Bekenstein bound from the Pauli principle

Acquaviva, Giovanni; Iorio, Alfredo; Smaldone, L. A.

doi:10.1103/physrevd.102.106002

Cited by 25 publications

(32 citation statements)

References 59 publications

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“…Like any quantum structure there are the observables of the theory which are the average quantities. There are approaches that focus more on quantum operators [22] and there are those that are concerned with observables that have more relevant experimental implications. In that article this last line is followed and for that reason effects such as the Stefan-Boltzmann and Casimir law are investigated.…”

Section: Introductionmentioning

confidence: 99%

On the temperature of gravitation in the de Sitter space-time

et al. 2021

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The temperature associated with gravitation as presented in the Unruh effect and Hawking temperature serves to link different areas of physics, such as gravity, statistical mechanics, and quantum physics. In this paper, teleparallel gravity is considered to study temperature effects on the de Sitter space-time. The effects of temperature are introduced using the thermo field dynamics formalism. The gravitational Stefan-Boltzmann law is obtained. Then the temperature of gravitation in the de Sitter space-time is calculated. Here an Unruh-type effect is discussed. This effect relates the temperature and the acceleration of a particle in the de Sitter space-time. The gravitational Casimir effect is calculated. The result shows that there is a transition between an attractive and a repulsive Casimir effect.

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Section: Introductionmentioning

confidence: 99%

On the temperature of gravitation in the de Sitter space-time

et al. 2021

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“…In fact, reviving in a quantum gravity context the original spirit of the Leningrad school, our results suggest that quantum groups might lend their powerful and well-developed calculus as the natural calculus of PQM in particular, and of quantum gravity in general. For instance, besides the expected impact on LQG, our results might be useful for quantum gravity theories based on discrete fundamental structures [44,51,52] such as those based on finite-dimensional Hilbert spaces, see, e.g., [53,54].…”

Section: Discussionmentioning

confidence: 88%

Quantum Groups and Polymer Quantum Mechanics

Acquaviva,

Iorio,

Smaldone

2021

Preprint

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“…On the other hand, for AdS BHs, R TG always points to attractive interaction. Although, in other systems, changes of sign of R TG have been seen [23][24][25] near the critical point (and, although recent general results, on the fundamental quantum gravitational interaction, indicate a fermionic nature of such degrees of freedom [72]), we take here the view that the physical region for Schwarzschild BHs in conformal gravity requires an entropy greater than the S 0 in Eq. (69), in order to have a consistent interpretation with the attractive nature of the gravitational interaction.…”

Section: Stability Analysis: Specific Heat and Tgmentioning

confidence: 94%

Stability of Schwarzschild (Anti)de Sitter black holes in conformal gravity

et al. 2021

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We study the thermodynamics of spherically symmetric, neutral and non-rotating black holes in conformal (Weyl) gravity. To this end, we apply different methods: (i) the evaluation of the specific heat; (ii) the study of the entropy concavity; (iii) the geometrical approach to thermodynamics known as thermodynamic geometry; (iv) the Poincaré method that relates equilibrium and out-of-equilibrium thermodynamics. We show that the thermodynamic geometry approach can be applied to conformal gravity too, because all the key thermodynamic variables are insensitive to Weyl scaling. The first two methods, (i) and (ii), indicate that the entropy of a de Sitter black hole is always in the interval $$2/3\le S\le 1$$ 2 / 3 ≤ S ≤ 1 , whereas thermodynamic geometry suggests that, at $$S=1$$ S = 1 , there is a second order phase transition to an Anti de Sitter black hole. On the other hand, we obtain from the Poincaré method (iv) that black holes whose entropy is $$S < 4/3$$ S < 4 / 3 are stable or in a saddle-point, whereas when $$S>4/3$$ S > 4 / 3 they are always unstable, hence there is no definite answer on whether such transition occurs. Since thermodynamics geometry takes the view that the entropy is an extensive quantity, while the Poincaré method does not require extensiveness, it is valuable to present here the analysis based on both approaches, and so we do.

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Bekenstein bound from the Pauli principle

Cited by 25 publications

References 59 publications

On the temperature of gravitation in the de Sitter space-time

On the temperature of gravitation in the de Sitter space-time

Quantum Groups and Polymer Quantum Mechanics

Stability of Schwarzschild (Anti)de Sitter black holes in conformal gravity

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