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''Intern. J. Mod. Phys. A'', '''16''', 2399.</ref>
''Intern. J. Mod. Phys. A'', '''16''', 2399.</ref>


The emergence of virtual [[black holes]] at the [[Planck scale]] is a consequence of the uncertainty relation <ref>[https://www.opastpublishers.com/open-access-articles/quantum-gravity.pdf A.P. Klimets. (2023). Quantum Gravity. Current Research in Statistics & Mathematics, 2(1), 141-155.]</ref>
The emergence of virtual [[black holes]] at the [[Planck scale]] is a consequence of the uncertainty relation <ref name="klimets1">[https://www.opastpublishers.com/open-access-articles/quantum-gravity.pdf A.P. Klimets. (2023). Quantum Gravity. Current Research in Statistics & Mathematics, 2(1), 141-155.]</ref>
:<math>\Delta R_{\mu}\Delta x_{\mu}\ge\ell^2_{P}=\frac{\hbar G}{c^3}</math>
:<math>\Delta R_{\mu}\Delta x_{\mu}\ge\ell^2_{P}=\frac{\hbar G}{c^3}</math>
where <math>R_{\mu}</math> is the radius of curvature of spacetime small domain, <math>x_{\mu}</math> is the coordinate of the small domain, <math>\ell_{P}</math> is the [[Planck length]], <math>\hbar</math> is the [[reduced Planck constant]], <math>G</math> is the [[Newtonian constant of gravitation]], and <math>c</math> is the [[speed of light]]. These uncertainty relations are another form of Heisenberg's [[uncertainty principle]] at the [[Planck scale]].
where <math>R_{\mu}</math> is the radius of curvature of spacetime small domain, <math>x_{\mu}</math> is the coordinate of the small domain, <math>\ell_{P}</math> is the [[Planck length]], <math>\hbar</math> is the [[reduced Planck constant]], <math>G</math> is the [[Newtonian constant of gravitation]], and <math>c</math> is the [[speed of light]]. These uncertainty relations are another form of Heisenberg's [[uncertainty principle]] at the [[Planck scale]].
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For any tensor field <math>N_{\mu\nu...}</math>, we may call <math>N_{\mu\nu...}\sqrt{-g}</math> a tensor density, where <math>g</math> is the [[determinant]] of the [[metric tensor]] <math>g_{\mu\nu}</math>. The integral <math>\int N_{\mu\nu...}\sqrt{-g}\,d^4x</math> is a tensor if the domain of integration is small. It is not a tensor if the domain of integration is not small, because it then consists of a sum of tensors located at different points and it does not transform in any simple way under a transformation of coordinates.<ref>[https://vk.com/doc264717166_454951866 P.A.M. Dirac(1975), General Theory of Relativity, Wiley Interscience], p.37</ref> Here we consider only small domains. This is also true for the integration over the three-dimensional [[hypersurface]] <math>S^{\nu}</math>.
For any tensor field <math>N_{\mu\nu...}</math>, we may call <math>N_{\mu\nu...}\sqrt{-g}</math> a tensor density, where <math>g</math> is the [[determinant]] of the [[metric tensor]] <math>g_{\mu\nu}</math>. The integral <math>\int N_{\mu\nu...}\sqrt{-g}\,d^4x</math> is a tensor if the domain of integration is small. It is not a tensor if the domain of integration is not small, because it then consists of a sum of tensors located at different points and it does not transform in any simple way under a transformation of coordinates.<ref>[https://vk.com/doc264717166_454951866 P.A.M. Dirac(1975), General Theory of Relativity, Wiley Interscience], p.37</ref> Here we consider only small domains. This is also true for the integration over the three-dimensional [[hypersurface]] <math>S^{\nu}</math>.


Thus, the [[Einstein field equations]] for a small spacetime domain can be integrated by the three-dimensional [[hypersurface]] <math>S^{\nu}</math>. Have<ref name="klimets">[https://philpapers.org/archive/ALXOTF.pdf Klimets A.P., Philosophy Documentation Center, Western University-Canada, 2017, pp.25–32]</ref><ref>[https://www.opastpublishers.com/open-access-articles/quantum-gravity.pdf A.P. Klimets. (2023). Quantum Gravity. Current Research in Statistics & Mathematics, 2(1), 141-155.]</ref>
Thus, the [[Einstein field equations]] for a small spacetime domain can be integrated by the three-dimensional [[hypersurface]] <math>S^{\nu}</math>. Have<ref name="klimets1"/><ref name="klimets">[https://philpapers.org/archive/ALXOTF.pdf Klimets A.P., Philosophy Documentation Center, Western University-Canada, 2017, pp.25–32]</ref>
: <math>\frac{1}{4\pi}\int\left (G_{\mu\nu} + \Lambda g_{\mu\nu}\right )\sqrt{-g}\,dS^{\nu} = {2G \over c^4} \int T_{\mu\nu}\sqrt{-g}\,dS^{\nu}</math>
: <math>\frac{1}{4\pi}\int\left (G_{\mu\nu} + \Lambda g_{\mu\nu}\right )\sqrt{-g}\,dS^{\nu} = {2G \over c^4} \int T_{\mu\nu}\sqrt{-g}\,dS^{\nu}</math>
Since integrable space-time ''domain'' is small, we obtain the tensor equation
Since integrable space-time ''domain'' is small, we obtain the tensor equation
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{{Equation box 1
{{Equation box 1
|indent=:
|indent=:
|title=''The basic equation of quantum gravity'' <ref name="klimets"/>
|title=''The basic equation of quantum gravity'' <ref name="klimets1"/><ref name="klimets"/>
|equation=<math>-2i\ell^2_{P}\frac{\partial}{\partial x^{\mu}}|\Psi(x_{\mu})\rangle=\hat R_{\mu}|\Psi(x_{\mu})\rangle</math>
|equation=<math>-2i\ell^2_{P}\frac{\partial}{\partial x^{\mu}}|\Psi(x_{\mu})\rangle=\hat R_{\mu}|\Psi(x_{\mu})\rangle</math>
|cellpadding
|cellpadding
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It is seen that at the [[Planck scale]] <math>r=\ell_P</math> space-time metric is bounded below by the [[Planck length]] (division by zero appears), and on this scale, there are real and virtual Planckian black holes.
It is seen that at the [[Planck scale]] <math>r=\ell_P</math> space-time metric is bounded below by the [[Planck length]] (division by zero appears), and on this scale, there are real and virtual Planckian black holes.


Similar estimates can be made in other equations of [[general relativity]]. For example, analysis of the [[Hamilton–Jacobi equation]] for a centrally symmetric gravitational field in spaces of different dimensions (with help of the resulting uncertainty relation) indicates a preference (energy profitability) for three-dimensional space for the emergence of virtual black holes ([[quantum foam]], the basis of the "fabric" of the Universe.).<ref name="klimets"/> This may have predetermined the three-dimensionality of the observed space.
Similar estimates can be made in other equations of [[general relativity]]. For example, analysis of the [[Hamilton–Jacobi equation]] for a centrally symmetric gravitational field in spaces of different dimensions (with help of the resulting uncertainty relation) indicates a preference (energy profitability) for three-dimensional space for the emergence of virtual black holes ([[quantum foam]], the basis of the "fabric" of the Universe.).<ref name="klimets1"/><ref name="klimets"/> This may have predetermined the three-dimensionality of the observed space.


Prescribed above uncertainty relation valid for strong gravitational fields, as in any sufficiently small domain of a strong field space-time is essentially flat.
Prescribed above uncertainty relation valid for strong gravitational fields, as in any sufficiently small domain of a strong field space-time is essentially flat.

Latest revision as of 06:03, 19 March 2024

In quantum gravity, a virtual black hole[1] is a hypothetical micro black hole that exists temporarily as a result of a quantum fluctuation of spacetime.[2] It is an example of quantum foam and is the gravitational analog of the virtual electronpositron pairs found in quantum electrodynamics. Theoretical arguments suggest that virtual black holes should have mass on the order of the Planck mass, lifetime around the Planck time, and occur with a number density of approximately one per Planck volume.[3]

The emergence of virtual black holes at the Planck scale is a consequence of the uncertainty relation [4]

where is the radius of curvature of spacetime small domain, is the coordinate of the small domain, is the Planck length, is the reduced Planck constant, is the Newtonian constant of gravitation, and is the speed of light. These uncertainty relations are another form of Heisenberg's uncertainty principle at the Planck scale.

If virtual black holes exist, they provide a mechanism for proton decay.[8] This is because when a black hole's mass increases via mass falling into the hole, and is theorized to decrease when Hawking radiation is emitted from the hole, the elementary particles emitted are, in general, not the same as those that fell in. Therefore, if two of a proton's constituent quarks fall into a virtual black hole, it is possible for an antiquark and a lepton to emerge, thus violating conservation of baryon number.[3][9]

The existence of virtual black holes aggravates the black hole information loss paradox, as any physical process may potentially be disrupted by interaction with a virtual black hole.[10]

See also[edit]

References[edit]

  1. ^ S. W. Hawking (1995) "Virtual Black Holes"
  2. ^ a b Fred C. Adams, Gordon L. Kane, Manasse Mbonye, and Malcolm J. Perry (2001), "Proton Decay, Black Holes, and Large Extra Dimensions", Intern. J. Mod. Phys. A, 16, 2399.
  3. ^ a b c d A.P. Klimets. (2023). Quantum Gravity. Current Research in Statistics & Mathematics, 2(1), 141-155.
  4. ^ P.A.M. Dirac(1975), General Theory of Relativity, Wiley Interscience, p.9
  5. ^ P.A.M. Dirac(1975), General Theory of Relativity, Wiley Interscience, p.37
  6. ^ a b c Klimets A.P., Philosophy Documentation Center, Western University-Canada, 2017, pp.25–32
  7. ^ Bambi, Cosimo; Freese, Katherine (2008). "Dangerous implications of a minimum length in quantum gravity". Classical and Quantum Gravity. 25 (19): 195013. arXiv:0803.0749. Bibcode:2008CQGra..25s5013B. doi:10.1088/0264-9381/25/19/195013. hdl:2027.42/64158. S2CID 2040645.
  8. ^ Al-Modlej, Abeer; Alsaleh, Salwa; Alshal, Hassan; Ali, Ahmed Farag (2019). "Proton decay and the quantum structure of space–time". Canadian Journal of Physics. 97 (12): 1317–1322. arXiv:1903.02940. Bibcode:2019CaJPh..97.1317A. doi:10.1139/cjp-2018-0423. hdl:1807/96892. S2CID 119507878.
  9. ^ The black hole information paradox, Steven B. Giddings, arXiv:hep-th/9508151v1.