In quantum gravity, a virtual black hole is a black hole that exists temporarily as a result of a quantum fluctuation of spacetime.[1] It is an example of quantum foam and is the gravitational analog of the virtual electron–positron 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.[2]
The emergence of virtual black holes at the Planck scale is a consequence of the uncertainty relation
\( \Delta R_{{\mu }}\Delta x_{{\mu }}\geq \ell _{{P}}^{2}={\frac {\hbar G}{c^{3}}} \)
where \( R_{{\mu }} \) is the radius of curvature of space-time small domain, \( x_{{\mu }} \) is the coordinate of the small domain, \( \ell _{{P}} \) is the Planck length, \( \hbar \) is the Planck constant, G is Newton's gravitational constant, and c is the speed of light. These uncertainty relations are another form of Heisenberg's uncertainty principle at the Planck scale.
Proof: Indeed, these uncertainty relations can be obtained on the basis of Einstein's equations
\( G_{{\mu \nu }}+\Lambda g_{{\mu \nu }}={8\pi G \over c^{4}}T_{{\mu \nu }} \)
where \( G_{{\mu \nu }}=R_{{\mu \nu }}-{R \over 2}g_{{\mu \nu }} \) is the Einstein tensor, which combines the Ricci tensor, the scalar curvature and the metric tensor; \( \Lambda \) is the cosmological constant; а \( T_{\mu \nu } \) is the energy-momentum tensor of matter; \( \pi \) is the mathematical constant pi; c is the speed of light; and G {\displaystyle G} G isNewton's gravitational constant.
In the derivation of his equations, Einstein suggested that physical space-time is Riemannian, ie curved. A small domain of it is approximately flat space-time.
For any tensor field \( N_{{\mu \nu ...}} \), we may call \( N_{{\mu \nu ...}}{\sqrt {-g}} \) a tensor density, where g {\displaystyle g} g is the determinant of the metric tensor \( g_{\mu \nu } \). The integral \( \int N_{{\mu \nu ...}}{\sqrt {-g}}\,d^{4}x \) 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.[3] Here we consider only small domains. This is also true for the integration over the three-dimensional hypersurface \( S^{{\nu }}. \)
Thus, Einstein's equations for small space-time domain can be integrated by the three-dimensional hypersurface \( S^{{\nu }} \). Have[4]
\( {\frac {1}{4\pi }}\int \left(G_{{\mu \nu }}+\Lambda g_{{\mu \nu }}\right){\sqrt {-g}}\,dS^{{\nu }}={2G \over c^{4}}\int T_{{\mu \nu }}{\sqrt {-g}}\,dS^{{\nu }} \)
Since integrable space-time domain is small, we obtain the tensor equation
\( R_{{\mu }}={\frac {2G}{c^{3}}}P_{{\mu }} \)
where \( P_{{\mu }}={\frac {1}{c}}\int T_{{\mu \nu }}{\sqrt {-g}}\,dS^{{\nu }} \) is the component of the 4-momentum of matter, \( R_{{\mu }}={\frac {1}{4\pi }}\int \left(G_{{\mu \nu }}+\Lambda g_{{\mu \nu }}\right){\sqrt {-g}}\,dS^{{\nu }} \) is the component of the radius of curvature small domain.
The resulting tensor equation can be rewritten in another form. Since \( P_{{\mu }}=mc\,U_{{\mu }} \) then
\( R_{{\mu }}={\frac {2G}{c^{3}}}mc\,U_{{\mu }}=r_{s}\,U_{{\mu }} \)
where \( r_{s} \) is the Schwarzschild radius, \( U_{{\mu }} \) is the 4-speed, m {\displaystyle m} m is the gravitational mass. This record reveals the physical meaning of the \( R_{{\mu }} \) values as a components of the gravitational radius \( r_{s} \).
In a small area of space-time is almost flat and this equation can be written in the operator form
\( {\displaystyle {\hat {R}}_{\mu }={\frac {2G}{c^{3}}}{\hat {P}}_{\mu }={\frac {2G}{c^{3}}}(-i\hbar ){\frac {\partial }{\partial \,x^{\mu }}}=-2i\,\ell _{P}^{2}{\frac {\partial }{\partial \,x^{\mu }}}} \)
or
The basic equation of quantum gravity [4]
\( {\displaystyle -2i\ell _{P}^{2}{\frac {\partial }{\partial x^{\mu }}}|\Psi (x_{\mu })\rangle ={\hat {R}}_{\mu }|\Psi (x_{\mu })\rangle } \)
Then the commutator of operators \( {\hat R}_{{\mu }} \) and \( {\hat x}_{{\mu }} \) is
\( [{\hat R}_{{\mu }},{\hat x}_{{\mu }}]=-2i\ell _{{P}}^{2}
From here follow the specified uncertainty relations
\( \Delta R_{{\mu }}\Delta x_{{\mu }}\geq \ell _{{P}}^{2} \)
Substituting the values of \( R_{{\mu }}={\frac {2G}{c^{3}}}m\,c\,U_{{\mu }} \) and \( \ell _{{P}}^{2}={\frac {\hbar \,G}{c^{3}}} \) and reducing identical constants from two sides, we get Heisenberg's uncertainty principle
\( \Delta P_{{\mu }}\Delta x_{{\mu }}=\Delta (mc\,U_{{\mu }})\Delta x_{{\mu }}\geq {\frac {\hbar }{2}} \)
In the particular case of a static spherically symmetric field and static distribution of matter \( U_{{0}}=1,U_{i}=0\,(i=1,2,3) \) and have remained
\( \Delta R_{{0}}\Delta x_{{0}}=\Delta r_{s}\Delta r\geq \ell _{{P}}^{2} \)
where \( r_{s} \) is the Schwarzschild radius, r is the radial coordinate. Here \( {\displaystyle R_{0}=r_{s}} \) and \( {\displaystyle x_{0}=c\,t=r} \), since the matter moves with velocity of light in the Planck scale.
Last uncertainty relation allows make us some estimates of the equations of general relativity at the Planck scale. For example, the equation for the invariant interval d S {\displaystyle dS} dS в in the Schwarzschild solution has the form
\( dS^{2}=\left(1-{\frac {r_{s}}{r}}\right)c^{2}dt^{2}-{\frac {dr^{2}}{1-{r_{s}}/{r}}}-r^{2}(d\Omega ^{2}+\sin ^{2}\Omega d\varphi ^{2}) \)
Substitute according to the uncertainty relations \( r_{s}\approx \ell _{P}^{2}/r \). We obtain
\( {\displaystyle dS^{2}\approx \left(1-{\frac {\ell _{P}^{2}}{r^{2}}}\right)c^{2}dt^{2}-{\frac {dr^{2}}{1-{\ell _{P}^{2}}/{r^{2}}}}-r^{2}(d\Omega ^{2}+\sin ^{2}\Omega d\varphi ^{2})} \)
It is seen that at the Planck scale \( r=\ell _{P} \) 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 for three-dimensional space for the emergence of virtual black holes (quantum foam, the basis of the "fabric" of the Universe.).[4] 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.
If virtual black holes exist, they provide a mechanism for proton decay. This is because when a black hole's mass increases via mass falling into the hole, and is theoretised 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.[2]
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.[5]
See also
Quantum foam
Virtual particle
References
S. W. Hawking (1995) "Virtual Black Holes"
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.
P. A. M.Dirac(1975), General Theory of Relativity, Wiley Interscience, p.37
A.P.Klimets(2012) "Postigaya mirozdanie", LAP LAMBERT Academic Publishing, Deutschland
The black hole information paradox, Steven B. Giddings, arXiv:hep-th/9508151v1.
vte
Black holes
Types
Schwarzschild Rotating Charged Virtual Kugelblitz Primordial Planck particle
Black hole - Messier 87 crop max res.jpg
Size
Micro
Extremal Electron Stellar
Microquasar Intermediate-mass Supermassive
Active galactic nucleus Quasar Blazar
Formation
Stellar evolution Gravitational collapse Neutron star
Related links Tolman–Oppenheimer–Volkoff limit White dwarf
Related links Supernova
Related links Hypernova Gamma-ray burst Binary black hole
Properties
Gravitational singularity
Ring singularity Theorems Event horizon Photon sphere Innermost stable circular orbit Ergosphere
Penrose process Blandford–Znajek process Accretion disk Hawking radiation Gravitational lens Bondi accretion M–sigma relation Quasi-periodic oscillation Thermodynamics
Immirzi parameter Schwarzschild radius Spaghettification
Issues
Black hole complementarity Information paradox Cosmic censorship ER=EPR Final parsec problem Firewall (physics) Holographic principle No-hair theorem
Metrics
Schwarzschild (Derivation) Kerr Reissner–Nordström Kerr–Newman Hayward
Alternatives
Nonsingular black hole models Black star Dark star Dark-energy star Gravastar Magnetospheric eternally collapsing object Planck star Q star Fuzzball
Analogs
Optical black hole Sonic black hole
Lists
Black holes Most massive Nearest Quasars Microquasars
Related
Black Hole Initiative Black hole starship Compact star Exotic star
Quark star Preon star Gamma-ray burst progenitors Gravity well Hypercompact stellar system Membrane paradigm Naked singularity Quasi-star Rossi X-ray Timing Explorer Timeline of black hole physics White hole Wormhole
Hellenica World - Scientific Library
Retrieved from "http://en.wikipedia.org/"
All text is available under the terms of the GNU Free Documentation License
