Submitted:
01 November 2023
Posted:
01 November 2023
You are already at the latest version
Abstract

Keywords:
1. Introduction

2. The Metaplectic group and the principle of minimal representation
Mp(2), SU(1,1) and Sp(2)
3. The Mp(2) vector representation and its coverings
4. Symmetry and Dynamics Principle: Steps to follow
4.1. The invariant action
4.2. Extended Hamiltonian of the system
4.3. Relativistic wave equation and the algebraic interpretation
4.4. Basic states of representation and the spectrum of physical states
5. Statement of the problem
6. Physical states from Symmetries
7. Supermetric and emergent spacetime
8. Superspace and discrete spacetime structure
Statistical distributions and classical limit
9. The Lowest n = 0 Level and its Length
10. Implications for the Black hole entropy: A superspace solution
11. Implications for Hawking Radiation
- Due to the interplay between the area of the black hole surface and the black hole mass, it is quantized as well. The mass of the black hole decreases when radiation is emitted due the quantum jump from one quantized value of the mass (energy) to a lower quantized value.
- As a consequence, (because radiation is emitted at quantized frequencies corresponding to the differences between energy levels), quantum gravity implies a discretized emission spectrum for the black hole radiation.
- The spectral lines can be very dense in macroscopic regimes leading physically no contradiction with Hawking’s prediction of a continuous thermal spectrum in the semiclassical regime.
- From the point of view of our approach here:
- If we now suppose simply that the constants A, B in the state solution eg. Eq. (27), Eq. (35), are different, we have :
- Then, we cannot reach the thermal (Hawking) spectrum at the macroscopic level.
-
This fact is clear because we need exact balance between the superposition of the two irreducible representations of the Metaplectic group.This will lead as a result, non classical states of radiation in the sense of [21] as can be easily seen putting, for example, the constants B equal to zero:
- Notice that only the up spinor part survives and the classical (thermal) limit is not reached, even in the continuous limit where the number of levels increases accordingly to
- In such a case where , (or ), the spectrum will takes only even (or odd) levels becoming evidently non thermal.
- if the thermal Hawking spectrum is reached at the continuum classical gravity level eg, the Poissonian behaviour of the distribution is complete.
- Otherwise, with , the spectrum belongs to a non classical one and the quantum properties of gravity are macroscopically manifest.
12. Concluding remarks
References
- N. G. Sanchez, G & C, Gravitation and Cosmology 25, 91 (2019), Springer Nature.
- N. G. Sanchez, Int. J. Mod Phys D28, 1950055 (2019).
- N. G. Sanchez, Int. J. Mod Phys A34, 1950155 (2019).
- N. G. Sanchez, Phys. Rev. D 104, 123517 (2021).
- N. G. Sanchez, Phys. Rev. D 107, 126018 (2023).
- H. J. de Vega, J.A. Siebert, Nucl.Phys. B707, 529 (2005).
- H. J. de Vega, N. Sanchez, Phys. Lett. B197, 320 (1987).
- A. H. Guth and S. Y. Pi, Phys. Rev. D 32, 1899 (1985).
- A. Albrecht, P. Ferreira, M. Joyce and T. Prokopec, Phys. Rev. D 50 , 4807-4820 (1994).
- D. J. Cirilo-Lombardo, , J.Math.Phys. 57 (2016) 6, 063503.
- D. J. Cirilo-Lombardo and Thiago Prudoncio, Int.J.Geom.Meth.Mod.Phys. 11 (2014) 08, 1450067.
- Diego Julio Cirilo-Lombardo, Physics Letters B 661,(2008) 186-191.
- D. J. Cirilo-Lombardo; The European Physical Journal C - Particles and Fields, (2012), Volume 72, Number 7, 2079.
- S. S. Sannikov, JETP 49, (1965) 1913.
- Arvind, Biswadeb Dutta, Mehta C. L., and Mukunda N., Phys. Rev. A 50, 39 (1994).
- P.A.M. Dirac, Proc. Roy. Soc. A322 (1971) 435.
- E. Majorana, Nuovo Cimento 9, (1932) 335.
- G. Dattoli et al., J. Phys. A: Math. Theor. 48, 125203 (2015).
- J. D. Bekenstein, Phys Rev D 7 (1973) 2333. SW Hawking, Black hole explosions, Nature 248 (1974) 30.
- J. D. Bekenstein, in "Quantum Black Holes as Atoms" : Proceedings of the Eight Marcel Grossmann Meeting, T. Piran and R. Ruffini, eds. (World Scientific Singapore 1999), pp. 92-111.
- V. V. Dodonov, `Nonclassical’ states in quantum optics: a `squeezed’ review of the first 75 years,J. Opt. B: Quantum Semiclass. Opt. (2002) 4 R1. [CrossRef]
- Diego Julio Cirilo-Lombardo; Foundations of Physics 37 (2007) 919-950.
- D. J. Cirilo-Lombardo, Found Phys 39 (2009) 373–396.
- D. J. Cirilo-Lombardo with V.I. Afonso, Phys.Lett.A376 (2012) 3599 .
- See for example: M. B. Green, J.H. Schwartz and E. Witten, Superstring Theory I and II, (CUP, Cambridge 1988).
- D. V. Volkov, A. I. Pashnev,“Supersymmetric lagrangian for particles in proper time”,Theoret. and Math. Phys. 44 (3) (1980) 770. [CrossRef]
- R. Casalbuoni, Relativity and Supersymmetries,Phys. Lett. B 62 (1976) 49. [CrossRef]
- J. D. Bekenstein, VF Mukhanov, “Spectroscopy of the quantum black hole”, [gr-qc/9505012].
- A. G. Bashkirov and A. D. Sukhanov, Entropy of open quantum systems and the Poisson distribution, Theoretical and Mathematical Physics, Vol. 123, No. 1, (2000), 504. [CrossRef]
Disclaimer/Publisher’s Note: The statements, opinions and data contained in all publications are solely those of the individual author(s) and contributor(s) and not of MDPI and/or the editor(s). MDPI and/or the editor(s) disclaim responsibility for any injury to people or property resulting from any ideas, methods, instructions or products referred to in the content. |
© 2023 by the authors. Licensee MDPI, Basel, Switzerland. This article is an open access article distributed under the terms and conditions of the Creative Commons Attribution (CC BY) license (http://creativecommons.org/licenses/by/4.0/).