Thermodynamics ◽  
Zero Temperature ◽  
The Third ◽  
Third Law Of Thermodynamics ◽  
Third Law ◽  
Extremal Black Holes

We discuss in the framework of black hole thermodynamics some aspects relative to the third law in the case of black holes of the Kerr–Newman family. In the light of the standard proof of the equivalence between the unattainability of the zero temperature and the entropic version of the third law it is remarked that the unattainability has a special character in black hole thermodynamics. Also the zero temperature limit which obtained in the case of very massive black holes is discussed and it is shown that a violation of the entropic version in the charged case occurs. The violation of the Bekenstein–Hawking law in favour of zero entropy SE=0 in the case of extremal black holes is suggested as a natural solution for a possible violation of the second law of thermodynamics. Thermostatic arguments in support of the unattainability are explored, and SE=0 for extremal black holes is shown to be again a viable solution. The third law of black hole dynamics by W. Israel is then interpreted as a further strong corroboration to the picture of a discontinuity between extremal states and non-extremal ones.

scholarly journals Remarks on Remnants by Fermions’ Tunnelling from Black Strings

2014 ◽  
Vol 2014 ◽  
pp. 1-9 ◽  
Author(s):  
Deyou Chen ◽  
Zhonghua Li
Keyword(s):  
Black Hole ◽  
Quantum Gravity ◽  
Uncertainty Principle ◽  
Final Stage ◽  
Generalized Uncertainty Principle ◽  
Black Hole Evaporation ◽  
Quantum Numbers ◽  
Black Strings

Hawking’s calculation is unable to predict the final stage of the black hole evaporation. When effects of quantum gravity are taken into account, there is a minimal observable length. In this paper, we investigate fermions’ tunnelling from the charged and rotating black strings. With the influence of the generalized uncertainty principle, the Hawking temperatures are not only determined by the rings, but also affected by the quantum numbers of the emitted fermions. Quantum gravity corrections slow down the increases of the temperatures, which naturally leads to remnants left in the evaporation.

scholarly journals Can Naked Singularities Exist Without Violating The Laws of Black Hole Thermodynamics?

2021 ◽  
Vol 19 ◽  
pp. 204-207
Author(s):  
Amal Pushp
Keyword(s):  
Black Hole ◽  
Cosmic Censorship ◽  
Black Hole Thermodynamics ◽  
Surface Gravity ◽  
Extremal Black Hole ◽  
Naked Singularities ◽  
The Third ◽  
Physical Singularity ◽  
Third Law ◽  
Cosmic Censorship Conjecture

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. In this paper we explore whether a true singularity can exist without defying this law.

scholarly journals String analog of Reissner–Nordström black holes cannot be overcharged

2019 ◽  
Vol 34 (30) ◽  
pp. 1950248 ◽  
Author(s):  
Koray Düztaş ◽  
Mubasher Jamil
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
String Theory ◽  
Black Hole Thermodynamics ◽  
Drop Out ◽  
Charged Black Holes ◽  
The Third ◽  
Test Particles ◽  
Third Law ◽  
Extremal Black Holes

In this work, we attempt to overcharge extremal and nearly extremal charged black holes in string theory, known as the Garfinkle–Horowitz–Strominger solution. We first show that extremal black holes cannot be overcharged analogous to the case of Reissner–Nordström (RN) black holes. Contrary to their analog in general relativity, nearly extremal black holes can neither be overcharged beyond extremality, nor can they be driven to extremality by the interaction with test particles. Therefore, the analysis in this work also implies that the third law of black hole thermodynamics holds for the relevant charged black holes in string theory perturbed by test particles. This can be interpreted as a stronger version of the third law since one can drop out the continuity proviso for the relevant process.

scholarly journals Minimal length and the flow of entropy from black holes

2018 ◽  
Vol 27 (14) ◽  
pp. 1847028 ◽  
Author(s):  
Ana Alonso-Serrano ◽  
Mariusz P. Da̧browski ◽  
Hussain Gohar
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Quantum Gravity ◽  
Uncertainty Principle ◽  
Hawking Radiation ◽  
Generalized Uncertainty Principle ◽  
Minimal Length ◽  
Evaporation Process ◽  
Black Hole Evaporation ◽  
The Impact

The existence of a minimal length, predicted by different theories of quantum gravity, can be phenomenologically described in terms of a generalized uncertainty principle. We consider the impact of this quantum gravity motivated effect onto the information budget of a black hole and the sparsity of Hawking radiation during the black hole evaporation process. We show that the information is not transmitted at the same rate during the final stages of the evaporation, and that the Hawking radiation is not sparse anymore when the black hole approaches the Planck mass.

scholarly journals EXTREMAL BLACK HOLES AND THE LIMITS OF THE THIRD LAW

2001 ◽  
Vol 10 (01) ◽  
pp. 33-39 ◽  
Author(s):  
STEFANO LIBERATI ◽  
TONY ROTHMAN ◽  
SEBASTIANO SONEGO
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Black Hole Thermodynamics ◽  
Quantum Field ◽  
Semiclassical Theory ◽  
Zero Temperature ◽  
The Third ◽  
The Status ◽  
Third Law ◽  
Extremal Black Holes

Recent results of quantum field theory on a curved spacetime suggest that extremal black holes are not thermal objects and that the notion of zero temperature is ill-defined for them. If this is correct, one may have to go to a full semiclassical theory of gravity, including backreaction, in order to make sense of the third law of black hole thermodynamics. Alternatively it is possible that we shall have to drastically revise the status of extremality in black hole thermodynamics.

scholarly journals Black Hole Evaporation: A Perspective from Loop Quantum Gravity

Universe ◽  
2020 ◽  
Vol 6 (2) ◽  
pp. 21 ◽  
Author(s):  
Abhay Ashtekar
Keyword(s):  
General Relativity ◽  
Black Hole ◽  
Quantum Gravity ◽  
Event Horizon ◽  
Loop Quantum Gravity ◽  
Personal Perspective ◽  
Black Hole Evaporation ◽  
Classical Quantum ◽  
Classical Gravity ◽  
The One

A personal perspective on the black hole evaporation process is presented using, as guidelines, inputs from: (i) loop quantum gravity, (ii) simplified models where concrete results have been obtained, and, (iii) semi-classical quantum general relativity. On the one hand, the final picture is conservative in that there are concrete results that support each stage of the argument, and there are no large departures from general relativity or semi-classical gravity in tame regions outside macroscopic black holes. On the other hand, it argues against certain views that are commonly held in many quarters, such as persistence of a piece of singularity that constitutes a part of the final boundary of space–time; presence of an event horizon serving as an absolute barrier between the interior and the exterior, and the (often implicit) requirement that purification must be completed by the time the ‘last rays’ representing the extension of this event horizon reach I + .

scholarly journals A new touch temperature of the event horizon and Rindler horizon in the Kinnersley spacetime

2022 ◽  
Vol 82 (1) ◽  
Author(s):  
Jie Zhang ◽  
Menquan Liu ◽  
Zhie Liu ◽  
Shuzheng Yang
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Dispersion Relation ◽  
Event Horizon ◽  
Dynamical Equation ◽  
Radiation Temperature ◽  
The Third ◽  
Touch Point ◽  
Third Law Of Thermodynamics ◽  
Third Law

AbstractThe Kinnersley spacetime not only describes a non-spherical symmetric, non-stationary and accelerating black hole, but also can be used to explore the characteristics of collision of two black holes because it has two horizons: the Rindler horizon and the event horizon. Previous research shows Rindler horizon and the event horizon cannot touch due to violation of the third law of thermodynamics. By solving a fermion dynamical equation including the Lorentz dispersion relation, we obtain a modified radiation temperature at the event horizon of the black hole, as well as the colliding temperature at the touch point of Rindler horizon and the event horizon. We find the temperature at the touch point is not equal to zero if $${\dot{r}}_H\ne 0$$ r ˙ H ≠ 0 . This result indicates that the event horizon and Rindler horizon can collide without violation of the third law of thermodynamics when Lorentz dispersion relation is considered.

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