Journal of High Energy Physics, Gravitation and Cosmology, 2018, 4, 361-440 http://www.scirp.org/journal/jhepgc ISSN Online: 2380-4335 ISSN Print: 2380-4327 DOI: 10.4236/jhepgc.2018.42023 Apr. 30, 2018 361 Journal of High Energy Physics, Gravitation and Cosmology Was Polchinski Wrong? Colombeau Distributional Rindler Space-Time with Distributional Levi-Cività Connection Induced Vacuum Dominance. Unruh Effect Revisited Jaykov Foukzon1, Alexander Potapov2, Elena Men'kova3 1Center for Mathematical Sciences, Israel Institute of Technology, Haifa, Israel 2IRE RAS, Moscow, Russia 3All-Russian Research Institute for Optical and Physical Measurements, Moscow, Russia Abstract The vacuum energy density of free scalar quantum field Φ in a Rindler distributional space-time with distributional Levi-Cività connection is considered. It has been widely believed that, except in very extreme situations, the influence of acceleration on quantum fields should amount to just small, sub-dominant contributions. Here we argue that this belief is wrong by showing that in a Rindler distributional background space-time with distributional Levi-Cività connection the vacuum energy of free quantum fields is forced, by the very same background distributional space-time such a Rindler distributional background space-time, to become dominant over any classical energy density component. This semiclassical gravity effect finds its roots in the singular behavior of quantum fields on a Rindler distributional space-times with distributional Levi-Cività connection. In particular we obtain that the vacuum fluctuations 2Φ have a singular behavior at a Rindler horizon ( )2 4 20 : , ,R c a aδ δ δ δ−= Φ →∞  . Therefore sufficiently strongly accelerated observer burns up near the Rindler horizon. Thus Polchinski's account doesn't violate the Einstein equivalence principle. Keywords Vacuum Energy Density, Rindler Distributional Space-Time, Levi-Cività Connection, Semiclassical Gravity Effect, Einstein Equivalence Principle How to cite this paper: Foukzon, J., Potapov, A. and E. Men'kova (2018) Was Polchinski Wrong? Colombeau Distributional Rindler Space-Time with Distributional Levi-Cività Connection Induced Vacuum Dominance. Unruh Effect Revisited. Journal of High Energy Physics, Gravitation and Cosmology, 4, 361-440. https://doi.org/10.4236/jhepgc.2018.42023 Received: January 18, 2018 Accepted: April 27, 2018 Published: April 30, 2018 Copyright © 2018 by authors and Scientific Research Publishing Inc. This work is licensed under the Creative Commons Attribution International License (CC BY 4.0). http://creativecommons.org/licenses/by/4.0/ Open Access J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 362 Journal of High Energy Physics, Gravitation and Cosmology Space-Time, Levi-Cività Connection, Semiclassical Gravity Effect, Einstein Equivalence Principle 1. Introduction In March 2012, Joseph Polchinski claimed that the following three statements cannot all be true [1]: 1) Hawking radiation is in a pure state, 2) the information carried by the radiation is emitted from the region near the horizon, with low energy effective field theory valid beyond some microscopic distance from the horizon, 3) the infalling observer encounters nothing unusual at the horizon. Joseph Polchinski argues that the most conservative resolution is: the infalling observer burns up at the horizon. In Polchinski's account, quantum effects would turn the event horizon into a seething maelstrom of particles. Anyone who fell into it would hit a wall of fire and be burned to a crisp in an instant. As pointed out by physics community such firewalls would violate a foundational tenet of contemporary physics known as the equivalence principle, it states in part that an observer falling in a gravitational field-even the powerful one inside a black hole-will see exactly the same phenomena as an accelerated observer floating in empty space. In this paper we argue that Polchinski was not wrong, but Unruh effect revision is needed. 1.1. What Is Colombeau Distributional Semi-Riemannian Geometry? Recall that the classical Cartan's structural equations show in a compact way the relation between a connection and its curvature, and reveal their geometric interpretation in terms of moving frames. In order to study the mathematical properties of singularities, we need to study the geometry of manifolds endowed on the tangent bundle with a symmetric bilinear form it is allowed to become degenerate (singular). Remark 1.1.1. But if the fundamental tensor is allowed to be degenerate (singular), there are some obstructions in constructing the geometric objects normally associated to the fundamental tensor. Also, local orthonormal frames and coframes no longer exist, as well as the metric connection and its curvature operator [2]. Remark 1.1.2. "Singular Semi-Riemannian Geometry"-the main brunch of contemporary semi-Riemannian geometry in which have been studied a smooth manifolds M furnished with a degenerate (singular) on a smooth submanifold M M′ metric tensor of arbitrary signature have been studied [2]. Remark 1.1.3. In order to solve problems of the gravitational singularity in classical general relativity the singular semi-Riemannian geometry based on Colombeau calculas and Colombeau generalized functions was much developed, see [3]-[22]. J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 363 Journal of High Energy Physics, Gravitation and Cosmology Remark 1.1.4. Let ( )M ′G be algebra of Colombeau generalized functions on M M′ ⊂ , let  be the ring of Colombeau generalized numbers [3] [4] [5]. Let ( )gε ε be Colombeau generalized metric tensor on M and let ( )M p′Ric be generalized Ricci tensor of the metric ( )( ) M g pε ε ′ [20] [21]. The main properties of such nonclassical manifolds with a degenerate (singular) metric tensor that is ( ) ( ) ( )\M p M C M∞′ ′ ′∈Ric G , i.e. for all ( ): \Mp M p′′∈ ∈  Ric . Definition 1.1.1. Let ( )M ′G be algebra of Colombeau generalized functions on M M′ ⊂ , and let ( )( )g pε ε be Colombeau generalized metric tensor on M such that ( )( )g pε ε is the Colombeau solution of the Einstein field Equation (1.3.19), (see Remark 1.3.7). We define now the Colombeau distributional scalar curvature ( ) ( )( ),M Mp pε ε =  R R (or distributional Ricci [20] [21] scalar) as the trace of ( ) ( )( ),M Mp pε ε =  Ric Ric , i.e. ( ) ( )( ),M Mp pε ε =  R tr Ric . Assume that ( ) ( ) ( )\M p M C M∞′ ′ ′∈R G . Then we say that: (i) gravitational field ( )( )g pε ε (or corresponding distributional spacetime) has a gravitational singularity on a smooth compact submanifold cM M⊂ iff ( ) ( ) ( )\cM c cp M C M ∞∈R G ; (ii) gravitational field ( )( )g pε ε has a gravitational singularity with compact support iff ( ) ( )3cM p D′∈ R . Remark 1.1.5. It turns out that the distributional Schwarzschild spacetime has a gravitational singularity with compact support at origin { }0r = [6]-[11] and at Schwarzschild horizon { }2 2r m× =S [18] [19]. Definition 1.1.2. (i) Let ( )MG be algebra of Colombeau generalized functions on M, and let ( )( )g pε ε be Colombeau generalized metric tensor on M such that ( )( )g pε ε is the Colombeau solution of the generalized Einstein field Equation (1.3.19). The generalized point value of ( )( )g pε ε at generalized point ( )( )pε ε is ( )( )g pε ε ε . (ii) We define now the generalized point value of the distributional scalar curvature ( )M pR at generalized point ( )( )pε ε =  p by formula ( ) ( )( ),M M pε ε ε =  R p R . 1.2. Distributional Møller's Geometry as Colombeau Extension of the Classical Moller's Spacetime As important example of Colombeau extension of the singular semi-Riemannian geometry mentioned above, we consider now Moller's uniformly accelerated frame given by Moller's line element [23]: ( )22 2 2 2 2d d d d d .s a gx t x y z= − + + + + (1.2.1) Of couse Moller's metric (1.2.1) degenerate at Moller horizon ( ) 1Molhorx a g −= − . Note that formally corresponding to the metric (1.2.1) classical Levi-Civitá connection is [23] ( ) ( ) ( ) ( )1 4 444 14 41 1,x a gx x x a gx Γ = + Γ = Γ = + (1.2.2) and therefore classical Levi-Civit'a connection (1.2.2) of couse is not available at Moller horizon 1Molhorx a g −= − ⋅ . Recall that fundamental tensor corresponding to J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 364 Journal of High Energy Physics, Gravitation and Cosmology the metric (1.2.1) was obtained in Moller's paper [23] as a vacuum solution of the classical Einstein's field equations 1 0, 2 k k k i i iG R Rδ= − = (1.2.3) where kiR is the contracted Riemann-Christoffel tensor formally calculated by canonical way by using classical Levi-Civitá connection (1.2.2) and iiR R= . Using Dingle's formula [23] in case of the metric (1.2.1) we get ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) 2 2 3 2 3 2 1 , 2 2 , x G x G x x x x x a gx  ′∆   ′′= = − ∆ −  ∆ ∆   ∆ = + (1.2.4) where ( ) ( )x x x′∆ = ∂∆ ∂ and all other components of kiG vanishes identically. Note that ( ) ( ) ( ) 22 , 2 .x g a gx x g′ ′′∆ = + ∆ = (1.2.5) Thus for any 1x a g−≠ − ⋅ we get a classical result ( ) ( ) ( ) ( ) ( ) 22 2 3 2 2 3 41 2 0. 2 2 g a gx G x G x g x x  + = = − − ≡  ∆ ∆   (1.2.6) Let { }n nx ∈ be a sequence such that 1 1lim , ,n n nx a g x a g n − − →∞ = − ⋅ ≠ − ⋅ ∈ . Then for any n∈ we get ( ) ( ) ( ) ( ) ( ) ( ) 22 2 3 2 2 3 41 2 0, 2 2 n n n n n n g a gx x G x G x g x x  + I = = = − − ≡  ∆ ∆   (1.2.7) and therefore ( )lim 0n nx→∞ I ≡ . However ( ) ( )4 414 41 1lim lim lim ,n nn n n n x x a gx→∞ →∞ →∞ Γ = Γ = = ∞ + (1.2.8) i.e. classical Levi-Civit'a connection given by (1.2.2) unavailable at Moller horizon. Remark 1.2.1. In order to avoid difficultness mentioned above, we consider now the regularized Moller's metric ( ) ( ) ( ) ( ] 2 2 2 2 2 2 2 d d d d d , , 0,1 . s x t x y z x a gx ε ε ε ε ε = −∆ + + +  ∆ = + + ∈  (1.2.9) Using now Dingle's formula [23] for the case of (1.2.9) we get ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) 2 2 3 2 3 2 2 1; ; ; , 2 2 . x x G x G x x x x x a gx ε ε ε ε ε ε ε ε ε  ′∆   ′′I = = = − ∆ −  ∆ ∆    ∆ = + +  (1.2.10) Note that ( ) 22 1 , 2g gx gε ε′ ′′∆ = + ∆ = (1.2.11) and therefore J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 365 Journal of High Energy Physics, Gravitation and Cosmology ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) 22 2 22 2 2 2 2 2 2 2 21; 2 2 2 21 2 2 . g a gx x g x x g a gx g g x x g x ε ε ε ε ε ε ε ε ε  + I = − −  ∆ ∆     + + −  = − −  ∆ ∆   = − ∆ (1.2.12) Remark 1.2.2. (i) Note that ( )( ) ( ]; , 0,1x εε εI ∈ is Colombeau generalized function such that ( )( ) ( );x εε I ∈  cl G and ( )( )( ) ( )1 2; .a g εεε ε − −   I − = ∈     cl cl Remark 1.2.3. Note that: (i) at any point x∈   such that x∈ and 1x a g−≠ − ⋅ one obtains ( )( ); 0x εεI ≈    (see Definition 1.5.0 (i)) and therefore the Ricci tensor as well as the Ricci scalar are infinite small beyond Moller horizon 1Mhorx a g −= − ⋅ . Thus at any point x such that x∈ and 1x a g−≠ − ⋅ we obtain the disered result in a good agriment with formall canonical calculation (see for example [24], subsect. 2.1.6), (ii) obviously at any finite point finx ∈  (see Definition 1.5.0 (iii)) one obtains again ( )( ); 0.x εεI ≈    Remark 1.2.4. (I) Thus Colombeau generalized fundamental tensor ( )( )ikg εε corresponding to Colombeau metric ( ) ( )( ) ( )( ) ( )( ) ( ] 2 2 2 2 2 2 2 d d d d d , , 0,1 s x t x y z x a gx ε ε ε ε ε ε ε ε = − ∆ + + +  ∆ = + + ∈  (1.2.13) that is non vacuum Colombeau solution (see [18] section 6 and [19] subsection 2.3 Distributional general relativity) of the Einstein's field equations ( )( ) ( )( ) ( )( ) ( ) 2 2 2 1 . 2 k k k i i iG R R g xεε ε ε ε ε ε ε δ ε   = − = −   ∆  (1.2.14) For Rindler metric 0, 1a g= = and we get ( )( ) ( )( ) ( )( ) ( ) ( ) 2 22 2 1 . 2 k k k i i iG R R xεε ε ε ε ε ε δ ε ε    = − = − ∈  +  G (1.2.15) Definition 1.2.1. Distributional Moller's geometry that is Colombeau extension of the classical Moller's spacetime given by Colombeau generalized fundamental tensor (1.2.13). 1.3. Distributional Schwarzschild Geometry as Colombeau Extension of the Classical Singular Schwarzschild Spacetime 1.3.1. Colombeau Extension of the Classical Singular Schwarzschild Spacetime Furnished with a Degenerate and Singular Schwarzschild Metric As another important example of Colombeau extension of the singular J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 366 Journal of High Energy Physics, Gravitation and Cosmology semi-Riemannian geometry we consider now classical singular Schwarzschild spacetime furnished with a degenerate and singular Schwarzschild metric 1 2 2 2 2 22 2d 1 d 1 d dm ms t r r r r −    = − − + − + Ω        (1.3.1) Remark 1.3.1. Note that formally corresponding to the metric (1.3.1) classical Levi-Civitá connection given by canonical Christoffel symbols are [24]: ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) 1 1 00 1132 22 2 0 01 2 2 2 1 1 1 12 222 22 2 3 1 1 1 2 13 332 22 2 2 lim 0, lim , 2 lim , 2 1lim 2 , lim 2 0, 1lim 2 , lim 2 sin 0, r m r mr m r m r m r m r m r mr m r m r m r mr m r m m r m mr r r r mr mr r r m r m r m r m r m r θ = =→ → = → − − = =→ → − − = =→ → − − Γ = = Γ = = ∞ − Γ = = ∞ − Γ = = Γ = − − = Γ = = Γ = − − = (1.3.2) ( ) ( ) ( ) ( ) 1 1 00 1130 00 0 2 3 33 23 2 lim , lim , 2 cossin cos , . sin r rr r m r m mr r r r mr θθ θ θ = =→ → − − Γ = = ∞ Γ = = ∞ − Γ = − Γ =  i.e. classical Levi-Civita connection given by Equation (1.3.2) unavailable at Schwarzschild horizon. Remark 1.3.2. Nevertheless in classical handbooks [24]-[37] were mistakenly assumed that classical semi-Riemannian geometry holds on whole Schwarzschild manifold and therefore canonical formal calculation gives ( ) ( ) 2 6 16 .abcdabcd mR r R r r = (1.3.3) By Equation (1.3.2) it is mistakenly pointed out that the Schwarzschild metric has only a coordinate singularity at 2r m= and there is no gravitational singularity at Schwarzschild horizon. Remark 1.3.3. Note that canonical formal calculation gives ( ) ( ) 2 6 5 2 5 2 2 7 2 5 2 5 16 24 1 21 24 sin 1 2 sin1 4 2 21 8 sin 2 sin1 4 21 sin sin abcd abcd m m m mR r R r m rr rr r m m m m rrr r m m m mmr mr r rr r m m m r r r θ θ θ θ θ        = + − − −       −            + − − −       −      + − +     −     + −    2 21 m r θ  −    (1.3.4) J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 367 Journal of High Energy Physics, Gravitation and Cosmology Assume that 0r ≠ and 2r m≠ , i.e. 221 0,sin 0m r θ− ≠ ≠ , then from Equation (1.3.4) one obtains directly ( ) ( ) 2 6 5 5 22 2 2 2 6 6 6 6 6 16 4 4 124 16 4 48 . abcd abcd s m m m m mR r R r r rr r r rm m m m r r r r r        = + − − + − −               + + + = = (1.3.5) Remark 1.3.4. Notice that: if 2r m= then RHS of the Equation (1.3.4) become uncertainty ( ) ( ) 2 2 6 5 5 2 2 2 5 7 2 5 2 2 6 16 4 4 sin sin 4 2 48 sin sin sin sin 16 0 . 0 abcd abcd m m m m mR r R r r rr r r m m m m mmr r rr r r m r θ θ θ θ θ θ        = + − − + − −               + + + = + (1.3.6) A. Einstein emphasized that uncertainty of the form 0/0 mentioned above that is a fundamental mathematical problem, see [38], p. 74. However in order to avoid this difficulty mentioned above in physical literature [24]-[37] one mistakenly defines ( ) ( ) 2 2 6 52 2 5 2 2 7 2 5 lim 16 2lim 4 1 21 24 sin 1 2 sin1 4 2 21 8 sin 2 sin1 4 1 abcd abcdr m r m R r R r m m m m m rr rr r m m m m rrr r m m m mmr mr r rr r m r θ θ θ θ → →           = + − − −         −             + − − −       −      + − +     −    + 2 2 6 5 2 2 48sin 2sin 1 m m m mr rr r θ θ   − =     −   (1.3.7) However Equation (1.3.7) doesn't holds at 2r m= because classical Levi-Civitá connection (1.3.2) of course is not available at Schwarzschild horizon, see Remark 1.3.1. Remark 1.3.5. Thus from Equation (1.3.4) for 0r ≠ and 2r m≠ we get ( ) ( ) ( ) ( ) 2 6 16 0 2 ,abcdabcd mR r R r r r m r = ⇔ ≠ ∧ ≠ (1.3.8) and we get nothing at Schwarzschild horizon. Therefore semi-Riemannian geometry break down at Schwarzschild horizon [18] [19]. J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 368 Journal of High Energy Physics, Gravitation and Cosmology Remark 1.3.6. Recall that canonical derivation of the canonical singular Schwarzschild metric in classical handbooks is always based on assumption that: Assumption 1.3.1. Classical semi-Riemannian geometry holds on the whole semi-Riemannian manifold, see for example [26]. Let 2ds be the metric ( ) ( )2 2 2 2 2d d d d ,s A r t B r r r= − + + Ω (1.3.9) where , 1A B → as r →∞ . Then under Assumption 1.3.1 one obtains [26]: (i) all 1 vμΓ are zero except ( )1 1 1 1 200 11 22 332 , 2 , , sin ,A B B B r B r B θ′ ′Γ = Γ = Γ = − Γ = − (1.3.10) The equations 0, , 0,1, 2,3vR vμ μ= = are ( )1 1 0 100 00,1 00 01 00 ,1 2 2 2 log 2 2 2 2 2 2 1 2 0, 2 2 2 R g A A A A B B AB B A B r A B A AA B B A r = Γ − Γ Γ + Γ − ′′ ′ ′ ′ ′   = − + + +         ′ ′ ′ ′ ′′= − − + =    (1.3.11) and ( ) ( ) ( ) ( ) ( ) ( ) 2 21 0 1 11 11,1 10 11,1,1 2 22 3 1 21 31 11 ,1 2 log log 1 2 0, 2 2 2 R g g A B A ABA A B A rB = − − + Γ − Γ − Γ − Γ − Γ + Γ −  ′ ′ ′ ′ ′′= − + + + =    (1.3.12) and ( ) ( ) ( ) ( ) 21 1 2 3 1 22 22,1 22 21 23 22,2,2 ,1 2 log 2 log d cot 2 2cot 0. d 2 R g g ABr r B B B r AB θ θ θ = − − + Γ − Γ Γ − Γ + Γ −  ′′   = − − + − − + =       (1.3.13) From Equation (1.3.11)-Equation (1.3.12) one obtains ( )2 0.AB rB ′ = (1.3.14) Therefore AB = constant. Since at r →∞ we have A and 1B → one obtains 1B A−= . From Equation (1.3.13)-Equation (1.3.14) one obtains 1,r B ′  =    (1.3.15) and by integration Equation (1.3.15) one obtains 2r B r m= − , where 2m is an integration constant. Finally one obtains well known classical result ( ) ( ) 12 21 , 1 .m mA r B r r r −  = − = −    (1.3.16) J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 369 Journal of High Energy Physics, Gravitation and Cosmology From Equation (1.3.16) and consideration above (see Remark 1.3.4) Assumption 1.3.1 wrong, otherwise one obtains the contradiction. Remark 1.3.7. In order to avoid this difficulty: (i) we have introduced instead a classical Einstein field equations 1 8π , 2v v v R Rg GTμ μ μ− = − (1.3.17) [where the sign of the energy-momentum tensor is defined by ( ρ is the energy density)] 0 44 00 0 ,T T T ρ= − = = (1.3.18) apropriate Colombeau generalization of the Equation (1.3.17)-Equation (1.3.18) such that ( )( ) ( ) ( )( ) ( )( )1 8π , 2v v v R R g G Tμ μ με ε εε ε ε ε− = − (1.3.19) where the sign of the distributional energy-momentum tensor is defined by ( ) ( ) ( ) ( ) ( )044 00 0 ,T T T Mε ε ε ρ ε= − = = ∈G (1.3.20) see [18] [19]. (ii) we have introduced instead of Assumption 1.3.1 the following assumption. Assumption 1.3.2. Distributional semi-Riemannian geometry holds on the whole distributional semi-Riemannian manifold. Definition 1.3.1. Let ( ) [ ], 0,1A rε ε± ∈ and ( ) [ ], 0,1B rε ε± ∈ the regularization of the functions ( )A r± and ( )B r± [defined above by Equation (1.3.16)] such that the following conditions are satisfied: (i) ( )( ) ( )A rε ε± +∈ G and ( )( ) ( ) ( ], 0,1B rε ε ε± +∈ ∈G are Colombeau generalized functions; (ii) ( ) ( ) 1 0 0 2 21 , 1 ;m mA r B r r r − ± ±  = − = −    (1.3.21) (iii) ( )( ) ( ) ( )( ) ( )12 , 2 ;A m B mε εεε ε εε ε ± ± −= ∈ = ± ∈    (iv) ( )( ) ( ) ( )( ) ( ) 1 2 20 1 , 0 1 .m mA Bε εε ε ε εε ε − ± ±   = − ∈ = − ∈        Let 2dsε be the Colombeau metric ( ) ( )( ) ( )( )2 2 2 2 2d d d d ,s A r t B r r rε ε εε ε ε ± ±= − + + Ω (1.3.22) and let ( )( )vημ εεΓ be the distributional Levi-Civita connection [18] [19] corresponding to Colombeau metric (1.3.22). Then under Assumption 1.3.2 one obtains: (i) all ( )( )1 3bdμ εεΓ are zero except ( )( ) ( ) ( ) ( )( ) ( ) ( ) ( )( ) ( ) ( )( ) ( ) 1 00 1 11 1 22 1 2 33 2 , 2 , , sin , A B B B r B r B ε εε εε ε εε εε εε ε εε ε ε ε ε θ ′Γ = ′Γ = Γ = − Γ = − (1.3.23) J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 370 Journal of High Energy Physics, Gravitation and Cosmology ( )( ) ( )( ) ( )( ) ( )( ) ( )( ) ( )( )( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) 1 1 0 00 00,1 00 01 1 00 ,1 2 2 2 log 2 2 2 2 2 2 21 , 2 2 2 R g AA A A B B A B B A B r A AA B A B B A r ε ε ε ε ε ε εε ε ε εε ε ε ε ε ε ε ε ε ε εε ε ε ε ε ε ε εε ε ε ε ε ε εε ε ε ε ε ε ε ε ε± = Γ − Γ Γ + Γ − ′ ′ ′  ′  ′ ′  = − + + +            ′ ′′ ′  ′′= − − +     (1.3.24) and ( )( ) ( )( )( ) ( )( ) ( )( ) ( )( )( ) ( )( )( ) ( )( )( ) ( )( ) ( )( )( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) 2 21 0 1 11 11,1 10 11 ,1,1 2 22 3 1 21 31 11 ,1 2 log log 21 , 2 2 2 R g g AA B A B A A B A r B ε ε ε ε ε εε ε εε ε ε εε ε ε ε ε ε ε ε ε εε ε ε ε ε ε ε ε ε ε ε ε ε ± ± = − − + Γ − Γ − Γ − Γ − Γ + Γ −  ′′ ′ ′  ′′= − + + +     (1.3.25) and ( )( ) ( )( )( ) ( )( )( ) ( )( )( ) ( )( )( ) ( )( )( ) ( ) ( )( )( ) ( ) ( ) ( ) ( ) ( )( ) ( ) ( ) 1 1 2 22 22,1 22 21 ,2,2 23 1 23 22 ,1 2 log 2 log d cot 2 2cot . d 2 R g g A Br r B B B r A B ε ε ε ε ε εε ε εε ε ε ε ε ε εε ε ε ε ε ε ε ε ε ε ε ε ε θ θ θ ± ± = − − + Γ − Γ Γ − Γ + Γ −  ′′   = − − + − − +          (1.3.26) Weak distributional limit in ( )3D′  of the RHS of the Equation (1.3.18), i.e. ( )0lim vw Tε μ ε→− is calculated in our papers [18] [19], see also Appendix B. Remark 1.3.8. It turns out that the distributional Schwarzschild metric (1.3.22) has a gravitational singularity with compact support at origin { }0r = [6]-[11] and at Schwarzschild horizon { }2 2r m× =S [18] [19]. 1.3.2. Colombeau Extension of the Schwarzschild Spacetime in Isotropic Coordinates Let us consider now nonclassical spacetime furnished with a degenerate at horizon 4srρ = but nonsingular (at horizon) metric and known in physical literature as Schwarzschild spacetime in isotropic coordinates [24]: ( ) 2 4 2 2 2 2 2 2 21 4d d 1 d d sin d . 1 4 4 s s s r rs c t r ρ ρ ρ θ θ φ ρ ρ  −    = − + + + +     +    (1.3.27) Nonsingular metric (1.3.27) is obtained by the coordinate transformation: ( )21 4sr rρ ρ= + , between the Schwarzschild radial coordinate r and the isotropic radial coordinate ρ . Under formal calculation one obtains [24]: 2 8 , 16 t s t s r rρ ρ Γ = − (1.3.28) J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 371 Journal of High Energy Physics, Gravitation and Cosmology i.e. classical Levi-Civitá connection given by (1.3.28) of course unavaluble at horizon 4srρ = . However in physical literature under ubnormal calculation it was mistakenly pointed out that the Ricci tensor and the Ricci scalar vanish identically and Kretschman scalar is ( ) ( ) ( ) ( ) 13 6 2 12 3 4 . 4 abcd s abcd s r K R R r ρ ρ ρ ρ ρ × = = + (1.3.29) Remark 1.3.9. In order to avoid difficulty with the degeneracy of the metric (1.3.27) mentioned above, we consider now the corresponding distributional Colombeau metric which reads ( ) ( )( ) ( ) ( ) 2 2 4 2 2 2 2 2 2 2 2d d 1 d d sin d ,s c t ε ε ε ρ ρ ε ρ ρ ρ θ θ φ ρρ ρ − +    = − + + + +   +   (1.3.30) where ( ]0,1ε ∈ . Definition 1.3.2. Distributional Schwarzschild geometry in isotropic coordinates which is Colombeau extension of the classical spacetime (1.3.27), given by Colombeau generalized fundamental tensor (1.3.30). Colombeau generalized metric (1.3.30) nondegenerate at horizon in Colombeau sence and distributional Levi-Civitá connection now available on the whole distributional Schwarzschild spacetime in isotropic coordinates. Notice that generalized metric (1.3.30) has the form given by Equation (A.1) (see Appendix A) with ( ) ( )( )( ) ( ) ( ) ( ) ( ) ( ) ( ) ( )( )( ) 2 22 4 2 22 1 , 1 , 0, 0 Thus . A B D C A B ε ε ε ε ε ε ε ρ ρ ρ ε ρ ρ ρρ ρ ρ ρ ρ ρ ρ ρ ρ ε ρ ρ ρ − − = − + +   = + = =    ∆ = = − + + (1.3.31) From Equation (A.2) (see Apendix A2) and Equation (1.3.31) in the limit ( ) 0ε ερ ρ− ≈  , we get ( )( ) ( ) ( ) ( ) ( )( ) ( ) ( ) ( ) ( ) ( )( ) ( ) ( ) ( ) 2 22 2 4 42 2 4 42 2 , , , , , , , . O O O O O ε ε ε ε μν ε μν ε ε ε ρσμν ε ρσμν ε ε ε ε ρ ε ρ ε ρ ρ ε ρ ε ρ ε ρ ε ρ ρ ρ ε ρ ε ρ ε ρ ε ρ ρ ρ ε     ≈ −   − +        ≈ +   − +        ≈ +   − +          R R R R R (1.3.32) Compare the equation ( )( ) ( ) ( ) 222 2, O ε ρ ε ρ ε ρ ρ ε −  − − + R with Equation (1.2.12). Remark 1.3.10. Notice that in contrast with result of naive formal calculation mentioned above (see Equation (1.3.29)) we get: J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 372 Journal of High Energy Physics, Gravitation and Cosmology (i) ( ) ( )( ) ( )3, ,ρσμν ρσμν ερ ε ρ ε ∈ R R G (ii) ( ) ( )( ) ( ) ( )3 3, , \ ,Cμν ε ρν ερ ε ρ ε ∞∈  R R G (iii) ( ) ( )( ) ( ) ( )3 3, , \ .Cρσμν ε ρσμν ε ερ ε ρ ε ∞∈  R R G 1.4. On the Near Horizon Colombeau Approximation for the Classical Singular Schwarzschild Black Hole Geometry Let us perform the following coordinate transformation ( ) ( ]2, 8 2 , 0,1 4 tt r m r m m ε ε ε= = − + ∈ (1.4.1) to the classical singular Schwarzschild metric 1 2 2 2 2 22 2d 1 d 1 d dm ms t r r r r −    = − − + − + Ω        (1.4.2) we get 1 22 2 2 2 2 2 2 2 2 2 2 2d 1 d 1 d 4 1 d .16 16 16 r r rs r t r m m m m ε ε ε ε ε −       = − + + + + + Ω            (1.4.3) In Equation (1.4.2), m is the central mass, 2 2 2 2d d sin dθ θ φΩ = + and 1G c= = . Taking the limit m →∞ , the spherical horizon becomes planar and Equation (1.4.3) leads to the Colombeau type metric ( ) ( ){ } ( )2 2 2 2 2 2d d d 4 ds r t r mε ε εε ε ε= − + + Ω (1.4.4) which is distributional Rindler's spacetime if we neglect the angular contribution. The condition m →∞ is equivalent to the "near horizon approximation" for the exterior geometry of a black hole: for ( )2 2r m r m≈ > the line element (1.4.2) appears, indeed, as 2 2 2 2 22 2d d d 4 d . 2 2 r m ms t r m m r m − = − + + Ω − (1.4.5) By using simple coordinate transformations it could be shown that (1.4.5) again becomes the distributional Rindler metric when we take , constθ φ = or θ∆ and φ∆ are negligible. We stress that the condition 2r m≈ only is not enough to obtain Rindler's spacetime which has no spherical symmetry as Schwarzschild. Remark 1.4.1. At this stage of consideration, it is already clear that near horizon Schwarzschild black hole geometry has a gravitational singularity at horizon. Notice that in classical literature (see, for example, [24]-[36]) near horizon Schwarzschild black hole geometry were mistakenly accepted as regular with the Ricci tensor and the Ricci scalar vanish identically. 1.5. Colombeau Distributional Semi-Riemannian Geometry. Preliminaries 1.5.1. The Ring of Colombeau Generalized Numbers  Designation 1.5.1. We denote by  the ring of real, Colombeau generalized J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 373 Journal of High Energy Physics, Gravitation and Cosmology numbers. Recall that [2] [3] by definition ( ) ( )/=   E N where ( ) ( ) ( ) ( ) ( )( )( ){ } ( ) ( ) ( ) ( ) ( )( )( ){ } 0,1 0 0 0,1 0 0 0,1 , = 0,1 . a a x a x x a x ε εε ε εε ε ε ε ε ε ε ε ε − + +  = ∈ ∃ ∈ ∃ ∈ ∀ ≤ ≤   ∈ ∀ ∈ ∃ ∈ ∀ ≤ ≤         E N (1.5.0) Designation 1.5.2. In the sequel we denote by: [ ]ΩE , where Ω an open subset of n , the algebra of all the sequences ( )( ) ( ]0,1u xε ε∈ (for short, ( )( )u xε ε ) of smooth functions ( ) ( )u x Cε ∞∈ Ω . [ ]M ΩE is the differential subalgebra of the elements ( )( ) [ ]u xε ε ∈ ΩE such that for all K Ω , for all nα ∈ there exists N ∈ with the following property: ( ) ( )sup Nx K u x Oα ε ε −∈ ∂ = as 0ε → . ( )ΩN the differential subalgebra of the elements ( )( ) [ ]u xε ε ∈ ΩE such that for all K Ω , for all nα ∈ and q∈ the following property holds: ( ) ( )sup qx K u x Oα ε ε∈ ∂ = as 0ε → . Definition 1.5.1. The elements of [ ]M ΩE and ( )ΩN are called moderate and negligible, respectively.The factor algebra ( ) [ ] ( )/MΩ = Ω ΩG E N (1.5.1) is the algebra of Colombeau generalized functions on Ω . Remark 1.5.0. Note that: (i) there exists natural embedding :r →    such that for all r∈ , ( ):r r rε ε→ , r rε = , for all [ )1,0ε ∈ , (ii) the ring  can be endowed with the structure of a partially ordered ring: for , ∈ r s , ≤ r s if and only if there are representatives ( )rε ε and ( )sε ε with r sε ε≤ for all [ )1,0ε ∈ . Definition 1.5.2. (i) Let δ ∈  . We say that δ is infinite small Colombeau generalized number and abbraviate 0δ ≈    or 0δ ≈  , if there exists representative ( ) ( ], 0,1ε εδ ε ∈ and some q∈ such that ( )qOεδ ε= , as 0ε → . We abbraviate α β≈  iff 0α β− ≈  . (ii) We say that ∆∈  is infinite large Colombeau generalized number and abbraviate ∆ ≈ ∞  if 1 0−∆ ≈  . (iii) We say that ∈ r is finite Colombeau generalized number and abbraviate finr if there are 1 2,r r ∈ such that 1 2r r≤ ≤ r . Definition 1.5.3. Let 1,MΩ and 2,MΩ be a set ( ) ( ] ( ){ } ( ) ( ] ( ){ } 0,1 1, 0,1 2, , , as 0 , , , as 0 . N M N M x N x O x N x O ε εε ε εε ε ε ε ε −Ω = ∈Ω ∃ ∈ = → Ω = ∈Ω ∃ ∈ = →   correspondingly. We introduce equivalence relation given by ( ) ( ) ( )~ , , as 0,qx y q x y Oε ε ε εε ε ε ε⇔ ∀ ∈ − = → J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 374 Journal of High Energy Physics, Gravitation and Cosmology and denote by ( )1, 2, ~M MΩ− Ω Ω  the set of generalized points. Moreover, if ( )xε ε   is the class of ( )xε ε in Ω then the set of compactly generalized points is ( ) ( ) ( ) ( ]( )[ ]{ }0 0, .c x x K K x Kε εε η η ε ε η Ω = = ∈Ω ∃ Ω ∃ > ∀ ∈ ∈    Note that if the cΩ -property holds for one representative of cx∈Ω then it holds for every representative. Also, for Ω =  we have that the factor ~M is the usual algebra of real generalized numbers. Definition 1.5.4. We denote by 1, ~IL MΩ Ω  and 2, ~ISM MΩ Ω  the set of inite large and infite small generalized points correspondingly. It is clear that the generalized point value of ( )u x at ISMx∈Ω is ( ) ( )( ) ( )u x u xε ε ε= + ΩN . Definition 1.5.5. Let δ ∈  be infinite small Colombeau generalized number with representative ( ) ( ], 0,1ε εδ δ ε′ = ∈ . We introduce a norm δ ′ of such representative by formula ( ]0,1sup εεδ δ∈′ = . 1.5.2. A Real Colombeau Vector Bundle Definition 1.5.6. A real vector bundle consists of: 1) Topological spaces X (base space) and E (total space) 2) A continuous surjection : E Xπ → (bundle projection) 3) For every x in X, the structure of a finite-dimensional vector space over Colombeau ring  on the fiber { }( )1 xπ − where the following compatibility condition is satisfied: for every point in X, there is an open neighborhood U, a natural number k, and a homeomorphism ( )1: kU Uφ π −× → such that for all x U∈ , ( )( ),x v xπ φ = for all vectors v in k , and the map ( ),v x vφ is a linear isomorphism between the vector spaces k and { }( )1 xπ − . The open neighborhood U together with the homeomorphism φ is called a local trivialization of the Colombeau vector bundle. The local trivialization shows that locally the map π "looks like" the projection of kU ×  on U. The Cartesian product kX ×  , equipped with the projection kX X× → , is called the trivial bundle of rank k over X. 1.5.3. The Algebra of Colombeau Generalized Functions The basic idea of Colombeau's theory of generalized functions is a regularization by sequences (nets) of smooth functions and the use of asymptotic estimates in terms of a regularization parameter ( ]0,1ε ∈ . Let ( ) (0,1]uε ε∈ with ( )u C Mε ∞∈ for all ( ]0,1ε ∈ (M a separable, smooth orientable Hausdorff manifold of dimension n).The algebra of Colombeau generalized functions on M is defined as the quotient ( ) ( ) ( )/MM M M=G E N (1.5.2) of the space ( )M ME of sequences of moderate growth modulo the space ( )MN of negligible sequences. More precisely the notions of moderateness J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 375 Journal of High Energy Physics, Gravitation and Cosmology resp. negligibility are defined by the following asymptotic estimates ( ( )M   X or ( )MX denoting the space of smooth vector fields on M). ( ) ( ) ( )( ] ( )( )( ){ ( ) ( )( ) ( ) ( ) ( ) ( ) ( ] ( )( ){ ( ) ( )( ) ( ) ( ) 1 1 0,1 0 1 0,1 0 1 , , sup , , , , sup . n n M n k p K q l k p K M u C M K M k n M M L L u p O M u M K M k q l M M L L u p O ε ε ξ ξ ε ε ε ξ ξ ε ξ ξ ε ξ ξ ε δ ∞ − ∈ ∈ = ∈ ∀ ⊂⊂ ∀ ∈ ∃ ∈  ∀ ∈ ∀ ∈ ≤   = ∈ ∀ ⊂⊂ ∀ ∈  ∀ ∈ ∀ ∈ ≤            E X X N X X    (1.5.3) Elements of ( )G M are denoted by ( ) ( ) ( ) ( ).u u u u Mε ε εε ε ε   = = = +   cl N (1.5.4) With componentwise operations ( )G M is a fine sheaf of differential algebras with respect to the Lie derivative defined by ( ) ( ): .L u L u L uξ ξ ε ξ εε ε   = =   cl (1.5.5) The spaces of moderate resp. negligible sequences and hence the algebra itself may be characterized locally, i.e., u ∈ ( )G M iff ( )( )u G Vα α αψ ψ∈ for all charts ( ),Vα αψ , where on the open set ( ) nVα αψ ⊂  in the respective estimates Lie derivatives are replaced by partial derivatives. Smooth functions are embedded into ( )G M simply by the "constant" embedding σ , i.e., ( ) ( ):f cl f εσ  =   , hence ( )C M ∞ is a faithful subalgebra of ( )G M . On open sets of n compactly supported distributions are embedded into G via convolution with a mollifier ( )nSρ ∈  with unit integral satisfying ( ) d 0x x xαρ =∫ for all 1α ≥ ; more precisely setting ( ) ( ) ( )1 nx xερ ε ρ ε= we have ( ) ( ):w cl w ε ει ρ = ∗  . In case ( )supp w is not compact one uses a sheaf-theoretical construction. 1.5.4. Colombeau Tangent Vector Let ( )( ) ( )( ) ( )nf cl f f Gε εε ε   = = ∈    x x , where ( ) ( ): , 0,1nfε ε→ ∈ x is a differentiable function and let v be a vector in n . We define the Colombeau directional derivative in the v direction at a point nx∈ by ( )( )( ) ( )( ) ( ) ( ) 10 d . d Col n i it i D f D f D f f f t t x ε εε ε ε ε ε ε==      = =         ∂   = + =       ∂          ∑ v v vx x x x v v (1.5.6) The Colombeau tangent vector at the point x may then be defined as ( ) ( )( )( ) ( )( ) .Col f f D fε εε ε   = =   vv v x x (1.5.7) Let ( )( ) ( ) ( )( ) ( ),n nf f G g g Gε εε ε   = ∈ = ∈    x x , where ( ), : , 0,1nf gε ε ε→ ∈  be differentiable functions, let ,v w be tangent vectors in n at nx∈ and let ,a b∈  . Then J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 376 Journal of High Energy Physics, Gravitation and Cosmology 1) ( ) ( ) ( ) ( )( ) ( )( ) ( )( ) ( ) ( ); Col Col Col a b f a b f a f b f a f b f ε ε ε εε ε  ⋅ + ⋅ = ⋅ + ⋅      = +    = + v w v w v w v w 2) ( ) ( ) ( )( ) ( )( ) ( )( ) ( ) ( ); Col Col Col a f b g a f b g a f b g a f b g ε εε ε ε εε ε    ⋅ + ⋅ = ⋅ + ⋅       = ⋅ + ⋅    = ⋅ + ⋅ v v v v v v 3) ( ) ( )( ) ( ) ( )( ) ( )( ) ( )( ) ( ) ( ) ( ) . Col Col Col f g f g f g g f f g g f ε ε ε ε ε ε εε ε εε  ⋅ = ⋅        = ⋅ + ⋅       = ⋅ + ⋅ v v x v x v v v 1.5.5. Colombeau Tangent Vector to Differentiable Manifold M Let M be a differentiable manifold and let ( )MG be the algebra of real-valued Colombeau generalized functions on M. Then the tangent vector to M at a point x in the manifold is given by the derivation ( ):D M → v G which shall be linear-i.e., for any ( ) ( ) ( ),f f g g Mε εε ε   = = ∈    G and ,a b∈  we have 1) ( ) ( ) ( )( ) ( )( ) ( )( ) ( ) ( ). Col Col Col D a f b g D a f b g a D f b D g a D f b D g ε εε ε ε εε ε    ⋅ + ⋅ = ⋅ + ⋅       = ⋅ + ⋅    = ⋅ + ⋅ v v v v v v Note that the derivation will by definition have the Leibniz property 2) ( ) ( )( ) ( )( ) ( )( ) ( )( ) ( )( ) ( ) ( ). Col Col Col D f g D f g D f g x f x D g D f g f D g ε ε ε ε ε ε εε εε ε  ⋅ = ⋅        = ⋅ + ⋅       = ⋅ + ⋅ v v v v v v 1.5.6. Colombeau Vector Fields on Distributional Manifolds Colombeau vector field   X (denoted often by X ) on a manifold M is a linear map   X : ( ) ( )M M→G G such that for all ( ),f g M∈G : ( ) ( ) ( ) .f g f f g f g⋅ = ⋅ ⋅ + ⋅         X X X (1.5.8) 1.5.7. Colombeau Tangent Space Suppose now that M is a C∞ manifold. A real-valued Colombeau generalized function ( ) ( ]: , 0,1f Mε ε ε→ ∈ is said to belong to ( )MG if and only if for every coordinate chart : nUφ →  , the map [ ]1 : nf Uε φ φ− ⊆ →   is infinitely differentiable. Note that ( )MG is a real associative algebra with respect to the pointwise product and sum of Colombeau generalized functions. J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 377 Journal of High Energy Physics, Gravitation and Cosmology Pick a point x M∈ . A derivation at x is defined as a linear map ( ):D M → G that satisfies the Leibniz identity: ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ), : ,f f g g M D f g D f g x f x D gε εε ε   = = ∈ ⋅ = ⋅ + ⋅    G which is modeled on the product rule of calculus. If we define addition and scalar multiplication on the set of derivations at x by ( )( ) ( ) ( )1 2 1 2D D f f D f D f+ = ⋅ + and ( )( ) ( ) ,D f f D fλ λ⋅ = ⋅ ⋅ where λ∈  , then we obtain a real vector space over  , which we define as the Colombeau tangent space ColxT M of M at x. 1.5.8. Colombeau Dual Space Given any vector space V  over Colombeau algebra  , the (algebraic) Colombeau dual space V ∗  (also denoted for a short by V ∗ ) is defined as the set of all linear maps :Vφ →     . Since linear maps are vector space homomorphisms, the Colombeau dual space is also sometimes denoted by ( ),Hom V  . The Colombeau dual space V ∗ itself becomes a vector space over  when equipped with an addition and scalar multiplication satisfying: (i) ( )( ) ( ) ( )x x xφ ψ φ ψ+ = + and (ii) ( ) ( )x xαφ φ α= , where ( ) ( ), ,x x Vφ ψ α∗∈ ∈     . 1.5.9. Colombeau Cotangent Space Let M be a smooth manifold and let x be a point in M. Let xT M be Colombeau tangent space at x. Then Colombeau cotangent space at x is defined as the Colombeau dual space of ( ):x x xT M T M T M ∗∗ =  . Suppose now that M is a C∞ manifold and let ( )f M∈G . The differential of f at a point x is the map: ( ) ( )x x xdf X X f= where xX is a tangent vector at x, thought of as a derivation. In either case, xdf is a linear map on xT M and hence it is a tangent covector at x. We can then define the differential map ( ): xd M T M∗→G at a point x as the map which sends f to xdf . Properties of the differential map include: (i) ( )d af bg adf bdg+ = + for ,a b∈  , (ii) ( ) ( ) ( )x xd fg f x dg g x df= + . Let : M Nεφ → for any ( ]0,1ε ∈ be a smooth map of smooth manifolds. Given some x M∈ , the Colombeau differential of ( )ε εφ at x is a linear map ( ) ( )( ), :x x xd T M T Nε εε φεφ → from Colombeau tangent space of M at x to Colombeau tangent space of N at ( )( )xε εφ . The application of ( ),xd ε εφ to a tangent vector X is called the pushforward of X by ( )ε εφ . 1.5.10. ( )MG -Module of Generalized Sections ( )M EG , of a Vector Bundle E M→ The ( )MG -module of generalized sections ( ),M EG of a vector bundle E M→ and in particular the space of generalized tensor fields ( )rs MG is defined along the same lines using analogous asymptotic estimates with respect J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 378 Journal of High Energy Physics, Gravitation and Cosmology to the norm induced by any Riemannian metric on the respective fibers. We denote generalized sections by ( ) ( ) ( ),S s s N M Eε εε ε = = + cl . Alternatively we may describe a section ( ),S M E∈G by a family ( ) ( )( ) 1 Ni i S Sα αα == , where Sα is called the local expression of S with its components ( )( )1i iS S Vα α α α αψ ψ−Ψ ∈   G ( ( ),Vα α αΨ a vector bundle atlas and 1, ,i N=  , with N denoting the dimension of the fibers) satisfying ( ) ( ) ( )( ) ( )( )1 1ii jjS x x S xα αβ β α β β αψ ψ ψ ψ ψ− −=   for all ( )x V V∈  , where αβψ denotes the transition functions of the bundle. Remark 1.5.1. Smooth sections of E M→ again may be embedded as constant nets, i.e., ( ) ( ): .s s s ε Θ →  cl Since ( )C M∞ is a subring of ( ) ( ), ,M M EG G also may be viewed as ( )C M∞ -module and the two respective module structures are compatible with respect to the embeddings. Moreover we have the following algebraic characterization of the space of generalized sections ( ) ( ) ( ), , ,M E M M E= ⊗ΓG G (1.5.9) where ( ),M EΓ denotes the space of smooth sections and the tensor product is taken over the module ( )C M∞ . Generalized tensor fields may be viewed likewise as C∞ -resp. G -multilinear mappings, i.e., as ( )C M∞ -resp. ( )MG -modules we have ( ) ( ) ( ) ( ) ( )( ) ( ) ( ) ( ) ( ) ( )( )0 11 0 , ; , , ; . r sr s C M r sr s M M L X M X M M M L M M M ∞ ∗≅ ≅   G G G G G G G (1.5.10) Here ( )X M resp. ( )X M∗ denotes the space of smooth vector resp. covector fields on M. 1.5.11. Generalized Pseudo-Riemannian Manifold A generalized ( )0,2 tensor field ( )02g M∈G is called a generalized Pseudo-Riemannian metric if it has a representative ( )gε ε satisfying (i) gε is a smooth Pseudo-Riemannian metric for all ( ]0,1ε ∈ , and (ii) ( )( )det g pε ε is strictly nonzero on compact sets, i.e., ( ) ( ) ( )inf det .mp KK K X m m N g pε ε∈ ∀ ⊂⊂ ∃ ∈ ≥  We call a separable, smooth Hausdorff manifold M furnished with a generalized pseudo-Riemannian metric ( )g gε ε   cl generalized pseudo-Riemannian manifold or generalized spacetime and denote it by ( ),M g . The action of the metric on a pair { }1 2,H H of generalized vector fields will be denoted by ( )1 2,g H H or 1 2,H H [20] [21]. A generalized metric g is non-degenerate in the following sense: ( ) ( )( ) ( )1 11 0 2 2 0 1 2 1, 0 0.H M H H M g H H H ∈ ∧∀ ∈ = =   G G (1.5.11) Note that condition (ii) above is precisely equivalent to invertibility of J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 379 Journal of High Energy Physics, Gravitation and Cosmology ( )det g in the generalized sense. The inverse metric ( )1 1g gε ε − −    cl is a well defined element of ( ) 2 0 MG , depending exclusively on g (i.e., independent of the particular representative ( )gε ε ). Moreover if kg g≈ , where g is a classical kC -pseudo-Riemannian metric then 1 1kg g − −≈ . From now on we denote the inverse metric by abg , its components by ijg and the components of a representative by ( )ijgε ε . Also we shall denote the generalized metric abg by ( ) 2 2ds dsε ε  =  cl and its representative by ( ) ( )( )2 i jijds g dx dxε ε εε= and use summation convention. Notice that g induces a ( )MG -linear isomorphism ( ) ( )1 00 1M M→G G by ( ),gΦ Φ ⋅ , which as in the classical context extends naturally to generalized tensor fields of all types. 1.5.12. Colombeau Isometric Embedding Let ( ),M g and ( ),N h be generalized pseudo-Riemannian manifolds. An isometric Colombeau embedding is a Colombeau generalized function ( )fε ε : M N→ which preserves the metric in the sense that ( )gε ε is equal to the pullback of ( )hε ε by ( )fε ε , i.e. ( ) ( )g f hε ε εε ε ∗= . Explicitly, for any two tangent vectors ( ), xT M∈v w we have ( )( ) ( ) ( )( )( ), ,g h df dfε ε ε εε ε=v w v w . 1.5.13. Generalized Connection on a Generalized Pseudo-Riemannian Manifold Generalized connection 1 2H D H on a manifold M is a map ( ) ( ) ( )1 1 10 0 0M M M× →G G G satisfying: (D1) ( ) 1 2H D H is  -linear in 2H . (D2) ( ) 1 2H D H is ( )MG -linear in 1H . (D3) ( ) ( ) ( )1 12 2 1 2H HD H D H H H⋅ = ⋅ +f f f for all ( )M∈f G . Let ( ),Vα αψ be a chart on M with coordinates xi. The generalized Christoffel symbols for this chart are given by the ( ) 3dim M   generalized functions ( )kij VαΓ ∈G defined by ( ) .i kj ij k k D∂ ∂ = Γ ∂∑ (1.5.12) Theorem. [21]. (I) Let ( ),M g be a generalized pseudo-Riemannian manifold. Then there exists a unique generalized connection ( ) 1 2H D H such that (D4) [ ] ( ) ( ) 1 21 2 2 1 , H HH H D H D H= − and (D5) ( ) ( ) 1 11 2 3 2 3 2 3 , , ,H HH H H D H H H D H= + hold for all 1 2 3, ,H H H in ( )10 MG . ( ) 1 2H D H is called generalized Levi-Civita connection of M and characterized by the so-called Koszul formula ( ) [ ] [ ] [ ] 1 2 3 1 2 3 2 3 1 3 1 2 1 2 3 2 3 1 3 1 2 2 , , , , , , , , , , . HD H H H H H H H H H H H H H H H H H H H H = + − − + + (1.5.13) J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 380 Journal of High Energy Physics, Gravitation and Cosmology (II) On every chart ( ),Vα αψ we have for the generalized Levi-Civita connection ( ) 1 2H D H of ( ),M g and any vector field ( )10H M∈G ( ) .i k j k j j ij ki HD H H x∂  ∂ ∂ = + Γ ∂ ∂  (1.5.14) The generalized Christoffel symbols are given by 1 , 2 jm ijk km im ij i j m g ggg x x x ∂ ∂ ∂ Γ = + + ∂ ∂ ∂  (1.5.15) or by using representative ( )( ) ( )( ) ( ) ( ) ( )1 . 2 jm ijimk km ij i j m g gg g x x xε ε εε ε ε εε ε ε  ∂ ∂   ∂  Γ = + +          ∂ ∂ ∂       (1.5.16) We define now the action of a classical (smooth) connection D on generalized vector fields ( )1H ε εξ =  cl and ( )2H ε εη =  cl by ( ) ( )( )1 2HD H D εξ ε εη =  cl (III) Let ( ),M g be a generalized pseudo-Riemannian manifold. (i) If ( )ab abg g= Θ where abg is a classical smooth metric then we have,in any chart, ( )i ijk jkΓ = Θ Γ (with ijkΓ denoting the Christoffel Symbols of abg ). Hence for all ( )10H M∈G : ( ) ( ) 1 12 2 .H HD H D H= (ii) If ab abg g∞≈ , where abg a classical smooth metric, ( )11 2 0,H H M∈G and ( )1H X Mξ∞≈ ∈  , ( )12 0H D Mη ′≈ ∈ or ( )11 0H D Mξ ′≈ ∈ , ( )2H X Mη∞≈ ∈  , then ( ) ( )1 2HD H Dξ η≈ . (iii) Let ab k abg g≈ , where abg a classical kC -metric, then, in any chart, 1 i i jk k jk−Γ ≈ Γ . If in addition, ( )11 2 0,H H M∈G , ( )11 1 ,kkH M TMξ −−≈ ∈Γ and ( )2 ,kkH M TMη≈ ∈Γ then ( ) ( ) 1 2 .H kD H Dξ η≈ 1.5.14. The Generalized Riemannian Curvature Tensor Let ( ),M g be a generalized pseudo-Riemannian manifold with a generalized Levi-Civita connection D . (i) The generalized Riemannian curvature tensor ( )13dabcR M∈G is defined by [ ]1 2 1 21 2, 3 3 3, , .H H H HH HR H D H D D H −   (1.5.17) (ii) The generalized Ricci curvature tensor is defined by .cab cabR R (1.5.18) (iii) The generalized Ricci scalar is defined by .aaR R (1.5.19) (iv) Finally we define the generalized Einstein tensor by 1 . 2ab ab ab G R R g− (1.5.20) J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 381 Journal of High Energy Physics, Gravitation and Cosmology 1.6. Super Generalized Functions 1.6.1. The Nonsmooth Regularization via Horizon Examining now the Schwarzschild metric (1.3.1) (note that the origin is now excluded from our considerations, the space we are working on is { }3 3 \ 0+   ) in a neighborhood of the horizon, we see that, whereas ( )h r is smooth, ( )1h r− is not even 1locL . Thus, regularizing the Schwarzschild metric amounts to embedding 1h− into ( )3+G , for example as that given in paper [17], one obtains Colombeau generalized metric ( ) ( ) ( )( ) ( ) ( ) 2 2 1 2 2 2 1 1 d d , d d , 1, 1 2 2 11 2 . 2 s h r t h r r r h r h m r r m m r m ε ε ε ε ε ε ε ε ρ ι − − − = − + Ω   = = − − ∗  −     = − − ⋅   −   vp vp (1.6.1) Here ( ) ( )3 3r rερ ε ρ ε− −= and ( )rρ is a mollifier. Obviously, (1.6.1) is degenerate at 2r m= , because ( )h r is zero at the horizon. Due to the degeneracy of (33), the Levi-Civitá connection is not available. In order avoid this difficultness in literature the following generalized pseudo-connection ikjΓ was considered ( )( ) ( )3i ikj kj εε + Γ = Γ ∈  cl G [17]: ( )( ) ( ) ( ) ( ) ( )( ), , ,1 .2i imkj mk j mj k kj mg g g gε ε ε εε εε ι ι ι ι Γ = + −  (1.6.2) Obviously the generalized pseudo-connection ikjΓ coincides with the classical Levi-Civitá connection ikjΓ on { }3 \ 2r m+ = since ( )( )im img gε ει = , ( )( )im img gε ει = there. However the generalized pseudo-connection i kjΓ is not a true generalized Levi-Civitá connection on 3+ since ikjΓ does not respect the Colombeau generalized metric (1.6.1), i.e., ( )( ), 0ij kgε ει ≠ , e.g., ( )( ) ( )( )100,1 1g h h hε ε εει − ′= − . Compatibility with the metric ( )( )gε ει is a priori ruled out by the following statement: there exists no connection whatsoever under which ( )( )gε ει would be a parallel tensor. However in a weak sense, the connection (1.6.2) is metric compatible: ( )( ), 0ij kgε ει ≈ . In additional [17]: ( )( ) 0,ijR εε ≈ (1.6.3) where ( )( )ijR εε is a Ricci tensor corresponding to generalized pseudo-connection (1.6.2), and therefore Colombeau object ( )( )ijR εε viewed as a classical distribution on { }3 \ 0 gives { }30 on \ 0 .ijR =  (1.6.4) Remark 1.6.1. In paper [17] the equality (1.6.4) mistakenly considered as a proof that the metric singularity at the Schwarzschild horizon is only a coordinate singularity. Remark 1.6.2. Due to the degeneracy of any smooth regularization of the metric (1.3.1) no canonical Levi-Civitá connection could be defined. In order to avoid such difficultnes in our papers [18] [19] the nonsmooth regularization via horizon is considered, see Section 2 below. However such regularization J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 382 Journal of High Energy Physics, Gravitation and Cosmology demands appropriate extension of the Colombeau algebra ( )MG . 1.6.2. The Super Generalized Functions The basic idea of the theory of super generalized functions is regularization by sequences (nets) of appropriate classes of non smooth and discontinuous functions or classical distributions and the use of asymptotic estimates in terms of a regularization parameter ( ]0,1ε ∈ . Let ( ) ( ]0,1uε ε∈ with ( )u D Mε ′∈ for all ( ]0,1ε ∈ (M a separable, smooth orientable Hausdorff manifold of dimension n). Such sequences are called super generalized functions. The algebra of super generalized functions on M is defined as the quotient ( ) ( ) ( )/MM M M′ ′=SG SE SN (1.6.5) of the space ( )M M′SE of sequences of moderate growth modulo the space ( )MN of negligible sequences. More precisely the notions of moderateness resp. negligibility are defined by the following asymptotic estimates ( ( )M   X or ( )MX denoting the space of smooth vector fields on M) [18] [19]: ( ) ( ) ( )( )( ] ( ) ( )( ){ ( ) ( )( ) ( )( ) ( ) ( ) } ( ) ( ) ( )( )( ] ( ) ( )( ){ ( ) ( )( ) ( )( ) ( ) ( ) } 1 1 0,1 0 1 0 0,1 0 1 0 = , , , = , , , . n n M n k f q k f M u D M K M k n M M f C K L L u f O M u D M K M k q n M M f C K L L u f O ε ε ξ ξ ε ε ε ξ ξ ε ξ ξ ε ξ ξ ε ∞ − ∞ ′ ′∈ ∀ ⊂⊂ ∀ ∈ ∃ ∈  ∀ ∈ ∀ ∈ ∀ ∈ ≤  ′ ′∈ ∀ ⊂⊂ ∀ ∈ ∃ ∈  ∀ ∈ ∀ ∈ ∀ ∈ ≤              SE X X SN X X (1.6.6) Here , 1, 2, , k wL k nξ =  denoting the weak Lie derivative in L.Schwartz sense and where Landau symbol ( )( )fa Oε φ ε= appears, having the following meaning: ( ) ( ]( ) ( ) ( )0 0 00 0,1 .f f ff C C a Cεε ε ε ε ε φ ε ∀ ∃ > ∃ ∈ ∀ < ≤  We denote by S the ring of real, Colombeau super generalized numbers. ( ) ( )/=   S SE SN , where ( ) ( ) ( ] ( ] ( ) ( ]( ){ ( )( ) } ( ) ( ) ( ] ( ] ( ) ( )( ){ ( )( ) } 0,1 0,1 , 0 0, 0 0 , 0,1 0,1 , 0 0, 0 0 , , 0,1 , , , 0,1 . a b a b x a b x x a b x ε δ ε δ ε δ ε δ ε δ ε ε δ ε ε δ δ ε δ ε δ ε ε δ δ ε δ × + − − × + = ∈ ∃ ∈ ∃ ∈  ∀ ≤ ∀ ≤ ≤  = ∈ ∀ ∈ ∃ ∈  ∀ ≤ ∀ ≤ ≤         SE SN (1.6.7) Let ( ) ( ], , 0,1uε δ ε δ∈ with ( ),u C Mε δ ∞∈ for all ( ], 0,1ε δ ∈ (M a separable, smooth orientable Hausdorff manifold of dimension n). By using canonical imbeding ( ) ( )D M M′ → G the algebra ( )MSG of Colombeau super generalized functions on M is defined also in the equivalent form as the quotient ( ) ( ) ( )/MM M M=SG SE SN (1.6.8) of the space ( )M MSE of sequences of moderate growth modulo the space J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 383 Journal of High Energy Physics, Gravitation and Cosmology ( )MSN of negligible sequences. More precisely the notions of moderateness resp. negligibility are defined by the following asymptotic estimates ( ( )MX    or ( )MX denoting the space of smooth vector fields on M). ( ) ( )( ] ( ] ( ) ( )( ){ ( ) ( )( ) ( ) ( ) ( ) ( ) ( ] ( ] ( ) ( ){ ( ) ( )( ) ( ) ( ) 1 1 0,1 0,1 , , 0 1 , 0,1 0,1 , 0, 1 3 5 ( ) , , , sup , , , , , sup . n n M n m k p K q l k b p K M u C M K M k n m M M L L u p O M u M K M k q l M M L L u p O ε δ ε δ ξ ξ ε δ ε δ ε δ ξ ξ ξ ξ ε δ ξ ξ ε δ ×∞ − − ∈ × ∈ = ∈ ∀ ⊂⊂ ∀ ∈ ∃ ∈  ∀ ∈ ∀ ∈ ≤    = ∈ ∀ ⊂⊂ ∀ ∈  ∀ ∈ ∀ ∈ ≤               SE X X SN X X (1.6.9) The ( )MSG -module of super generalized sections ( ),M ESG of a vector bundle E M→ and in particular the space of super generalized tensor fields ( )rs MSG is defined along the same lines using analogous asymptotic estimates with respect to the norm induced by any Riemannian metric on the respective fibers. We denote super generalized sections by ( ) ( ) ( ), ,, , ,S s s M Eε δ ε δε δ ε δ = = + cl SN . Alternatively we may describe a section ( ),S M E∈SG by a family ( ) ( )( ) 1 Ni i S Sα αα == , where Sα is called the local expression of S with its components ( )( )1i iS S Vα α α α αψ ψ−Ψ ∈   SG ( ( ),Vα α αΨ a vector bundle atlas and 1, ,i N=  , with N denoting the dimension of the fibers) satisfying ( ) ( ) ( )( ) ( )( )1 1ii jjS x x S xα αβ β α β β αψ ψ ψ ψ ψ− −=   for all ( )x V V∈  where αβψ denotes the transition functions of the bundle. Remark 1.6.3. Smooth sections of E M→ again may be embedded as constant nets, i.e., ( ) ( ) ,: .s s s ε δ Θ →  cl Since ( )C M∞ is a subring of ( ) ( ), ,M M ESG SG also may be viewed as ( )C M∞ -module and the two respective module structures are compatible with respect to the embeddings. Moreover we have the following algebraic characterization of the space of super generalized sections ( ) ( ) ( ), , ,M E M M E= ⊗ΓSG SG (1.6.10) where ( ),M EΓ denotes the space of smooth sections and the tensor product is taken over the module ( )C M∞ . Generalized tensor fields may be viewed likewise as C∞ -resp. SG -multilinear mappings, i.e., as ( )C M∞ -resp. ( )MSG -modules we have ( ) ( ) ( ) ( ) ( )( ) ( ) ( ) ( ) ( ) ( )( )0 11 0 , ; , , ; . r sr s C M r sr s M M L X M X M M M L M M M ∞ ∗≅ ≅   SG SG SG SG SG SG SG (1.6.11) Here ( )X M resp. ( )X M∗ denotes the space of smooth vector resp. J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 384 Journal of High Energy Physics, Gravitation and Cosmology covector fields on M. 1.6.3. Super Generalized Pseudo-Riemannian Manifold A super generalized ( )0,2 tensor field ( )02g M∈SG is called a super generalized Pseudo-Riemannian metric if it has a representative ( ), ,gε δ ε δ satisfying: (i) ,gε δ is a smooth Pseudo-Riemannian metric for all ( ], 0,1ε δ ∈ , and (ii) ( )( ), ,det g pε δ ε δ is strictly nonzero on compact sets, i.e., ( ) ( ) ( ) ( ),inf det .m lp KK K X m m N l l N g pε δ ε δ∈ ∀ ⊂⊂ ∃ ∈ ∃ ∈ ≥  We call a separable, smooth Hausdorff manifold M furnished with a super generalized pseudo-Riemannian metric ( ), ,g gε δ ε δ   cl super generalized pseudo-Riemannian manifold or super generalized spacetime and denote it by ( ),M g . The action of the metric on a pair { }1 2,H H of super generalized vector fields will be denoted by ( )1 2,g H H or 1 2,H H . A super generalized metric g is non-degenerate in the following sense: ( ) ( )( ) ( )1 11 0 2 2 0 1 2 1, 0 0.H M H H M g H H H ∈ ∧∀ ∈ = ⇒ =   SG SG (1.6.12) Note that condition (ii) above is precisely equivalent to invertibility of ( )det g in the super generalized sense. The inverse metric ( )1 1, ,g gε δ ε δ − −      cl is a well defined element of ( )20 MSG , depending exclusively on g (i.e., independent of the particular representative ( ), ,gε δ ε δ ). Moreover if kg g≈ , where g is a classical kC -pseudo-Riemannian metric then 1 1kg g − −≈ . From now on we denote the inverse metric by abg , its components by ijg and the components of a representative by ( ) , ijgε ε δ . Also we shall denote the super generalized metric abg by ( ) 2 2 , , ds dsε δ ε δ  =    cl and its representative by ( ) ( )( )2, , ,, i j ijds g dx dxε δ ε δ ε δε δ= and use summation convention.Notice that g induces a ( )MSG -linear isomorphism ( ) ( )1 00 1M M→SG SG by ( ),gΦ Φ ⋅ , which as in the classical context extends naturally to generalized tensor fields of all types. Let ( ),M g and ( ),N h be super generalized pseudo-Riemannian manifolds. An isometric Colombeau embedding is a Colombeau super generalized function ( ), , :f M Nε δ ε δ → which preserves the metric in the sense that ( ), ,gε δ ε δ is equal to the pullback of ( ), ,hε δ ε δ by ( ), ,fε δ ε δ , i.e. ( ) ( ), , ,, ,g f hε δ ε δ ε δε δ ε δ ∗= . Explicitly, for any two tangent vectors ( ), xT M∈v w we have ( )( ) ( ) ( )( )( ), , , ,, ,, ,g h df dfε δ ε δ ε δ ε δε δ ε δ=v w v w . 1.6.4. Super Generalized Connection on a Super Generalized Pseudo-Riemannian Manifold Super generalized connection 1 2H D H on a manifold M is a map ( ) ( ) ( )1 1 10 0 0M M M× →SG SG SG satisfying: (D1) ( ) 1 2H D H is S -linear in 2H . (D2) ( ) 1 2H D H is ( )MSG -linear in 1H . (D3) ( ) ( ) ( )1 12 2 1 2H HD H D H H H⋅ = ⋅ +f f f for all ( )M∈f SG . Let ( ),Vα αψ be a chart on M with coordinates ix . The super generalized J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 385 Journal of High Energy Physics, Gravitation and Cosmology Christoffel symbols for this chart are given by the ( ) 3dim M   super generalized functions ( )kij VαΓ ∈SG defined by ( ) .i kj ij k k D∂ ∂ = Γ ∂∑ (1.6.13) Theorem. (I) Let ( ),M g be a super generalized pseudo-Riemannian manifold. Then there exists a unique super generalized connection ( ) 1 2H D H such that (D4) [ ] ( ) ( ) 1 21 2 2 1 , H HH H D H D H= − and (D5) ( ) ( ) 1 11 2 3 2 3 2 3 , , ,H HH H H D H H H D H= + hold for all 1 2 3, ,H H H in ( )10 MSG . ( ) 1 2H D H is called super generalized Levi-Civita connection of M and characterized by the so-called Koszul formula ( ) [ ] [ ] [ ] 1 2 3 1 2 3 2 3 1 3 1 2 1 2 3 2 3 1 3 1 2 2 , , , , , , , , , , . HD H H H H H H H H H H H H H H H H H H H H = + − − + + (1.6.14) (II) On every chart ( ),Vα αψ we have for the super generalized Levi-Civita connection ( ) 1 2H D H of ( ),M g and any vector field ( )10H M∈SG ( ) .i k j k j j ij ki HD H H x∂  ∂ ∂ = + Γ ∂ ∂  (1.6.15) The super generalized Christoffel symbols are given by 1 , 2 jm ijk km im ij i j m g ggg x x x ∂ ∂ ∂ Γ = + + ∂ ∂ ∂  (1.6.16) or by using representative ( )( ) ( )( ) ( ) ( ) ( ) , , , , , ,1, , 2 ,, . jmk km ij i ijim j m g g x gg x x ε δ ε δ ε δ ε δ ε δ ε δ ε δ ε δ ε δε δ  ∂   Γ =       ∂  ∂ ∂  + +     ∂ ∂      (1.6.17) We define now the action of a classical (smooth) connection D on super generalized vector fields ( )1 , ,H ε δ ε δξ =  cl and ( )2 , ,H ε δ ε δη =  cl by ( ) ( )( )1 ,2 , ,HD H D ε δξ ε δ ε δη =   cl (III) Let ( ),M g be a super generalized pseudo-Riemannian manifold. (i) If ( )ab abg g= Θ where abg is a classical smooth metric then we have,in any chart, ( )i ijk jkΓ = Θ Γ (with ijkΓ denoting the Christoffel Symbols of abg ). Hence for all ( ) ( ) ( ) 1 1 1 0 2 2: H HH M D H D H∈ =SG . (ii) If ab abg g∞≈ , where abg a classical smooth metric, ( )11 2 0,H H M∈SG and ( )1H X Mξ∞≈ ∈  , ( )12 0H D Mη ′≈ ∈ or ( )11 0H D Mξ ′≈ ∈ , ( )2H X Mη∞≈ ∈  , then ( ) ( )1 2HD H Dξ η≈ . (iii) Let ab k abg g≈ , where abg a classical kC -metric, then, in any chart, 1 i i jk k jk−Γ ≈ Γ . If in addition , ( )11 2 0,H H M∈SG , ( )11 1 ,kkH M TMξ −−≈ ∈Γ and ( )2 ,kkH M TMη≈ ∈Γ then ( ) ( )1 2H kD H Dξ η≈ . J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 386 Journal of High Energy Physics, Gravitation and Cosmology 1.6.5. The Super Generalized Riemannian Curvature Tensor Let ( ),M g be a super generalized pseudo-Riemannian manifold with a super generalized Levi-Civita connection D . (i) The super generalized Riemannian curvature tensor ( )13dabcR M∈SG is defined by [ ]1 2 1 21 2, 3 3 3, , .H H H HH HR H D H D D H −   (1.6.18) (i) The super generalized Ricci curvature tensor is defined by .cab cabR R (1.6.19) (iii) The super generalized Ricci scalar is defined by .aaR R (1.6.20) 4) Finally we define the super generalized Einstein tensor by 1 . 2ab ab ab G R R g− (1.6.21) 2. Distributional Schwarzschild Geometry by Using Nonsmooth Regularization via Horizon 2.1. Distributional Schwarzschild Spacetime as Colombeau Extension of the Lorentzian Manifold with Nonregularity Conditions on Schwarzschild Horizon Singular space-times present one of the major challenges in general relativity. Originally it was believed that their singular nature is due to the high degree of symmetry of the well-known examples ranging from the Schwarzschild geometry to the Friedmann-Robertson-Walker cosmological models. However, Penrose and Hawking [36] have shown in their classical singularity theorems that singularities are a phenomenon which is inherent to general relativity. Since the standard approach allows only smooth space-time metrics, one has to exclude the so called singular regions from the space-time manifold. In a recent work many authors advocated the use Colombeau distributional techniques [5]-[22] to calculate the energy-momentum tensor of the Schwarzschild geometry. It turns out that it is possible to include the singular region (i.e. the space-like line 0r = with respect to Schwarzschild coordinates) in the space-time which now no longer is a vacuum geometry, and to identify it with the support of the energy-momentum tensor [5] [9] [11] [12] [13]. The same "physically expected" result for the distributional energy momentum tensor of the Schwarzschild geometry was obtained in papers [12]-[22], i.e., ( )00 8π ,T m xδ=  (2.1.1) in a conceptually satisfactory way. Remark 2.1.1. The result (2.1.1) can be easily obtained by using apropriate nonsmooth regularization of the Schwarzschild singularity at the origin 0r = . The nonsmooth regularization of the Schwarzschild singularity at the origin 0r = was originally considered by N. R. Pantoja and H. Rago in paper [12]. J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 387 Journal of High Energy Physics, Gravitation and Cosmology Such non smooth regularization of the Schwarzschild singularity is ( )( ) ( ) ( ]1 , 0,1 , .s s rh r r r r rε εε ε ε ε = − + Θ − ∈ <    (2.1.2) Here ( )( )uε εΘ is the generalized Heaviside function,where ( ) ( ) , 0 1, 0 u u u ε ε ε <Θ =  ≥ (2.1.3) and the limit 0ε → is understood in a weak distributional sense. The equation ( ) ( )( )( ) ( )( )( ) ( ) ( ) ( ) 2 2 2 22 1 2 2 0 d d d d sin d , 1 ,s s h r t h r r r rh r r ε ε εε ε ε θ θ φ−  = − + +  = − + (2.1.4) with ( ], 0,1hε ε ∈ , as given in (2.1.4) can be considered as Colombeau version of the Schwarzschild line element in curvature coordinates. From Equation (2.1.2), the calculation of the distributional Einstein tensor ( )( ),ttG r εε , ( )( ), r rG r εε , ( )( ),G rθθ εε , ( )( ),G r φ φ ε ε proceeds in a straighforward manner. By simple calculation one obtains [12]: ( )( ) ( )( ) ( ) ( ) ( ) ( ) 2 2 2 1 , ,t rt r s s h r h r G r G r r r r r r r r r ε ε ε ε ε ε ε ε ε δ ε δ ′ +    = = − −        −  = − = −    (2.1.5) and ( )( ) ( )( ) ( ) ( ) ( ) ( ) ( ) '' 2 2 2 2 , , 2 d . ds s s h r h r G r G r r r r r r r r rr r r ε εθ φ θ φε ε εε εε ε ε δ ε δε δ ε     = = − −        −   = − − ≈ −       (2.1.6) In papers [10] [27] Colombeau distributional techniques were extended to the general axisymmetric, stationary Kerr and Newman space-time family. This family also contains the Schwarzschild geometry and its charged extension the Reissner-Nordstrø m solution as special cases of spherical symmetry. In the paper [22] it was shown that the solutions will satisfy the Einstein equations everywhere if the energy-momentum tensor has an appropriate singular addition of nonelectromagnetic origin. When this addition term is included, the total energy turns out to be finite and equal to 2mc , while the angular momentum for the Kerr and Kerr-Newman solutions is mca . Remark 2.1.2. The nonsmooth regularization of the Schwarzschild singularity above the horizon sr r= is ( )( ) ( )( ) ( ]1 , 0,1 , .s s srh r r r r rrε εε ε ε ε+  = − + Θ − − ∈ ≥    (2.1.7) Here ( )( )uε εΘ is the generalized Heaviside function and the limit 0ε → is understood in a weak distributional sense. The equation J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 388 Journal of High Energy Physics, Gravitation and Cosmology ( ) ( )( )( ) ( ) ( )( ) ( ) ( ) ( ) 12 2 2 22 2 2 0 d d d d sin d , 1 ,s s h r t h r r r rh r r ε ε εε ε ε θ θ φ −+ + +   = − + +    = − + (2.1.8) ( ], 0,1hε ε ∈ , as given in (2.1.8) can be considered as Colombeau version of the Schwarzschild line element in curvature coordinates above horizon. From Equation (2.1.7), the calculation of the distributional Einstein tensor above horizon ( )( ),ttG r εε + , ( )( ),rrG r εε + , ( )( ),G rθθ εε + , ( )( ),G rφφ εε + proceeds in a straighforward manner. By simple calculation one obtains ( )( ) ( )( ) ( )( ) ( )( ) ( )( ) ( ) 2 2 2 , , 1 . t r t r s s s s s s G r G r h r r h r r r r r r r r r r r r ε ε ε ε ε ε ε ε ε ε ε δ ε δ + +=    ′ − − + − −    = − −          − − −  = − ≈ −     (2.1.9) The truncated distributional Schwarzschild geometry. There exist two different types of distributional Schwarzschild blackhole geometry corresponding to classical Schwarzschild solution. That is: (i) full distributional Schwarzschild blackhole geometry, given by Colombeau generalized object, for example by Equation (1.3.30), see Figure 1(a) and (ii) the truncated distributional Schwarzschild space-time given by Colombeau generalized object (2.1.7)-(2.1.8), i.e. in this case distributional spacetime ends just on the Schwarzschild horizon, see Figure 1(b). Remark 2.1.3. In a nutshell, there is a widespread but mistaken belief that there exist true gravitational singularities, for example at origin 0r = of the Figure 1. (a) The picture of a distributional Schwarzschild blackhole, given by Colombeau generalized object (1.3.30). Distributional spacetime ends just on the Schwarzschild singularity. (b) The truncated Schwarzschild distributional geometry, given by Colombeau generalized object (2.1.7)-(2.1.8). Distributional spacetime ends just on the Schwarzschild horizon. J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 389 Journal of High Energy Physics, Gravitation and Cosmology Schwarzschild spacetime, and non principal and non gravitational, i.e. purely coordinate singularities, for example at horizon gr r= of the Schwarzschild spacetime. A coordinate singularity or coordinate degeneracy occurs when an apparent singularity or degeneracy occurs in one coordinate frame, which can be removed by choosing a different frame. Classical example of such mistake is ubnormal deletion of the gravitational singularity, for example from Schwarzschild spacetime { }( ) ( )2 2 , , , ,ijS r m g r θ φ= × ≥ ×Sch (2.1.10) originally defined by singular and degenerate Schwarzschild metric [30], ( )( ) ( )( ) ( ) ( ) ( )2 2 2 22 0 1 2 2d d d d sin d , 1 .grs h r x h r r r h r rθ θ φ −  = − + + + = −  (2.1.11) by using apropriate singular coordinate change [27]-[35]. Remark 2.1.4. Note that: (i) metric (2.1.11) is singular and degenerate at Schwarzschild horizon gr r= , and thus metric (2.1.11) beiond canonical rigorous semi-Riemannian geometry. (ii) however in physical literature (see for example [28] [29] [30]) singularity and degeneracy at Schwarzschild horizon gr r= are accepted as coordinate singularity and coordinate degeneracy. Remark 2.1.5. (see [30] section 100, p. 296). "In the Schwarzschild metric (97.14), 00g goes to zero and 11g to infinity at gr r= (on the 'Schwarzschild sphere'). This could give the basis for concluding that there must be a singularity of the space-time metric and that it is therefore impossible for bodies to exist that have a 'radius' (for a given mass) that is less than the gravitational radius. Actually, however, this conclusion would be wrong. This is already evident from the fact that the determinant ( ) 4 2sing r r θ= − has no singularity at gr r= , so that the condition 0g < (82.3) is not violated. We shall see that in fact we are dealing simply with the impossibility of establishing a suitable reference system for gr r< ." Remark 2.1.6. Notice that consideration above meant the following definition of the gravitational singularity. Definition 2.1.1. There is no gravitational singularity at r r= iff the determinant ( ) ( )( ), det ,ijg r g rθ θ= has no singularity at r r= . Remark 2.1.7. Notice that at singular point gr r= the determinant ( )gg r is well defined only by the limit ( ) ( )( ) 4 2lim det , sin . g g ij gr r g r g r rθ θ → = = − (2.1.12) however in the limit = 2gr r m→ the classical Levi-Civitá connection l kjΓ becomes infinite ( ) ( ) ( ) ( ) 1 0 11 012 22 2 lim , lim , 2 2r m r mr m r m m mr r r r m r r m= =→ → − Γ = = ∞ Γ = = ∞ − − (2.1.13) and therefore the Definition 2.1.1 is not sound and even does not any sense J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 390 Journal of High Energy Physics, Gravitation and Cosmology under canonical semi-Riemannian geometry. Remark 2.1.8. Notice that: (i) in order to fix the problem with singularity and degeneracy of the Schwarzschild metric (2.1.11) at Schwarzschild horizon gr r= , in physical literature [27]-[35], many years oneconsiders the abnormal formal change of coordinates obtained by replacing the canonical Schwarzschild time by "retarded time" ( ),t rν , i.e., Eddington-Finkelstein coordinates, given by ( ) ( ) ( ) 1 d , d d , 1 ;g t r t h r r r h r r ν − = +    = − (2.1.14) (ii) the change (2.1.14) of Schwarzschild coordinates is singular at Schwarzschild horizon gr r= , as at Schwarzschild horizon ( )gh r = ∞ and therefore the change (2.1.14) does not holds on Schwarzschild horizon [36]; (iii) under the singular change (2.1.14) Schwarzschild metric (2.1.11) becomes to well known regular and nondegenerate Eddington-Finkelstein metric [27]-[35]: ( ) ( )2 22 2 2 22d 1 d 2d d d sin d ;ms v r v r r θ θ φ   = − − + + +     EF (2.1.15) (iv) in physical literature many years exist abnormal belief that by formal singular change (2.1.15) the singular and degenerate Schwarzschild spacetime { }( )2 2r m× > ×S was immersed in a larger Eddington-Finkelstein spacetime { } { }( ) ( )2 2 0 2 , , ,r m r m g r θ≥ ≥= × ≥ < ≤ ×  EFEF S (2.1.16) with regular and non degenerate metric tensor ( ),g r θ ≥EF , and whose manifold is not covered by the canonical Schwarzschild coordinate with 2r m≤ , and therefore singularity and degeneracy on Schwarzschild horizon gr r= are only coordinate singularity and coordinate degeneracy; (v) from statement (iii) it was mistakenly assumed that there is no gravitational singularity at BH horizon. We remind now canonical definitions. Definition 2.1.2. Let ( ),M g and ( ),N h be semi-Riemannian manifolds. An isometric embedding is a smooth embedding :f M N→ which preserves the metric in the sense that g is equal to the pullback of h by f, i.e. g f h∗= . Explicitly, for any two tangent vectors ( ), xT M∈v w we have ( ) ( ) ( )( ), , .g h df df=v w v w (2.1.17) Remark 2.1.9. Notice that such isometric embedding is a mathematical definition only and does not mean the equivalence ( ) ( )( ), ,M g f M h≡ in absolute sense. Thus, it is not always appropriate as equivalence of the Lorentzian manifolds ( ),M g and ( ),N h corresponding to the physical frames ( ),M gph ph and ( ),N hph ph . Definition 2.1.3. [31]. In general, a Lorentzian manifold ( ),M h′ is said to be an extension of a Lorentzian manifold ( ),M g if there exists an isometric embedding :i M M ′→ . J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 391 Journal of High Energy Physics, Gravitation and Cosmology Remark 2.1.10. Notice that such extension is a mathematical definition only and therefore it is not always apropriate as extension of the Lorentzian manifolds ( ),M g and ( ),M h′ corresponding to the physical frames ( ),M gph ph and ( ),M h′ph ph . Remark 2.1.11. In order to obtain example for the statement mentioned and Remark 2.1.8 and Remark 2.1.9 we are going to prove below that the geometry of Schwarzschild spacetime { }( ){ }2 2 ,r m g >> × > ×  SchSch S above Schwarzschild horizon is essentially cardinally different in comparison with the geometry of Eddington-Finkelstein spacetime { }( ){ }2 2 ,r m g >> × > ×  EFEF S above Eddington-Finkelstein horizon. We remind now canonical definitions. Definition 2.1.4. Let kAΓ∆ be the change in a vector ( )iA x after parallel displacement (as ploted in Figure 2) around closed contour Γ located in BH spacetime as ploted in Figure 3. This change kAΓ∆ can clearly be written in the form kAδ Γ ∫ . Substituting in place of kAδ the canonical expression ( )i lk kl kA x A dxδ = Γ (see [31], Equation (85.5)) one obtains Figure 2. Paralel displacement along a closed contour Γ in a curved space. Figure 3. Paralel displacement along a closed contour Γ in BH spacetime. J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 392 Journal of High Energy Physics, Gravitation and Cosmology ( ) d .i lk k kl kA A x A xδΓ Γ Γ ∆ = = Γ∫ ∫  (2.1.18) Definition 2.1.5. (I) Let gShΣ be Schwarzschild horizon, let xΓ be a contour located in Schwarzschild spacetime as plotted in Figure 4 and such that (i)  xx∈Γ , (ii)   g x xΣ Γ =Sch , and let xΓ be a curve   \ x x xΓ = Γ . Let x kAΓ∆ be the integral ( )   \ \  d .x x x i l k k kl k x x A A x A xδ Γ Γ Γ ∆ = = Γ∫ ∫  (2.1.19) (II) Let gΣEF be Eddington-Finkelstein horizon, let xΓ be a contour located in Eddington-Finkelstein spacetime as plotted in Figure 5 and such that (i)  xx∈Γ , (ii)   g x xΣ Γ =EF , and let xΓ be a curve   \ x x xΓ = Γ . Let x kAΓ∆ be the integral ( )   \ \  d .x x x i l k k kl k x x A A x A xδ Γ Γ Γ ∆ = = Γ∫ ∫  (2.1.20) Figure 4. Parallel displacement x kAΓ∆ along a curve xΓ in Schwarzschild spacetime such that   g x xΣ Γ =Sch , then always x kAΓ∆ = ∞ . Figure 5. Parallel displacement along a curve xΓ in Eddington-Finkelstein spacetime   g x xΣ Γ =EF , then always x kAΓ∆ < ∞ . J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 393 Journal of High Energy Physics, Gravitation and Cosmology Remark 2.1.12. (I) Note that the geometry of Schwarzschild spacetime >Sch { }( ){ }2 2 ,r m g >> × > ×  SchSch S (2.1.21) above Schwarzschild horizon gΣSch , essantially cardinally different in comparizon with the geometry of Eddington-Finkelstein spacetime >EF { }( ){ }2 2 ,r m g >> × > ×  EFEF S (2.1.22) above Eddington-Finkelstein horizon gΣEF . (II) Note that Schwarzschild spacetime >Sch obviously satisfies a very strong nonregularity condition  if , then .x g x kx AΓΣ Γ = ∆ = ∞Sch (2.1.23) Thus the geometry of spacetime >Sch that is nonclassical geometry beyond apparatus of the classical semi-Riemannian geometry. Of course, the geometry any part of spacetime >Sch located above some neighborhood of Schwarzschild horizon as plotted in Figure 6 that is a classical semi-Riemannian geometry. Remark 2.1.13. Note that from Remark 2.1.11 it follows that Eddington-Finkelstein spacetime does not hold in rigorous mathematical sense as extension of the Schwarzschild spacetime { }( ){ }2 2 ,r m g >> × > ×  SchSch S above Schwarzschild horizon. Remark 2.1.14. It is clear that nonregularity condition (2.1.23) arises not only from singularity of the function ( )1h r− at point gr r= but from degeneracy of the function ( )h r at point gr r= . Remark 2.1.15. We remind now that the relations (see [30] p. 234, Equation (84.7)) 0 0 00 g g g g α β αβ αβγ = − + (2.1.24) Figure 6. Parallel displacement along a closed contour Γ located in region of the classical semi-Riemannian geometry of the Schwarzschild spacetime such that gΣ = ∅Sh , then always kAΓ∆ < ∞ . J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 394 Journal of High Energy Physics, Gravitation and Cosmology give the connection between the metric of real space 2d d dl x xα βαβγ= (2.1.25) and the metric of the four-dimensional space-time ( )22 0 00 00d d d 2 d d d .s g x x g x x g xα β ααβ α= + + (2.1.26) For Eddington-Finkelstein metric (2.1.15) metric of the corresponding real space is ( ) ( ) 2 2 22 2 2dd d sin d .21 rl rm r θ θ φ = + +  − EF (2.1.27) Remark 2.1.16. Notice that the Eddington-Finkelstein metric (2.1.15) is regular at the horizon and therefore the infalling observer encounters nothing unusual at the horizon. However from Equation (2.1.17) it follows that the infalling observer encounters singularity on horizon. But this is a contradiction. Remark 2.1.17. Note that in order to deal with singular Schwarzschild metric (2.1.11) using mathematically and logically soundness approach, one applies contemporary distributional geometry based on Colombeau generalized functions [2] [3] [4]. Distributional Schwarzschild geometry and distributional BHs geometry by using Colombeau generalized functions [2] [3] [4] was developed by many papers [4]-[22]. By aproporiate regularization ( ) ( ], , , , 0,1ijg rε θ φ ε ∈ of the singular Schwarzschild metric ( ), ,ijg r θ φ such that: (i) ( ) ( ),0 , , , ,ij ijg r g rθ φ θ φ= and (ii) for any ( ]0,1ε ∈ metric tensor ( ), , ,ijg rε θ φ is regular and nondegenerate, one obtains Colombeau generalized object ( )( ) ( )3, , ,ijg rε εθ φ ∈  G with an representative ( )( ), , ,ijg rε εθ φ , for a more detailed explanation see [11] [18] [19]. Using rigorous Colombeau approach one obtains mathematically and logically soundness notion of singularity in Distributional Schwarzschild spacetime. Remark 2.1.18. Note that in the case of Schwarzschild spacetime the conditions (i) and (ii) mentioned above (see Remark 2.1.13) are satisfied only by using non smooth regularization of the singular and degenerate Schwarzschild metric ( ), ,ijg r θ φ via Schwarzschild horizon [18] [19]. By apriporiate nonsmooth regularization one obtain Colombeau generalized object modeling the singular Schwarzschild metric above and below horizon [18] [19]: ( ) ( )( ) ( )( ) ( ) ( )( ) ( )( ) ( ) ( )( ) ( ) ( ] 12 2 2 2 2 12 2 2 2 2 2 2 d d d d , d d d d , , , 0,1 . s g g s h r t h r r r s h r t h r r r r r r r h r r r r ε ε εε ε ε ε ε εε ε ε ε ε ε ε ε −+ + + −− − − +  = − + + Ω   = − + Ω  Θ − − − + = ≥ ∈ (2.1.28) J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 395 Journal of High Energy Physics, Gravitation and Cosmology Remark 2.1.19. Let us rewrite now the metric (2.1.24) (above horizon) in the form ( ) ( )( ) ( )( ) ( ) ( )( ) ( ) ( ) ( ) 12 2 2 2 2 2 2 1 1 2 2 2 2 d d d d sin d d d d d d sin d , s h r t h r r r h r t h r r t h r r r ε ε εε ε ε ε ε εε ε θ θ φ θ θ φ −+ + + − −+ + +  = − + + +         = − − +            + + (2.1.29) and define a new generalized Colombeau coordinates ( )( ), , ,rε ετ θ φ , where ( )( ) ( )2,t rε ετ ∈ G , by formula ( )( ) ( )( )1d , d d , . t r t h r r r r ε εε ε τ −+ = +   = (2.1.30) Remark 2.1.20. Notice that: (i) Colombeau generalized coordinates (2.1.26) are the Colombeau extension of the canonical Eddington-Finkelstein coordinates (2.1.14) by Colombeau generalized function. (ii) In contrast with canonical Eddington-Finkelstein coordinates (2.1.14) (see Remark 2.1.7), Colombeau generalized coordinates (2.1.26) holds at Schwarzschild horizon gr r= as at Schwarzschild horizon Colombeau generalized function ( )( )1h rε ε −+   become well defined Colombeau generalized number ( ) 1gh rε −+  ∈   . Rewriting now the metric (2.1.25) in terms of the Colombeau generalized coordinates ( )( ), , ,rε ετ θ φ , it then above horizon takes the form ( ) ( )( )( ) ( ) ( ) ( )( )( )( ) ( ) ( ) 12 2 2 2 2 2 2 2 2 2 d d 2 d d d sin d d 2d d d sin d . s h r h r r r h r r r ε ε ε ε εε ε ε ε ε ε εε ε τ τ θ θ φ τ τ θ θ φ −+ + + +    = − − + +      = − + + + (2.1.31) We rewrite now Colombeau metric (2.1.27) in the equivalent form ( ) ( )( ) ( )2 2 2 2 2 2d d 2d d d sin d .s h r r rε εε ετ τ θ θ φ + += − + + + (2.1.32) Colombeau metric (2.1.28) define the distributional Eddington-Finkelstein space-time { }( ){ }2 2 ,r m g ≥+ +≥ × ≥ ×   EFEF S (2.1.33) above the Eddington-Finkelstein horizon 2r m= . Remark 2.1.21. Notice that ( )( ) ( ) ( )( ) ( ) ( ) ( )( ) ( ) ( )( ) ( )( ) ( ] 11 1 1 2 2 1 2 2 2 , , d d d , d d 2 d d d , 0,1 . g g g g g g r r r r gr r g g r r h r r h r r t r r t r t r r r ε εεε εε ε ε ε ε ε ε ε ε ε τ ε τ ε ε ε −+ − + − = = − = − − =  = = ⋅ ∈  = + ⋅ = + ⋅ + ∈   (2.1.34) J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 396 Journal of High Energy Physics, Gravitation and Cosmology Of course at horizon ( )( ), 0gh t rε ε+ ≈ , because at horizon ( )0 , 0gh t r+ = , however it follows from (2.1.24) at horizon the quantities ( )( )( ) ( )( ) ( )( )2 1 2d , dg g gh r t r r rε ε εε ετ ε+ −≈ and ( ) ( )( )1d dgr rε ε ετ ε −≈ are infinite large Colombeau quantities, i.e., the differential ( )d ε ετ is not classical but it is Colombeau differential. Remark 2.1.22. Note that: (i) under coordinate change (2.1.26) the distributional curvature scalars of the distributional Schwarzschild space-time given by metric (2.1.24), does not changes because these scalars depend only on variable r r= , (ii) in contrast with classical Eddington-Finkelstein space-time { } { }( ) ( )2 2 0 2 , , ,r m r m g r θ≥≥ = × ≥ < ≤ ×  EFEF S distributional Eddington-Finkelstein space-time has a gravitational singularity at horizon. Remark 2.1.23. Note that for the case of the distributional space-time the relations (2.1.24) obviously takes the form ( )( ) ( ) ( ) ( )( ) 0 0 00 g g g g α β αβ αβε ε ε ε γ ε ε ε   = − +     (2.1.35) where (2.1.30) give the connection between the Colombeau metric of the distributional real space ( ) ( )( )( )2d d dl x xα βε αβε εγ ε= (2.1.36) and the Colombeau metric of the four-dimensional distributional space-time ( ) ( )( ) ( )( ) ( )( )( ) 2 0 0 20 00 d d d 2 d d d . s g x x g x x g x α β α ε αβ αε ε ε ε ε ε ε = + + (2.1.37) For distributional Eddington-Finkelstein metric (2.1.29) above horizon of the corresponding Colombeau metric of the distributional real space is ( ) ( )( )( ) ( ) ( ) 12 2 , 2 22 2 d d d sin d . l h r r r εε ε ε θ θ φ + ≥ −+ +=  + +  EF (2.1.38) Remark 2.1.24. Notice since the distributional Eddington-Finkelstein space-time (2.1.29) has a gravitational singularity (see Definition 1.1.1) at horizon, there is no contradiction mentioned above for the case of the regular classical Eddington-Finkelstein metric (2.1.15) and the corresponding singular metric (2.1.17), see Remark 2.1.15. 2.1.2 Distributional Kruskal-Szekeres Spacetime Recall that the classical Kruskal-Szekeres coordinates are defined, from the classical Schwarzschild coordinates ( ), , ,t r θ φ , by replacing t and r by a new time coordinate T and a new spatial coordinate X: J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 397 Journal of High Energy Physics, Gravitation and Cosmology 1 2 1 2 1 2 1 2 : 1 exp sinh , 2 1 exp cosh , 2 0 : 1 exp sinh , 2 1 exp cosh 2 g g g g g g g g g g g g g g r r tr r T r r r r r tX r r r r r tr r T r r r r r tX r r r       > = −                       = −                       < < = −                       = −              .  (2.1.39) It follows that the Schwarzschild radius r, in terms of Kruskal-Szekeres coordinates, is implicitly given by 1 2 2 2 1 exp g g r rT X r r     − = −           (2.1.40) for both interior and exterior regions, i.e. { }\ 0r +∈ . In these new coordinates the metric of the Schwarzschild black hole manifold is given by 3 2 2 2 2 24d exp d d d .g g r rs T X r r r    = − − + + Ω       (2.1.41) The location of the event horizon ( 2gr GM= ) in these coordinates obviously is given by 2 2 0 .T X T X− = ⇒ = ± (2.1.42) Remark 2.1.25. Note that the metric (2.1.37) ofcourse is perfectly well defined and non-singular at the event horizon. The curvature singularity is located at 2 2 1T X− = . Under this property Kruskal-Szekeres spacetime in physical literature mistakenly considered as regular Lorentzian spacetime, except singular submanifold ( ){ }2 2, | 1T X T X− = . Remark 2.1.26. In contrast with Eddington-Finkelstein coordinates the classical Kruskal-Szekeres coordinates holds at Schwarzschild horizon, but however the differentials d ,dT X of the functions ( ) ( ), , ,T r t X r t are singular at Schwarzschild horizon gr r= and therfore Kruskal-Szegeres spacetime cannot be considered as Schwarzschild spacetime in Kruskal-Szekeres coordinates (2.1.35)-(2.1.36). Remark 2.1.27. In order to avoid these difficulties one can apply instead of the Kruskal-Szekeres coordinates (2.1.35)-(2.1.36) the following distributional Kruskal-Szekeres coordinates to Colombeau generalized metric (2.1.8) ( ] ( ) ( )( )( ) ( ) ( )( )( ) 1 2 1 2 , 0,1 : 1 exp sinh , 2 1 exp cosh , 2 g g g g g g g g g r r r r tT r r r r r r r tX r r r r r ε εε ε ε ε εε ε ε ε ε ε ε ε ≥ ∈            = Θ − − − +                                    = Θ − − − +                         J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 398 Journal of High Energy Physics, Gravitation and Cosmology ( ) ( )( )( ) ( ) ( )( )( ) 1 2 1 2 0 : 1 exp sinh , 2 1 exp cosh . 2 g g g g g g g g g r r r r tT r r r r r r r tX r r r r r ε εε ε ε ε εε ε ε ε ε ε ε < <            = Θ − − − +                                    = Θ − − − +                         (2.1.43) Therefore for both interior and exterior regions we get ( ) ( ) 1 2 2 2 1 exp . g g r rT X r rε εε ε ε ε        − = − +               (2.1.44) Remark 2.1.28. Note that in contrast with (2.1.37) at horizon gr r= : ( ) ( ) ( )2 2 1 2 0 .T X eε εε ε εε − = ≠   (2.1.45) In these new distributional coordinates the Colombeau metric (2.1.8) of the distributional Schwarzschild black hole manifold above horizon is given by formula ( ) ( )( )( )3 2 2 2 2 2 4 d exp d d d . g g g r r r rs T X r r r ε ε ε ε εε ε ε Θ − −    = − − + + Ω         (2.1.46) Here ( )( )uε εΘ is the generalized Heaviside function given by Equation (2.1.3). Remark 2.1.29. Note that in contrast with (2.1.36) Colombeau generalized metric (2.1.39) is non degenerate at horizon gr r= in Colombeau sense. 2.2. Distributional Schwarzschild Spacetime and Distributional Rindler Spacetime with Distributional Levi-Cività Connection. Generalized Einstein Equivalence Principle 2.2.1. Distributional Schwarzschild Spacetime with Distributional Levi-Cività Connection Remark 2.2.1. Note that due to the degeneracy of the metric (2.1.11) at Schwarzschild horizon, the classical Levi-Civit'a connection on whole Schwarzschild spacetime is not available [18] [19] as classical Levi-Civit`a connection on Schwarzschild horizon becomes infinity ( ) ( ) ( ) ( ) 1 0 11 012 22 2 lim , lim , 2 2r m r mr m r m m mr r r r m r r m= =→ → − Γ = = −∞ Γ = = ∞ − − (2.2.1) Remark 2.2.2. In order to avoid difficulties with classical Levi-Civit'a connection mentioned above in Remark 2.2.1, in papers [18] [19] we have applied the non smooth regularization via Schwarzschild horizon, see Remark 2.1.5 and Equation (2.1.6). Corresponding Colombeau distributional connections ( )( )lkj εε +Γ and ( )( )lkj ε−Γ above and below Schwarzschild horizon are [18] [19]: J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 399 Journal of High Energy Physics, Gravitation and Cosmology ( )( ) ( ) ( ) ( ) ( )( ) ( )( ) ( ) ( ) ( ) ( )( ) , , , , , , 1 , 2 1 . 2 l lm kj mk j mj k kj m l lm kj mk j mj k kj m g g g g g g g g ε ε ε εε ε ε ε ε εε ε ε ε + + + + + − − − − −  Γ = + −    Γ = + −   (2.2.2) Obviously distributional connections ( ) ( ),l lkj kjh hε εε ε+ + − +   Γ Γ    coincides, in distributional sense, with the corresponding classical Levi-Cività connections on { }3 \ 2r m= , since ( ) 0h hε ε + += , ( ) 0h hε ε − −= and ( ) 0lm lmg gε ε + += , ( ) 0lm lmg gε ε − −= there. Clearly, connections ( ) ( ) ( ], , 0,1l lkj kj+ −Γ Γ ∈   in respect the regularized metric ( ], 0,1g± ∈  , i.e., ( ) ; 0ij kg ± = . Proceeding in this manner, we obtain the nonstandard result [22] [23] see also Appendix B: ( ) ( ) ( ) ( ) ( ) ( ) 1 0 21 0 1 0 21 0 2 4π , 2 4π . r m R R m r r m R R m r ε ε ε ε δ δ + + − − −      = = −          −      = =              (2.2.3) Remark 2.2.3. As expected, the distributional Ricci tensor as well as the distributional Ricci scalar vanish identically on { }3 \ 2r m= , since ( )( ) { }supp 2 2r m r mδ − = = . This result is in a good agreement with canonical result [24]-[30] on { }3 \ 2r m= since distributional connections (2.2.2) coincide with the corresponding classical Levi-Cività connections on { }3 \ 2r m= at least in distributional sense. For ( )2 0r mε ε− ≈  we obtain the nonstandard result: ( ) ( )( ) ( )( ) ( ) ( )( ) ( )( ) 4 324 2 4 324 2 , , , 4 2 , , , 4 2 r r m r m r r m r m μν ε μν ε ε ε ε ρσμν ε ρσμν ε ε ε ε εε ε ε εε ε ε ± ± ± ±     ≈ +   + −       ≈ +   + −       R R R R   (2.2.3) where ( )2 0r mε ε− ≈  , see Appendix C. For ( ) ( )2r mε εε ε− ≈  , see Appendix C, Remark C.10, Equation (C22), we obtain [18] [19]: ( ) ( )( ) ( ) ( ) ( ] ( ) ( )( ) ( ) ( ) ( ] 4 24 2 0, 4 24 2 0, , , 1 , 4 2 , , 1 , 4 2 r r O m r m r r O m r m μν ε μν ε ε ε ε η ρσμν ε ρσμν ε ε ε ε η εε ε ε εε ε ε ± ± ∈ ± ± ∈    ≈ +  − +       ≈ +  − +        R R R R   (2.2.4) For ( ]2 0, , 1r m η η− ∈  , see Appendix C, Remark C.10, Equation (C22), we obtain ( ) ( )( ) ( ) ( ) ( ] ( ) ( )( ) ( ) ( ) ( ] 24 2 0, 24 2 0, 1, , 1 , 4 2 1, , 1 . 4 2 r m r m r r O m r m r r O m r m μν ε μν ε ε η ρσμν ε ρσμν ε ε η ε ε ε ε ± ± − ∈ ± ± − ∈ ≈ + − ≈ + −       R R R R (2.2.4) J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 400 Journal of High Energy Physics, Gravitation and Cosmology 2.2.2. Distributional Rindler Space-Time with Distributional Levi-CivitàConnection. Non-Regularity Conditions and Nonclassical Nature of the Rindler Space-Time We remind now that 2D Rindler spacetime is a patch of Minkowski spacetime, see Figure 7. In 2D, the Rindler metric is 2 2 2 2d d d .s R R η= − (2.2.5) Remark 2.2.4. Due to the degeneracy of the metric (2.2.5) at Rindler gorizon 0R = , the classical Levi-Cività connection is not available on whole 2 , e.g., 1 4 4 1 44 14 41, ,R R −Γ = Γ = Γ = (2.2.6) and all other components being zero. Remark 2.2.5. We emphazize that Rindler space-time 1.1 is satisfied the same non-regularity conditions as Schwarzschild space-time Sch>, see Remark 2.1.12. Let xΓ be a contour located in Rindler space-time 1.1 and let x be Rindler horizon as plotted in Figure 8 and let kAΓ∆ be the change in a vector ( )kA x after parallel displacement (as ploted in Figure 2) around closed contour Γ (see Definition 2.1.4) located in Rindler space-time 1.1 as ploted in Figure 8. Remark 2.2.6. We emphazize that in physical literature the Rindler metric (2.2.5) mistakenly were considered as is just a part of the Minkowski space-time 1.1 . Obviously by non-regularity conditions kAΓ∆ = ∞ the geometry of Rindler space-time essantially ardinally different in comparizon with the geometry of Minkowski space-time 1.1 even if the Rindler horizon is excluded Figure 7. Hyperbolic motion in the right rindler wedge. ( )22 2 2 2x c t c a− = . J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 401 Journal of High Energy Physics, Gravitation and Cosmology Figure 8. This is the right wedge, which covers one quarter of the Penrose diagram. Parallel displacement along a curve xΓ in Rindler spacetime R1.1 such that { }  \x x xΓ = Γ , then always kAΓ∆ = ∞ . from the space 1.1 . Remark 2.2.7. Note that in order to avoid this difficultnes mentioned above (see Remark 2.2.4-2.2.5), the origin in classical consideration the Rindler horizon is always excluded from the space 3.1 and we are working on { }3.1 3.1 \ 0=  , and therefore for Einstein's tensor (2.2.7) following Moller [24] we get (2.2.8) where the accents indicate differentiation with respect variable R, and all other components of vanish identically. Thus Rindler metrical tensor satisfy on the Einstein field equations 1 0. 2 k k k i i iδ− =G R R (2.2.9) Remark 2.2.8. By calculations mentioned above, from Mo ller's times until nowdays, Rindler metrical tensor was mistakenly considered in physical literature as an vacuum solution of the Einstein's field equations,e.g.,solution for empty space,see Møller [23]. 1 , 2 k k k i i i i iδ− G R R R R ( ) ( )2 2442 3 2 3 44 2 2 44 44 21 1= 2 0, 2 2 2 2 g R g g g R R    ′ ′′= = − − − − ≡           G G k iG { }3.1 \ 0 J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 402 Journal of High Energy Physics, Gravitation and Cosmology Remark 2.2.9. Note that Levi-Cività connection on the whole space R3.1 is available only in Colombeau sense under smooth regularization ( ]2 2 2 , 0,1R R ε ε→ + ∈ and therefore we forced to change metric (2.5) by Colombeau object ( ) ( ) ( ) ( ) ( ) ( ] 2 2 2 2 2 2 2 44, 2 2 44, d d d d d , 0,1 . s R R R g g R ε ε εε ε ε ε ε ε η η ε ε      = − + = −         = + ∈    (2.2.10) Then for Einstein distributional tensor [18] [19] [20]: ( ) ( ) ( ) ( ), , ,1 ,2 k k k i i i i iε ε ε ε εε εε ε δ− G R R R R (2.2.11) we get ( )( ) ( )( ) ( ) ( ) 2 2 44,2 3 2, 3, 44, 22 2 44, 44, 1 . 2 2 g R R g g g R ε ε ε εε ε ε ε ε ε ε ε    ′    ′′= = − − −      +     G G (2.2.12) Thus, ( )( ) ( )( ) ( )2 3 22, 3,0 0 ,ε εε ε εε −     = =     G G (2.2.13) where ( )2 ε ε − ∈   is infinite Colombeau generalized numbers, and therefore ( )( )22, Rε εG and ( )( ) 3 3, Rε εG is nontrivial Colombeau generalized functions and distributional Rindler metric tensor given by (2.2.12) that is non vacuum Colombeau solution of the Einstein field equations. 2.2.3. Generalized Einstein Equivalence Principle We remind that originally Einstein's gravity was formulated by using classical pseudo Riemannian geometry with classical Levi-Civit'a connection. In classical pseudo Riemannian geometry, the Levi-Civita connection is a specific connection on the tangent bundle of a manifold. More specifically, it is the torsion-free metric connection, i.e., the torsion-free connection on the tangent bundle (an affine connection) preserving a given (pseudo-Riemannian) Riemannian metric. The fundamental theorem of classical Riemannian geometry states that there is a unique connection which satisfies these properties. Remark 2.3.1. Note that classical Einstein "Equivalence Principle" asserts the equivalence between inertial and gravitational forces of acceleration. The classical Einstein equivalence principle is the heart and soul of gravitational theory, for it is possible to argue convincingly that if EEP is valid, then gravitation must be a "curved spacetime" phenomenon, in other words, gravity must be governed by a "metric theory of gravity", whose postulates are: 1) Spacetime is endowed with a symmetric Lorentzian metric. 2) The trajectories of freely falling test bodies are geodesics of that metric. 3) In local freely falling reference frames, the non-gravitational laws of physics are those written in the language of special relativity. In order to obtain appropriate generalization of EEP based on distributional Colombeau geometry [4] [5] [6] [7] we claim the following generalized J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 403 Journal of High Energy Physics, Gravitation and Cosmology equivalence principle (GEEP): 1) Spacetime in general case is endowed with a symmetric distributional Lorentzian metric. 2) The trajectories of freely falling test bodies are geodesics of that distributional metric. 3) In local freely falling distributional reference frames, the non-gravitational laws of physics are those written in the language of special relativity. 3. Quantum Scalar Field in Curved Distributional Spacetime. Unruh Effect Revisited 3.1. Canonical Quantization in Curved Distributional Spacetime In a recent work [19] the authors advocated the use De Witt-Schwinger approach [37] [38] [39] [40] in order to establish QFT in general ditributional curved spacetime. The vacuum energy density of free scalar quantum field Φ with a distributional background spacetime is considered successfully. It has been widely believed that, except in very extreme situations, the influence of gravity on quantum fields should amount to just small, sub-dominant contributions. Here we argue that this belief is false by showing that there exist well-behaved spacetime evolutions where the vacuum energy density of free quantum fields is forced, by the very same background distributional spacetime such as in BHs, to become dominant over any classical energy density component. This semiclassical gravity effect finds its roots in the singular behavior of quantum fields on curved distributional spacetimes. In particular we obtain that the vacuum fluctuations 2Φ have a singular behavior on BHs horizon ( ) 22: ~r r r r −+ +Φ − . Much of formalism can be explained with Colombeau generalized scalar field [19]. The basic concepts and methods extend straightforwardly to distributional tensor and distributional spinor fields. To begin with let us take a spacetime of arbitrary dimension D, with a metric vgμ of signature ( )+ − − . The action for the Colombeau generalized scalar field ( ) ( )Mε εφ ∈G is ( ) ( ) ( )2 21d . 2 D M S x g g m Rμνε ε ε μ ε ν ε ε εε ε φ φ ξ φ   = ∂ ∂ − +    ∫ (3.1.1) Here ξ is a coupling constant (see [40] chapter 3). The corresponding equation of motion is ( ) ( ]2, , 0,1 .x m Rε ε ε εξ φ ε + + ∈  (3.1.2) Here ( ) ( )1 2 1 2, .x g g g μνε ε ε μ ε ε μ εε εφ φ −= ∂ ∂ (3.1.3) With  explicit, the mass m should be replaced by m  . Separating out a time coordinate 0x , ( )0 , , 1, 2,3ix x x iμ = = we can write the action as ( ) ( ) ( ) ( )0 1d , d .DS x L L xε ε ε εε εε ε−= =∫ ∫  (3.1.4) J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 404 Journal of High Energy Physics, Gravitation and Cosmology The canonical momentum at a time 0x is given by ( )( ) ( )( )( ) ( )( )1 20 = ,x L x h n xμε ε ε ε μ εε ε επ δ δ φ φ= ∂ ∂ (3.1.5) where x labels a point on a surface of constant 0x , the 0x argument of ( )ε εφ is suppressed, n μ is the unit normal to the surface, and ( )hε ε is the determinant of the induced spatial metric ( )( )ijh εε . In order to quantize, the Colombeau generalized field ( )ε εφ and its conjugate momentum ( )( )xε επ are now promoted to hermitian operators and required to satisfy the canonical commutation relation, ( ) ( )( ) ( ) ( ]1, , , 0,1 .Dx y i x yε ε ε φ π δ ε−  = ∈   (3.1.6) Here ( ) ( ) ( )1 1d ,D Dy x y f y f xδ− − =∫ for any scalar function ( )3f D∈  , without the use of a metric volume element. We form now a conserved bracket from two complex Colombeau solutions to the scalar wave Equation (3.1.2) by [19]: ( ) ( ], d , 0,1 ,jμε ε μ εε ε φ φ ε Σ   = Σ ∈    ∫ (3.1.7) where ( )( ) ( ) ( )( )1 2, .j i g gμ μνε ε ε ε ε ε ν ε ε ν εε εφ φ φ φ φ φ= ∂ − ∂ (3.1.8) Using equation of motion Equation (3.1.2) one obtains corresponding Colombeau generalization of the canonical Green functions equations. In particular for the Colombeau distributional propagator ( )( ) ( ) ( )( )( ) ( ], 0 0 , 0,1 ,i G x x T x xε ε εε εφ φ ε± ± ±′ ′= ∈ (3.1.9) one obtains directly ( ) ( )( ) ( )( ) ( )1 22, , , , .nx m x G x x g x x xε ε ε εξ ε ε δ −± ± ±   ′ ′+ + = − − −    R (3.1.10) We obtan now an adiabatic expansion of ( )( ),G x xε ε ± ′ [19]. Introducing Riemann normal coordinates yμ for the point x , with origin at the point x′ one obtains ( )( ) ( )( ) ( )( ) ( )( ) ( )( ) ( )( ) ; ; 1 1, 3 6 1 2 20 45 v g x y y y y y y y y y α β α β γ μυ μυ μαυβ μαυβ γε ε ε λ α β γ δ μαυβ γδ αμβλ γ δε ε ε ε η ε ε ε ε ε ± ± ± ± ± ±    = + −      + + +     R R R R R (3.1.11) where μυη is the Minkowski metric tensor, and the coefficients are all evaluated at 0y = . Defining now ( )( ) ( )( )( ) ( )( )1 4, , ,x x g x G x xε μυ εε εεε± ± ± ′ ′= −   (3.1.12) and its Colombeau-Fourier transform ( )( )kε ε ± by ( )( ) ( ) ( )( ), 2π d en n ik yx x k kε εε ε −± − ⋅ ±′ = ∫  (3.1.13) where k y k yαβ α βη⋅ = , one can work in a sort of localized momentum space. J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 405 Journal of High Energy Physics, Gravitation and Cosmology Expanding (3.1.10) in normal coordinates and converting to k-space, ( )( )kε ε ± can readily be solved by iteration to any adiabatic order. The result to adiabatic order four (i.e., four derivatives of the metric) is ( )( ) ( ) ( ) ( )( ) ( ) ( )( ) ( )( ) ( ) ( )( ) ( )( ) ( ) 1 22 2 2 2 22 2 ; 22 2 2 32 2 2 1 6 1 2 6 1 3 1 2 , 6 3 k k m k m i k m a k m a k m ε ε ε α α ε α β αβ ε λ λε ε ξ ε ξ ε ε ξ ε ε − −± ± − ± −± −± ±  = − − − −     + − ∂ −     − ∂ ∂ −    + − + −        R R R (3.1.14) where kαα∂ = ∂ ∂ , ( )( ) ( )( ) ( )( ) ( )( ) ( )( ) ( )( ) ( )( ) ( )( ) ( )( ) ( )( ) ; ; ; 1 1 1 2 120 140 1 1 30 60 1 , 60 a λαβ αβ αβ αβ λε ε ε ε λ κλ α λβ α β κλε ε ε ε λμκ α λμκβε ε ε ξ ε ε ε ε ε ε ε ε ε ± ± ± ± ± ± ± ± ± ±  − + −       − +     +    R R R R R R R R R (3.1.15) and we are using the symbol  to indicate that this is an asymptotic expansion. One ensures that Equation (3.1.13) represents a time-ordered product by performing the 0k integral along the appropriate contour in Figure 9. This is equivalent to replacing by . Similarly, the adiabatic expansions of other Green functions can be obtained by using the other contours in Figure 9. Substituting Equation (3.1.14) into Equation (3.1.13) gives [19] (3.1.16) Figure 9. The contour in the complex 0k plane  to be used in the evaluation of the integral giving + . The cross indicates the pole at ( )1 220 2k m= +k . 2m 2m i−  ( )( ) ( ) ( ) ( )( ( ) ( ) 12 2 0 2 1 22 2 , 2π d e , ; , ; , ; , n n ikyx x k k m a x x a x x a x x m m ε ε ε ε ε ε −−± − ± ± ± ′ ′= × −  ∂ ∂   ′ ′ + − +     ∂ ∂      ∫ J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 406 Journal of High Energy Physics, Gravitation and Cosmology where ( )( )0 , ; 1a x x εε ± ′ = and, to adiabatic order 4, ( )( ) ( )( ) ( )( ) ( )( ) ( )( ) ( )( ) ( )( ) 1 ; 2 2 1 1, ; 6 2 6 1 3 1 1 1, ; 2 6 3 ia x x y a y y a x x a α αε ε ε α β αβ ε λ λε ε ε ε ξ ε ξ ε ε ε ξ ε ε ± ± ± ± ± ± ±       ′ = − − −           −     ′ = − +     R R R (3.1.17) with all geometric quantities on the right-hand side of Equation (3.1.17) evaluated at x′ . In Equation (3.16), then the dnk integration may be interchanged with the ds integration, and performed explicitly to yield (dropping the i ). ( )( ) ( ) ( ) ( ) ( ) ( ) 2 2 2 0 , , 4π d exp , ; 2 1, . 2 n n x xx x i i s is im s x x is is x x y y ε ε ε ε α α σ σ ±∞ − −±  ′  ′ ′= − − +     ′ = ∫  (3.1.18) The function ( ),x xσ ′ which is one-half of the square of the proper distance between x and x′ , while the function ( )( ), ;x x isε ε′ has the following asymptotic adiabatic expansion ( )( ) ( )( ) ( )( ) ( ) ( )( )20 1 2, ; , ; , ; , ;x x is a x x is a x x is a x xε ε ε ε εε ε ε ± ± ± ±′ ′ ′ ′+ + +  (3.1.19) Using Equation (3.1.12), Equation (3.1.18) gives a representation of ( )( ),G x xε ε ± ′ : ( )( ) ( ) ( )( ) ( ) ( ) ( ) 2 21 2 0 2 , 4π , ; d , exp , ; 2 n nG x x i x x i s is x x im s x x is is ε εε ε ε ε σ ∞ − −± ±   ′ ′= − ∆   ′  ′× − +      ∫ (3.1.20) where ( )( ), ;x x εε± ′∆ is the distributional Van Vleck determinant ( )( ) ( ) ( ) ( )( )1 2, ; det , , , .x x x x g x g xμ νε εε σ ε ε −± ± ±  ′ ′ ′ ∆ = − ∂ ∂    (3.1.21) In the normal coordinates about x′ that we are currently using, ( )( ), ;x x εε± ′∆ reduces to ( )( )1 2,g x εε −± −  . The full asymptotic expansion of ( )( ), ;x x isε ε ± ′ to all adiabatic orders are ( )( ) ( ) ( )( )2 0 , ; , ;j j x x is is a x xε ε εε ∞ ± ± = ′ ′∑  (3.1.22) with ( )( )0 , ; 1a x x εε ± ′ = , the other ( )( ), ;ja x x εε ± ′ being given by canonical recursion relations which enable their adiabatic expansions to be obtained. Remark 3.1.1. Note that the Expansions (3.1.19) and (3.1.22) are, however, only asymptotic approximations in the limit of large adiabatic parameter T. J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 407 Journal of High Energy Physics, Gravitation and Cosmology If (3.1.22) is substituted into (3.1.20) the integral can be performed to give the adiabatic expansion of the Feynman propagator in coordinate space: ( )( ) ( ) ( ) ( ) ( ) ( ) ( ) 2 1 2 20 2 12 4 2 2 2 2 2 , 4π , ; , ; 2 2 j n jj n n G x x i x x a x x m m H m ε ε ε ε ε σ σ − ∞± ± ± = − −  ∂ ′ ′ ′− ∆ −  ∂        × −              (3.1.23) which, strictly, a small imaginary part i should be subtracted from σ . Remark 3.1.2. Since we have not imposed global boundary conditions on the distributional Green function Colombeau solution of (3.1.10), the expansion (3.1.23) does not determine the particular vacuum state in (3.1.9). In particular, the " i " in the expansion of ( )( ),G x xε ε ± ′ only ensures that (3.1.23) represents the expectation value, in some set of states, of a time-ordered product of fields. Under some circumstances the use of " i " in the exact representation (3.1.20) may give additional information concerning the global nature of the states. 3.2. Effective Action for the Quantum Matter Fields in Curved Distributional Space-Time As in classical case one can obtain Colombeau generalized quantity ( )Wε ε , called the effective action for the quantum matter fields in curved distributional spcetime, which, when functionally differentiated, yields ( )( ) ( ) ( )( )1 2 2 W gg ε μνμν ε ε δ ε δ εε     =   −  T (3.2.1) Note that the generating functional [ ]( ) [ ] ( ) ( ) ( ){ }( )exp dnZ D iS i x x xε ε ε ε εε εφ ε φ= + ∫mJ J (3.2.2) was interpreted physically as the vacuum persistence amplitude ( ),0 0,ε ε εout in . The presence of the external distributional current density ( )ε εJ can cause the initial vacuum state ( )0, ε εin to be unstable, i.e., it can bring about the production of particles. Following canonical calculation one obtains [19] [ ]( ) ( )( ) 1 20 det ,Z G x xε εε ε ± ±    ′∝ −      (3.2.3) where the proportionality constant is metric-independent and can be ignored. Thus we obtain ( ) [ ]( ) ( )( )ln 0 ln .2 iW i Z Gε ε εε ε ε ± ± ± = − = − − tr (3.2.4) In (3.2.4) ( )Ĝε ε± is to be interpreted as an Colombeau generalized operator which acts on an linear space I of generalized vectors ( ], , 0,1x ε ε ∈ normalized by J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 408 Journal of High Energy Physics, Gravitation and Cosmology ( ) ( ) ( ) 1 2, , ,x x x x g x ε ε ε ε δ ε −±  ′ ′= − −     (3.2.5) in such a way that ( )( ) ( ), , , .G x x x G xε εε εε ε± ±′ ′= (3.2.6) Remark 3.2.1. Note that the trace [ ]( )ε⋅tr of an Colombeau generalized operator ( )ε εR which acts on a linear space I , is defined by [ ]( ) ( ) ( ) 1 1 2 2 ; ;d , d , . n n xx xxx g x x g x x xε ε εε ε ε ε ε± ±         ′R = − R = − R           ∫ ∫tr (3.2.7) Writing now the Colombeau generalized operator ( )Ĝε ε± as ( ) ( )1 0  d exp ,G i s sε ε εεε ε ∞ ± ±− ±  = − = − −     ∫  (3.2.8) by Equation (3.1.20) we obtain ( ) ( ) ( )( ) ( ) ( )( ) 2 1 2 22 exp 4π , ; , exp , ; . 2 n n x s x i x x x x im s x x is is is ε ε ε ε σ −± ± −±    ′ ′− = ∆    ′  ′× − +      (3.2.9) Proceeding in standard manner we get [19] ( ) ( ) ( ) 2 1 2 22d , lim , ; d . 2 n x x m iW x g x G x x m mε εε ε ε ε ∞ ± ± ± ′→        ′= −             ∫ ∫ (3.2.10) Interchanging now the order of integration and taking the limit x x′→ one obtains ( ) ( ) ( ) 2 1 2 22d d , , ; . 2 n m iW m x g x G x x mε εε ε ε ∞ ± ± ±  = −      ∫ ∫ (3.2.11) Colombeau generalized quantity ( )Wε ε ± is colled as the one-loop effective action. In the case of fermion effective actions, there would be a remaining trace over spinorial indices. From Equation (3.2.11) we may define an effective Lagrangian density ( )( );L xε ε ± eff by ( ) ( ) ( ) 1 2 ;d , nW x g x L xε εε ε ε± ± ±    = −     ∫ eff (3.2.12) whence one get ( )( ) ( ) ( ) ( ) 2 1 2 22 ;, lim d , ; .2 x x m iL x g x x m G x x mε ε εε ε ε ε ∞ ± ± ± ± ′→      ′= − =          ∫ eff (3.2.13) 3.3. Stress-Tensor Renormalization Note that ( )( )L xε ε ± diverges at the lower end of the s integral because the 2sσ damping factor in the exponent vanishes in the limit x x′→ . (Convergence at the upper end is guaranteed by the i−  that is implicitly added J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 409 Journal of High Energy Physics, Gravitation and Cosmology to 2m in the De Witt-Schwinger representation of ( )( )L xε ε ± . In four dimensions, the potentially divergent terms in the DeWitt-Schwinger expansion of ( )( )L xε ε ± are ( )( ) ( ) ( )( ) ( ) ( ) ( ) ( ) ( ) ) 12 1 2 2 ; 3 0 2 0 1 2 ,d32π lim , ; exp 2 , ; , ; , ; x x x xsL x x x im s iss a x x isa x x is a x x ε ε ε ε σ ε ε ε ε ∞−± ±′→ ± ± ±  ′  ′= − ∆ − +        ′ ′ ′× + +  ∫div (3.3.1) where the coefficients 0a ± , 1a ± and 2a ± are given by Equation (3.1.17). The remaining terms in this asymptotic expansion, involving 3a ± and higher, are finite in the limit x x′→ . Let us determine now the precise form of the geometrical ( )( );L xε ε ± div terms, to compare them with the distributional generalization of the gravitational Lagrangian that appears in [19]. This is a delicate matter because (3.3.1) is, of course, infinite. What we require is to display the divergent terms in the form ∞ × geometrical object]. This can be done in a variety of ways. For example, in n dimensions, the asymptotic (adiabatic) expansion of ( )( );L xε ε ± eff is ( )( ) ( ) ( )( ) ( ) ( ) ( ) 21 1 2 ; 0 1 2 2 0 2 4π lim , ; , ; , d exp 2 n jx x j j n L x x x a x x x x i s is im s is ε ε ε ε ε ε σ ∞ −± − ±′→ = ∞ − −   ′ ′∆   ′  × − +      ∑ ∫ eff (3.3.2) of which the first 2 1n + terms are divergent as 0σ → . If n is treated as a variable which can be analytically continued throughout the complex plane, then we may take the x x′→ limit ( )( ) ( ) ( ) ( ) ( ) ( )( ) ( ) ( ) 2 1 21 2 ; 0 0 221 2 0 2 4π ; d exp 2 4π ; , ; , ; . 2 n j n j j n jn j j j j L x a x i s is im s na x m j a x a x x ε ε ε ε ε ε ε ∞∞ − − −± − = ∞ −−− =    −      = Γ − =    ∑ ∫ ∑ eff (3.3.3) From Equation (3.3.3) it follows we shall wish to retain the units of ( );L xε± eff as (length)−4, even when 4n ≠ . It is therefore necessary to introduce an arbitrary mass scale μ and to rewrite Equation (3.3.3) as ( )( ) ( ) ( )( ) 4 4 221 2 ; 0 2 4 ; . 2 n jn j j m nL x a x m jε ε ε π ε μ − ∞ −−± − =     Γ −          ∑eff (3.3.4) If 4n → , the first three terms of Equation (3.3.4) diverge because of poles in the Γ-functions: ( ) ( ) ( ) ( ) ( ) 4 2 4 , 4 2 4 4 21 4 , 2 2 4 22 4 . 2 4 n O n n n n n O n n n n O n n γ γ γ    Γ − = − + −   − −       Γ − = − + −   − −     Γ − = − + −  −  (3.3.5) J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 410 Journal of High Energy Physics, Gravitation and Cosmology Denoting these first three terms by ( )( );L xε ε ± div , we have ( )( ) ( ) ( ) ( ) ( ) ( ) 2 2 ; 2 4 2 0 1 2 1 14π ln 4 2 4 ; 2 ; ; . 2 2 n mL x n m a x m a x a x n n n ε ε ε γ μ ε ε ε −±     = + +   −          × − +   − −    div (3.3.6) The functions ( ) ( )0 1; , ;a x a xε ε and ( )2 ;a x ε are given by taking the coincidence limits of (3.1.17) ( )( ) ( )( ) ( )( ) ( )( ) ( ) ( )( ) ( ) ( )( ) ( )( ) ( )( ) 0 1 2 , 2 1; 1, ; , 6 1; , , 180 1 , , 180 1 1 , 6 5 1 1 , . 2 6 x a x a x a x x x x x x x ε ε ε αβγδ αβγδε ε αβ αβ ε ε ε ε ε ε ξ ε ε ε ε ε ε ξ ε ξ ε ± ± ± ± ± ± ± ± ± ±  = = −    = −  − −     + −    R R R R R R R  (3.3.7) Finally one obtains [19] ( )( ) ( ) ( ) ( ) 2 3 ; 2 3 0 1 d ln , ; e . 64π ismL x i s is x x is is ε εε ε ∞ ± ± −  ∂   −   ∂  ∫ ren (3.3.8) Remark 3.3.1. All the higher order ( )2j > terms in the DeWitt-Schwinger expansion of the effective Lagrangian (3.3.4) are infrared divergent at 4n = as 0m → , we can still use this expansion to yield the ultraviolet divergent terms arising from 0,1j = and 2 in the four-dimensional case. We may put 0m = immediately in the 0j = and 1 terms in the expansion, because they are of positive power for ~ 4n . These terms therefore vanish. The only nonvanishing potentially ultraviolet divergent term is therefore 2j = : ( ) ( ) 4 21 22 4π , 2 ,2 n n m na x ε μ − −−    Γ −       (3.3.9) which must be handled carefully. Substituting for ( )2a x with ( )nξ ξ= from (3.3.7), and rearranging terms, we may write the divergent term in the effective action arising from (3.3.9) as follows ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) 4 1 21 2 , 2 4 21 1 2 2 4π 2 d , , 2 2 4π 2 2 d , 4 , n n n n n n m nW x g x a x m n x g x x G x O n ε ε ε ε ε ε ε ε μ μ ε α β − −± − ± − −− ± ± ±       = Γ − −              = Γ −           × − + + −       ∫ ∫  div (3.3.10) J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 411 Journal of High Energy Physics, Gravitation and Cosmology where ( )( ) ( ) ( )( ) ( ) ( )( ) ( )( ) ( )( ) ( ) ( )( ) 2 , , 2 , , 1 , , 3 , , , 1 1, . 120 360 x x x x x x G x x x αβγδ αβ ε αβγδ αβε ε ε ε αβγδ ε αβγδε ε ε ε ε ε ε ε ε α β ± ± ± ± ± ± ± ± = − + = = = − R R R R R R R  (3.3.11) Finally we obtain [19] ( )( ) ( ) ( ) ( ) ( )( ) ( ) ( ) ( )( ) ( ) ( )( ) ( )( ) 2 , 2 , , 2= 1 2880π , 3 1 2880π , , , , , . x x T x x x G x x x x x x μ μ ε ε ε ε ε ε αβγδ αβγδ ε αβ αβ εε ε ε α ε β ε ε ε ε ε ± ± ± ± ± ± ±   − − +      = − ×  − −       ren R R R R R R (3.3.12) Therefore for the case of the distributional Schwarzchild spesetime using Equation (2.2.4) and Equation (3.3.12) ( ) ( ) ( ]0,2 , 1r mε ε ηε ε η∈− ≈   , see Appendix C, Remark C.10, Equation (C22), we obtain ( )( ) ( ) ( ) ( )( ) ( ) 11 22 1 2 2 1 22 2 , 2880 π 16 2 1 2880 16 π 2 . T r m r m O m r m μ μ ε ε ε ε ε ε −− − − −−    ≈ − ⋅ − + +      ≈ − ⋅ ⋅ −     ren (3.3.13) Finally from Equation (3.3.13) for ( ]2 0, , 1r m η η− ∈  , see Appendix C, Remark C.10, Equation (C22), we obtain ( )( ) ( ] ( ) ( ) ( ) ( ] 1 22 2 2 0,2 0, , 1 2880 16 π 2 .r mr m T r O m r mμμ ηη ε − −− − ∈− ∈ ≈ − ⋅ ⋅ − ren (3.3.14) Remark 3.3.2. Thus QFT in distributional curved spacetime predict that the infalling observer burns up at the BH horizon. Remark 3.3.3. In order to avoid singularity at horizon 2r m= in Equation (3.3.13) one have to apply the Loop Quantum Gravity approach [41]-[46]. The first one concerns the requirement of selfadjointness to the metric components. For instance, the classical quantity ( ) 2 , 22 1 x tx x x E K g GmE K E φ φ ′ = − + − (3.3.14) defined as an evolving constant (i.e. a Dirac observable), must correspond to a selfadjoint operator at the quantum level. Classically, Kφ and xE are pure gauge, and txg is just a function of the observable m. In the interior of the horizon, if txg is a selfadjoint operator, a necessary condition will be [41]-[46] 2 21 0. j GmK l kφ + − ≥ P (3.3.15) J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 412 Journal of High Energy Physics, Gravitation and Cosmology At the singularity, i.e. 1j = , and owing to the bounded nature of 2Kφ < ∞ , ( )1 2 2 0. 1 Gmk l Kφ ≥ > +P (3.3.16) Therefore, this argument strongly suggests that the classical singularity will be resolved at the quantum level since 1k must be a non-vanishing integer. Remark 3.3.4. Let ( ) H T rμν ren be ( )0 0 H HT rμν ren , where 0 H is the Hartle-Hawking vacuum state [37]. Notice that the main feature of the tensor ( ) ( ) H T r T rμ μν ν ren formally calculated in classical literature (see, for example, [37] chapter 11.3) is that its components are finite on the event horizon r+ . An observer at rest at a point r close to the event horizon records the local energy density ( ) ttT r= − . This quantity remains finite as r r+→ . On the other hand, the temperature measured by the such observer is ( ) 1 2 1 , 2π rkr r − + Θ = +    loc (3.3.17) grows infinitely near the horizon [37]. The local temperature can be measured by using a two-level system as a thermometer. Transitions between levels are caused by the absorption and emission of quanta of the fields (photons). After a sufficiently long exposure, the probability for a system to occupy the upper level will be less than that for the lower level by a factor ( )( )exp E r∆ Θloc , where E∆ is the energy difference between the levels. It is well known that the temperature in the vicinity of r+ is 2πa aθΘ ≈ =loc , where a is the observer's acceleration [37]; as ( ), .r r r+→ Θ →∞loc The radiation energy density ε in the neighborhood of such a point is [37] ( )4 42π .akσ σθ  (3.3.18) Therefore Stefan-Boltzmann law under formal calculation by using classical Schwarzschild geometry is evidently violated. Let us remind that the acceleration i ia a a= of free fall of a body which is initially at rest in the Schwarzschild reference frame is [37] ( ) 1 2 2 . 21 ma r mr r =  −    (3.3.19) The acceleration points along the radius and is directed toward the center; as 2r m→ : ( ) ( )1 2 2 . 4 2 ma r m r m = − (3.3.20) From Equation (3.3.20) and Equation (3.3.14) as ( ]2 0, , 1r m η η− ∈  , see Appendix C, Remark C.10, Equation (C22), we obtain: ( ) ( ] ( )( ) ( ] 4 22 2 0, 2 0, , . 64 2 a r m r m T r m r m μ μ η η σσθ ε − ∈ − ∈ = − − ren  (3.3.21) J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 413 Journal of High Energy Physics, Gravitation and Cosmology Therefore Stefan-Boltzmann law under rigorous calculation by using distributional Schwarzschild geometry evidently is not violated. 3.4. Unruh Effect Revisited We remind now that a black holes have an approximate Rindler region near the Schwarzschild horizon. For the the distributional Schwarzschild solution (2.1.8) by coordinate transformation ( )( ) ( ]2 22 1 , 0,1 ,r m εδ ε ε= + + ∈ (3.4.1) we obtain ( ) ( )( )2 2 2 2 2 2 2 22d d 16 d 4 ds t m mε ε εδ ε δ= − + + + Ω + (3.4.2) The ( ),t δ piece of this metric (3.4.2) is Rindler space (we can rescale t , δ and ε to make it look exactly like (2.2.10). Thus from (3.3.13) using (3.4.1) we obtain directly for 0δ  ( )( ) 4 0 , .T μμ ε δ ε δ − ren   (3.4.3) Therefore, sufficiently strongly accelerated observer burns up near the Rindler horizon. Thus, Polchinski's account is not a violation of the Einstein equivalence principle. Remark 3.4.1. Note that by using Equation (A.8) and Equation (A.9) (see Appendix A) one obtains Equation (3.4.3) directly from distributionel Möller metric (1.2.13) and distributionel Rindler metric (2.2.10). ( )( ) ( ) ( ) ( ) 4 22 2 4 1 , . g O T x a gx μ μ ε ε ε ε −  + +  ren  (3.4.4) The Unruh effect is the prediction that an accelerating observer will observe blackbody radiation where an inertial observer would observe none. The Unruh effect was first described by Stephen Fulling in 1973, Paul Davies in 1975 and W. G. Unruh in 1976 [47]. The Unruh temperature, derived by William Unruh in 1976, is the effective temperature experienced by a uniformly accelerating detector in a vacuum field. It is given by [47]: , 2 B gT cπ κ =  (3.4.5) where g is the local acceleration, Bκ is the Boltzmann constant,  is the reduced Planck constant, and c is the speed of light. Thus, for example, a proper acceleration of 2.47 × 1020 m/sec2 corresponds approximately to a temperature of 1 K. Notice that for a proper acceleration of 2.47 × 1020 m/sec2 the event horizon very close to observer by distance 1 2748horx ≅ . 2m−1 = 3. 6387 × 10−4 m. It is currently not clear whether the Unruh effect has actually been observed, since the claimed observations are disputed. There is also some doubt about whether the Unruh effect implies the existence of Unruh radiation. Although Unruh's prediction that an accelerating detector would see a thermal bath is not J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 414 Journal of High Energy Physics, Gravitation and Cosmology controversial, the interpretation of the transitions in the detector in the nonaccelerating frame is. It is widely, although not universally, believed that each transition in the detector is accompanied by the emission of a particle, and that this particle will propagate to infinity and be seen as Unruh radiation. The existence of Unruh radiation is not universally accepted. Some claim that it has already been observed [48], while others claim that it is not emitted at all [49]. While the skeptics accept that an accelerating object thermalizes at the Unruh temperature, they do not believe that this leads to the emission of photons, arguing that the emission and absorption rates of the accelerating particle are balanced. By the Einstein equivalence principle Stefan-Boltzmann law holds near the Mӧller horizon. Therefore by Equation (3.4.4) and Stefan-Boltzmann law the temperature measured by the observer located near the Mӧller horizon is ( ) 11 .T g gx −+ (3.4.6) Thus observer with a proper acceleration of 2.47 × 1020 m/sec2 burns up near the Mӧller horizon. 4. Conclusion On a Riemannian or a semi-Riemannian manifold, the metric determines invariants like the Levi-Civita connection and the Riemann curvature. If the metric becomes degenerate (as in singular semi-Riemannian geometry), these constructions no longer work, because they are based on the inverse of the metric, and on the related operations like the contraction between covariant indices. In order to avoid these difficulties distributional geometry by using Colombeau generalized functions [3]-[10]. In authors papers [18] [19] appropriate generalization of classical GR based on Colombeau generalized functions is proposed. Such generalization of classical GR based on appropriate generalization of the Einstein equivalence principle (GEEP) is mentioned above in subsection 2.3. Using Rindler distributional geometry Unruh effect revisited. We pointed out that GEEP avoid the contradiction which was mentioned by Z. Merali in paper [47], and therefore Polchinski's account [1] doesn't violates the Einstein equivalence principle. Acknowledgements We thank the Editor and the referee for their comments. 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DOI: 10.4236/jhepgc.2018.42023 418 Journal of High Energy Physics, Gravitation and Cosmology Appendix Appendix A1 Let us introduce now Colombeau generalized metric which has the form ( ) ( )( )( ) ( )( ) ( ) ( )( )( )( ) ( ) ( ) ( )( ) 2 22 0 0 2 22 2 d d 2 d d d d sin d , . s A r x D r x r B r C r r B r r r ε ε ε ε εε ε εε ε ε θ θ φ = − − + +  + + ∈   (A1.1) The Colombeau scalars ( )( ) ( ) ( )( ), , , ,r r rμν μνε εε ε εR R R and ( ) ( )( ), ,r rρσμν ρσμν εε εR R , in terms of Colombeau generalized functions ( )( ) ( )( ) ( )( ) ( )( ), , ,A r B r C r D rε ε ε εε ε ε ε are expressed as ( )( ) 2 2 2 2 2, 2 3 1 12 2 , 2 2 A A B A C D Ar r A B A B Ar B B A B A B B B A B A B ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε    ′ ′ ′  ′′∆ + = − − + + −    ∆ ∆   ′′  ′  ′ ′  ′ ′  ′∆ − + − + +    ∆       R ( ) ( )( ) 22 2 2 2 2 2 2 2 2 , , 1 1 1 1 2 4 2 1 1 12 2 2 1 1 1 1 1 2 2 4 2 4 r r A A A A B A A A A B r A A A B A C D r A B A Br A B B B A A A B B B A μν μν ε ε ε ε ε ε ε ε ε ε ε ε εε ε ε ε ε ε ε ε ε ε ε ε ε εε ε ε ε ε ε ε ε ε ε ε ε ε εε ε ε ε   ′′ ′ ′ ′ ′ ′ ∆ = − + +  ∆∆       ′ ′ ′ ∆ + + − − +    ∆∆    ′ ′ ′′ ′ ′  ′′ ′∆ − − + + − ∆ ∆  R R 22 1 1 1 1 2 , 2 2 2 A A A B B B B A B A B B B B r A B ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε   ′∆   ∆ ′ ′ ′′  ′  ′ ′  ′ ′ ′ ∆ ∆ + + − − + − +     ∆ ∆      ( ) ( )( ) 2 22 2 2 2 222 2 2 2 2 2 , , 1 1 12 2 2 1 1 14 4 1 12 2 2 r r A A A A A A B A A r A A B A B A C D B r B A B Br A A B A B B r A B A B B ρσμν ρσμν ε ε ε ε ε ε ε ε ε ε ε ε ε ε εε ε ε ε ε ε ε ε ε ε ε εε ε ε ε ε ε ε ε ε ε ε ε ε εε ε ε   ′′ ′ ′   ′ ′ ′ ∆= − + +    ∆∆ ∆     ′  ′ + + − +   ∆       ′ ′ ′  ′ ′ ′′∆ + + − + +  ∆∆   R R ( ) 22 2 1 1 . 2 2 B B B B A B C D ε ε ε ε ε ε ε ε ε ε ε ε  ′  ′ ′∆ − −   ∆      ∆ = + + (A1.2) Remark A1.1. Note that the Colombeau scalars ( )( ) ( ) ( )( ), , , ,r r rμν μνε εε ε εR R R and ( ) ( )( ), ,r r ρσμν ρσμν ε ε εR R can be extended on Colombeau generalized numbers ( )rε ε = ∈  r as corresponding generalized point value (see Definition 1.5.4) by formulas: J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 419 Journal of High Energy Physics, Gravitation and Cosmology ( )( ) ( )( ) ( ) ( )( ) ( ) ( )( ) ( ) ( )( ) ( ) ( )( ) (i) , , , (ii) , , , , (iii) , , , , . r r r r r εε ε μν μν μν ε μν εε ε ρσμν ρσμν ρσμν ε ρσμν εε ε ε ε ε ε ε ε ε ε ε ε                          R r R R r R r R R R r R r R R (A1.3) The distributional Mӧller's metric is ( ) ( )( ) ( ) ( ) ( ] 2 2 2 2 2 2 2 d d d d d , , 0,1 . s A x t x y z A x a gx ε εε ε ε ε ε = − + + +  = + + ∈  (A1.4) In order to aply Equation (A1.2) directly we chose now ( ),g g θ φ= , where angles ,θ φ correspond to spherical coordinates: sin cosx r θ φ= sin sin , cosy r z rθ φ θ= = . In spherical coordinates we get ( ) ( )( )( ) ( ) ( ) ( ) ( ] ( ) ( ) ( ) ( ) 2 2 2 2 2 2 2 2 2 2 2 2 d , d d d , d d sin d , , sin cos , , 0,1 , 2 , 2 , , . s A r t r r A r a g r A r g a g r A r g ε εε ε ε ε ε η θ φ θ θ φ η θ φ θ φ η η ε ε η η η η η η θ φ = − + + Ω Ω = + =  = + + ∈  ′ ′′= + = = (A1.5) We choose now in the Equation (A1.2): ( ) ( )1, 0B r C rε ε= = , and ,g g constη = ∗ = sin cos 0θ φ ≠ and rewrite Equation (A1.5) in the following equivalent form ( ) ( )( ) ( ) ( ) 2 2 2 2 2 2 2 d d d d , . s A r t r r A r a gr ε εε ε ε ε = − + + Ω = + + (A1.6) Note that ( ) .A B C Aε ε ε ε ε∆ = + = (A1.7) From Equations (A1.5)-(A1.7) by Equation (A1.2) we get ( )( ) 2 2 2 , 2 22 3 1 12 2 2 2 r A A B A C D A r A B A B Ar B B A B A B B B A B A B ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε   ′ ′ ′ ′′ ∆ + = − − + + −    ∆ ∆   ′′ ′ ′ ′ ′ ′ ′    ∆ − + − + +    ∆       R ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) 2 2 222 2 22 22 2 2 2 2 2 2 2 2 22 222 2 2 1 2 4 22 4 22 A A A r A A A g a gr g a grg a grr a gr a gr a gr g a gr gg a grr a gra gr ε ε ε ε ε ε ε ε ε εε ε ε ε εεε  ′ ′′ ′ = − − +      + +  = − − +   + ++ +   + +        + + − +  = − −   + ++ +  + +         J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 420 Journal of High Energy Physics, Gravitation and Cosmology ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) 2 2 2 2 2 2 222 222 2 2 2 2 2 22 2 42 2 2 42 . g a grg g g a gr a grr a gra gr g a grg r a gra gr ε ε ε ε εεε ε εε   +−  = + − −  + + + ++ +  + +       +−  = −  + +  + +                   (A1.8) From Equation (A1.8) in the limit 0a g rε ∗+ → we get ( )( ) ( ) ( ) 2 2 22 2 2, , 0.gr a g r a g r ε εε ε ε ε ε ε ε ∗ ∗ ∗    −  ≈ + ≈     + +       R (A1.9) Remark A1.2. Note that: (1) Equation (1.2.14) in a nice agriment with Equation (A1.9), see Remark 1.2.2-Remark 1.2.4. (2) For ( )r rε ε= located beyond horizon, i.e. 0a g r∗+ ≈/  one obtains classical result ( )( ) ( )( )2 2, 0,r O gε εε ε ∗≈ ≈   R (A.1.10) see Definition 1.5.2. (i). (3) At horizon : 0hor horr r a g rε ∗= + = from Equation (A1.9) one obtains nonclassical result ( )( ) ( )( )2 2, ,horr O gε εε ε ∗ −≈ ≈ ∞   R   (A1.11) see Definition 1.5.2. (ii). Remark A1.3. Let ( ) 0a g rε ε ∗ + ≈   , then from Equation (A1.3) and Equation (A1.9) we obtain ( )( ) ( ) 2 2 22 2 2, .gr a g r ε ε ε ε εε ε ∗ ∗      −   ≈       + +        R  (A1.12) From Equations (A1.5)-(A1.7) by formulae (A1.2) we get ( ) ( )( ) 22 2 2 2 2 2 2 2 2 , , 1 1 1 1 2 4 2 1 1 12 2 2 1 1 1 1 1 2 2 4 2 4 r r A A A A B A A A A B r A A A B A C D r A B A Br A B B B A A A B B B A μν μν ε ε ε ε ε ε ε ε ε ε ε ε εε ε ε ε ε ε ε ε ε ε ε ε ε εε ε ε ε ε ε ε ε ε ε ε ε ε εε ε ε ε  ′′ ′ ′ ′ ′ ′ ∆ = − + +  ∆∆      ′ ′ ′ ∆ + + − − +    ∆∆    ′ ′ ′′ ′ ′ ′′ ′∆ − − + + − ∆ ∆  R R 22 1 1 1 1 2 2 2 2 A A A B B B B A B A B B B B r A B ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε  ′ ∆   ∆ ′ ′ ′′ ′ ′ ′ ′ ′ ′   ∆ ∆ + + − − + − +     ∆ ∆      J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 421 Journal of High Energy Physics, Gravitation and Cosmology 22 2 2 22 2 1 1 1 1 1 12 2 4 2 1 1 1 2 4 1 1 1 12 2 4 2 A A A A A A r A r A r A A A A A r A A A A A r A rA ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε εε ε     ′′ ′ ′ ′ ′ ′   ∆ ∆  = − + + − −       ∆ ∆           ′′ ′ ′ ′ ′ ∆ ∆ + − + −   ∆ ∆       ′′ ′ ′ = − + + −     2 22 2 1 1 2 4 A A A A A A ε ε ε ε ε ε ε ε  ′          ′′ ′ + −     ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) 2 222 2 2 22 22 2 2 2 22 2 222 2 22 2 2 4 21 2 1 1 2 4 21 12 2 41 2 1 2 4 g a gr g a grg ra gr a gra gr g a gr r ra gr g a grg a gr a gr ε ε ε εε ε ε ε    + + = − +   + + + + + +         + + − −    + +        + + −  + +  + +                     . ε   (A1.13) From Equation (A1.13) in the limit 0a g rε ∗+ → we get ( ) ( )( ) ( ) ( ) ( ) 4 4 42 2 4 1 , , , 0. g O r r a g r a g r μν ε μν ε εε ε ε ε ε ε ε ε ∗ ∗ ∗     ≈ + ≈    + +       R R (A1.14) Remark A1.4. At horizon : 0hor horr r a g rε ∗= + = from Equation (A1.14) one obtains nonclassical result ( ) ( )( ) ( )( )2 4, , ,hor horr r O gμν μν ε εε ε ε ∗ −≈ ≈ ∞   R R (A1.15) see Definition 1.5.2. (ii). Remark A1.5. Let ( ) 0a g rε ε ∗ + ≈   , then from Equation (A1.3) and Equation (A1.14) we obtain ( ) ( )( ) ( ) ( ) 4 4 42 2 4 1 , , . g O r r a g r μν ε μν ε ε ε ε ε ε ε ε ∗ ∗          ≈       + +       R R (A1.16) From Equation (A1.4)-Equation (A1.6) by formulae (A1.2) we get ( ) ( )( ) 2 22 2 2 2 , , 1 1 1= 2 2 2 r r A A A A A A B A A r A A B ρσμν ρσμν ε ε ε ε ε ε ε ε ε ε ε ε ε ε εε ε ε ε  ′′ ′ ′ ′ ′ ′   ∆ − + +    ∆∆ ∆    R R J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 422 Journal of High Energy Physics, Gravitation and Cosmology 222 2 2 2 222 2 22 2 2 2 1 1 14 4 1 1 1 12 2 2 2 2 1 1= 2 2 A B A C D B r B A B Br A A B A B B B B r A B A B B B B A A A A rA A ε ε ε ε ε ε ε ε ε εε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε εε ε ε ε ε ε ε ε ε  ′ ′ +  + − +   ∆      ′ ′ ′ ′ ′ ′′ ′ ′ ′   ∆ ∆ + + − + + − −     ∆ ∆∆            ′′ ′ ′ − +       ε   ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) 2 22222 2 2 22 22 2 2 2 22 2 2 22 2 222 2 822 1= 2 82 1= g a g rg a grg ra g r a g r a g r g a g r g a g rg ra g r a g r εε ε ε ε ε ε ε ε ε ∗ ∗ ∗ ∗ ∗ ∗ ∗ ∗ ∗∗ ∗ ∗         ++ − +           + + + + + +                   + + −  +   − +     + + + +          ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) 2 22 2 2 22 22 2 2 2 2 22 2 22 2 22 22 2 24 4 42 2 22 2= 81 84 1= a g r g a grg g a gr a gr a gr g a gr r a gr g ag ra gr ε ε ε ε ε ε ε ε ε ε ε ε ε ∗         + +        + +   − +   + +     + + + +          +  +     + +      +  +    + +                 ( ) ( ) 2 22 2 gr a gr ε ε         + +      (A1.17) In the limit 0a g rε ∗+ → from (A1.12) we get ( ) ( )( ) ( ) ( ) 4 4 42 2 4, , , 0. gr r a g r a g r ρσμν ρσμν ε ε ε ε εε ε ε ∗ ∗ ∗     ≈     + +     + ≈   R R   (A1.18) Remark A1.6. At horizon : 0hor horr r a grε = + = from Equation (A1.18) one obtains nonclassical result ( ) ( )( ) ( )( )2 4, , ,r r O gρσμν ρσμν ε εε ε ε ∗ −≈ ≈ ∞   R R (A1.19) see Definition 1.5.2. (ii). Remark A1.7. Let ( ) 0a g rε ε ∗ + ≈   , then from Equation (A1.3) and Equation (A1.18) we obtain J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 423 Journal of High Energy Physics, Gravitation and Cosmology ( ) ( )( ) ( ) 4 4 42 2 4, , .gr r a g r ρσμν ε ρσμν ε ε ε ε εε ε ε ∗ ∗          ≈       + +       R R (A1.20) Remark A1.8. We assume now there exist a fundamental generalized length ( )lε ε ( ) ( ] ( ) ( ] ( ) ( ] 0,0, ,1 , 1,l b l a ε ε ηε η ε ε η ε η ∈∈ ∈ = × =  (A1.21) such that ( ) ( ) ( ) ,a g r l b bε ε εεε ε ∗+ ≥ = × ∈ . It mean there exist a thickness ( )horth lε ε= of horizon. We introduce a norm horth of a thickness horth by formula ( ]0,sup ,horth lεε η η∈= = (A1.22) where parameter η is a classical thickness of horizon. By using (A1.21) we get the estimate ( ) ( )( ) ( ) ( ] ( ) ( ] ( ) ( ] ( ) ( ] ( ) 4 4 42 2 0, 4 2 2 22 22 0,0, 2 2 2 0, 4 2 22 2 2 4, , 4 1 4 1 gr r a g r g a g ra g r a g r g b a g r ρσμν ε ρσμν ε ε ε η ε ηε η ε η εε ε ε ε εε ε ε ε ∗ ∗ ∈ ∗ ∗∗ ∈∈ ∗ ∈ ∗ ∗     ≈     + +             = ×       + + + +              ×  + +       ≤     + + +     R R ( ] ( ) ( ] 0, 4 2 22 4 0, 1 4 . 1 a g r g b a g r ε η η∗ ∈ ∗ ∗ + ∈            =       + +       (A1.23) Appendix A2 Let us consider now distributional Colombeau metric given by Equation (1.3.30) with 1c = ( ) ( )( ) ( ) ( ) 2 2 4 2 2 2 2 2 2 2d d 1 d d sin d , r s t r r rr ε ε ε ρ ε ρ θ θ φ ρ − +    = − + + + +    + (A2.1) where ( ]0,1ε ∈ , 4srρ = , sr is a schwarzschild radius. J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 424 Journal of High Energy Physics, Gravitation and Cosmology We choose now ( ) ( ) 0D r C rε ε= = , and rewrite Equation (A2.1) in the following equivalent form ( ) ( )( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( )( ) 2 2 2 2 2 2 42 2 2 2 2 2 d d d , , 1 , 1, , , . 2 2 2 , d s A r t B r r r r A r B r rr A A B A B A B B A B A B A B A B A B rA A r r ε εε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ρ ε ρ ρ ε ρ ρ ρ ρ ε  = − + + Ω  − +  = = +   + ′ ′ ′∆ = = ∆ = + ∆ ′ ′ ′ ′ ′∆ + = = + ∆ + −′ = − + − + ( ) ( ) ( )( ) ( ) ( ) ( ) ( )( ) ( ) ( ) ( )( ) ( ) ( ) ( )( ) ( ) ( ) ( )( ) ( ) ( )( ) ( ) ( )( ) 22 22 2 4 2 2 22 2 2 22 2 22 2 24 2 22 2 2 22 2 4 2 2 2 2 22 2 2 2 2 22 2 2 22 4 2 2 4 16 16 164 16 4 16 16 16 , 2 3 8 4 r r rA A r r r r rr r r r r r r rr r r r rA A ε ε ε ε ε ρ ρ ε ρ ρ ρ ρ ρ ρ ε ρ ρ ε ρ ρ ε εε ρ ρ ρ ρ ε ρ ρ ε ε ρ ρ ρ ρ ρ ερ ρ ε ρ ε ρ ρ ε ε ρ + − + − + − ′ = =    + − + + − +  − + −+ −  = + + − + + − + + − = + + − ++ − + − + − + + −′′ = ( ) ( ) ( )2 2 2 . r r ρ ρ ρ ε + − +    (A2.2) We assume now that r ρ , then from Equation (A2.2) we obtain ( )( ) ( )( ) ( ) ( )( ) ( ) ( )( ) ( ) ( ) ( ) ( ) ( ) 2 2 2 2 4 2 2 22 22 22 2 2 2 2 22 22 2 2 2 2 2 22 2 2 2 2 22 2 2 4 4 , 3 4 2 , 2 1 2 2 2 2 2 . A A r A A rr r A A rr A A A A r r r r ε ε ε ε ε ε ε ε ε ε ε ρ ρ ε ε ε ρ ερ ρ ε ρ ε ε ρ ρ ερ ρ ε ε ρ ε ρ ε ρ ε ε ρ ε ′ − − +  ′ + −   − +  − + − +  +′′ − +− +  ′′ ′ − + − + −  − + − +    − +  = −  − +       (A2.3) J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 425 Journal of High Energy Physics, Gravitation and Cosmology From Equation (A2.3) by formulae (A1.2) we get ( )( ) 2 2 2, 2 3 2 1 12 2 2 1 2 2 2 1 12 2 2 A A B A B r r A B A B B A B A B B A B A B A B A B B r A B A B B A B B A B ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε   ′ ′ ′ ′′ ′′ ∆ = − − + − −    ∆ ∆   ′ ′ ′ ′ ′ ′    ∆ + − + +    ∆         ′ ′ ′′ ′′  = − − − −       ′ ′ ′  + − +    R A B A B A B A B ε ε ε ε ε ε ε ε ε ′ ′ ′ ′   + +       ( ) ( )2 2 2 2 1 2 2 2 1 3 1 . 2 2 2 A B A B B r A B A B A B A B A B A B ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε    ′ ′ ′′ ′′ = − − − −       ′ ′ ′ ′ + + −   (A2.4) From Equation (A2.4) in the limit rε ρ→ by formulae (A2.3) we get ( )( ) ( ) 2 22 2 2, .r r ε ε ε ε εε ρ ε     ≈ −   − +    R (A2.5) Remark A2.1. Note that: (1) Equation (A2.5) in a nice agriment with Equation (A1.9). For ( )r rε ε= located beyond horizon, i.e. 0r ρ− ≈/  one obtains classical result ( )( ) ( )( )2, 1 0,r Oε ε εε ε≈ ≈  R (A2.6) see Definition 1.5.2. (i). (3) At horizon : 0hor horr r rε ρ= − = from Equation (A2.5) one obtains nonclassical result ( )( ) ( )( )2, 1 ,horr Oε εε ε −≈ ≈ ∞   R (A2.7) see Definition 1.5.2. (ii). Remark A2.2. Let ( ) 0rε ερ − ≈   , then from Equation (A1.3) and Equation (A2.5) we obtain ( )( ) ( ) 2 22 2 2, .r r ε ε ε ε ε ε ρ ε        ≈ −      − +     R (A2.8) From Equation (A2.3) by formulae (A1.2) we get ( ) ( )( ) 22 2 22 2 , , 1 1 1 1 2 4 2 1 1 1 1 12 2 2 2 2 4 ' r r A A A A B A A A A B r A A A B A B B B r A B A B B B μν μν ε ε ε ε ε ε ε ε ε ε ε ε ε εε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε εε ε ε ε  ′′ ′ ′ ′ ′ ′ ∆ = − + +  ∆∆       ′ ′ ′ ′ ′′ ′ ′ ∆ ∆ + − − − − +     ∆ ∆∆     R R J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 426 Journal of High Energy Physics, Gravitation and Cosmology 22 2 2 1 1 1 1 2 4 2 2 1 1 2 2 A A A A B B B A A A B B B B A B B r A B ε ε ε ε ε ε ε ε ε ε ε ε ε ε εε ε ε ε ε ε ε ε ε ε ε ε   ′′ ′ ′ ′ ′ ′′ ′ ∆ + − + + −   ∆∆    ′ ′ ′ ′ ′ ∆ ∆ − + − +   ∆ ∆    2 2 2 2 2 2 1 1 1 1 1 2 4 2 1 1 12 2 2 1 1 1 2 2 4 1 2 A A A B A B A A A A B A B r AB A B A B r A B A BB A B B B A B A B B B A B A ε ε ε ε ε ε ε ε ε ε ε ε ε εε ε ε ε ε ε ε ε ε εε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε   ′′ ′ ′ ′ ′ ′ ′  = − + + +           ′ ′ ′ ′  + + − −         ′ ′ ′′ ′ ′ ′  − − + +      ′ + ∆ 22 1 1 4 2 1 1 1 . 2 2 A A A B A B A A A B A B B B B B B B B r B ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε   ′ ′ ′ ′ ′ ′  − + +       ′′ ′ ′ ′ ′  ∆ + − − +  ∆      (A2.9) From Equation (A2.9) in the limit rε ρ→ by formulae (A2.3) we get ( ) ( )( ) ( ) 4 42 2 , , .r r r μν μν ε ε ε εε ε ρ ε     ≈    − +    R R (A2.10) Remark A2.3. Note that: (1) For ( )r rε ε= located beyond horizon, i.e. 0r ρ− ≈/  one obtains classical result ( ) ( )( ) ( )( )4, , 1 0,r r Oμν ε μν ε ε εε ε ε≈ ≈  R R (A2.11) see Definition 1.5.2. (i). (2) At horizon : 0hor horr r rε ρ= − = from Equation (A2.10) one obtains nonclassical result ( ) ( )( ) ( )( )4, , 1 ,hor horr r Oμν μν ε εε ε ε −≈ ≈ ∞   R R (A2.12) see Definition 1.5.2. (ii). Remark A2.4. Let ( ) 0rε ερ − ≈   , then from Equation (A1.3) and Equation (A2.10) we obtain ( ) ( )( ) ( ) 4 42 2 , , .r r r μν ε μν ε ε ε ε εε ε ρ ε        ≈       − +     R R (A2.13) From Equation (A2.3) by formulae (A1.2) we get ( ) ( )( ) 2 22 2 2 2 , , 1 1 12 2 2 r r A A A A A A B A A r A A B ρσμν ρσμν ε ε ε ε ε ε ε ε ε ε ε ε ε ε εε ε ε ε  ′′ ′ ′ ′ ′ ′   ∆= − + +    ∆∆ ∆    R R J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 427 Journal of High Energy Physics, Gravitation and Cosmology 222 2 2 2 22 1 1 14 2 2 4 1 1 1 2 2 2 A B B A A B r B B r A B A B B B B A B B B B ε ε ε ε ε ε ε ε ε ε ε εε ε ε ε ε ε ε ε ε ε ε ε ε ε ε   ′ ′ ′ ′ ′   ∆  + + + + −   ∆∆ ∆       ′ ′ ′′ ′ ′ ′  ∆ + + − −  ∆      2 2 2 2 22 2 2 1 1 1 1 12 2 2 1 1 1 1 14 2 2 4 1 1 2 2 A A A B A A B B A A A B B r A A B B B A B A B B r B B B r A B A B A B B A B B ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε      ′′ ′ ′ ′ ′ ′ ′= − + + +                   ′ ′ ′ ′ ′ ′   + + + + − +                ′ ′ ′′ + + − 22 1 . 2 'B B A B B B A B ε ε ε ε ε ε ε ε ε     ′ ′ ′ − +             (A2.14) From Equation (A2.14) in the limit ( ], 0,1rε ρ ε→ ∈ by formulae (A2.3) we get ( ) ( )( ) ( ) ( ) 4 42 2 , , ,r r K r ρσμν ε ρσμν ε ε ε ε εε ε ρ ρ ε     ≈ +    − +    R R (A2.15) where ( )K r is a Kretschman scalar: ( ) ( ) 1213 6 23 4 4s sK r r r r r −= ⋅ + . Remark A2.5. Note that: (1) For ( )r rε ε= located beyond horizon, i.e. 0r ρ− ≈/  one obtains classical result ( ) ( )( ) ( )( ), , ,r r K rρσμν ε ρσμν ε εεε ε ≈ R R (A2.16) see Definition 1.5.2. (i). (2) At horizon : 0hor horr r rε ρ= − = , ( ]0,1ε ∈ from Equation (A2.15) one obtains nonclassical result ( ) ( )( ) ( ) ( )( )4, , 1 ,r r K Oρσμν ρσμν ε εε ε ρ ε −≈ + ≈ ∞   R R (A2.17) see Definition 1.5.2. (ii). Remark A2.6. Let ( ) 0rε ερ − ≈   , then from Equation (A1.3) and Equation (A2.15) we obtain ( ) ( )( ) ( ) ( ) 4 42 2 , , .r r K r ρσμν ε ρσμν ε ε ε ε εε ε ρ ρ ε        ≈ +       − +     R R (A2.18) Remark A2.7. We assume now there exist a fundamental generalized length ( )lε ε ( ) ( ] ( ) ( ] ( ) ( ] 0,0, ,1 , 1, , l a l a ε ε ηε η ε ε η ε η ∈∈ ∈ = =  (A2.19) such that ( ) ( ) ( )r l aε ε εε ερ ε− ≥ = It meant there exist a thickness ( )horth lε ε= of BH horizon. We introduce a norm horth of a thickness horth by formula J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 428 Journal of High Energy Physics, Gravitation and Cosmology ( ]0,sup ,horth lεε η η∈= = (A2.20) where parameter η is a classical thickness of BH horizon. By using (A2.19) we get the estimate ( ) ( )( ) ( ) ( ) ( ] ( ) ( ] ( ) ( ] ( ) ( ] 4 42 2 0, 2 2 2 22 2 0,0, 2 2 2 0, , , 1 r r K r rr r ρσμν ε ρσμν ε ε ε ε η εε ε ηε η ε ε η ε ε ερ ρ ε ε ρ ερ ε ε ρ ε ∈ ∈∈ ∈     ≈ +    − +           ≈ ×      − + − +          ×  − +        R R ( ) ( ) ( ] ( ] ( ) ( ) ( ] ( ) ( ) ( ] 2 2 2 2 2 22 2 0, 0, 2 22 2 2 0, 2 42 0, 1 1 1 1 1 1 1 r K ar K a r K ra ε ηε ε η ε ε η ρ η ερ ε ερ ε ρ ρ ε ρ ρ ∈ ∈ ∈ − ∈         ≤ +      +   − +            = +      + − +         ≤ +  − +    (A2.21) Appendix B We calculate now the distributional curvature at Schwarzschild horizon. In the usual Schwarzschild coordinates ( ), 0, , , 2t r r mθ φ> ≠ the metric is ( ) ( ) ( ) 12 2 2 2 2d d d d , 21 . s h r t h r r r mh r r − = − + Ω   = − +  (B.1) Metric takes the form above horizon 2r m> and below horizon 2r m< correspondingly ( ) ( ) ( ) ( ) ( ) ( ) 12 2 2 2 2 12 2 2 2 2 above horizon 2 : d d d d , 2 21 below horizon 2 : d d d d , 2 21 r m s h r t h r r r m r mh r r r r m s h r t h r r r m m rh r r r −+ + + + −− − − − >   = − + Ω    − = − + = −  <  = − + Ω  − = − + = (B.2) J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 429 Journal of High Energy Physics, Gravitation and Cosmology Remark B.1. Following the above discussion we consider the metric coefficients ( )h r+ , ( ) ( )1h r h r−+ −   , and ( ) 1 h r −−   as an element of ( )3D′  and embed it into ( )3D by replacement above horizon 2r m≥ and below horizon 2r m≤ correspondingly ( ) ( ) 2 2 2 2 2 : 2 2 , 2 : 2 2 . r m r m r m r m m r m r ≥ − − + ≤ − − +     (B.3) Note that, accordingly, we have fixed the differentiable structure of the manifold: the Cartesian coordinates associated with the spherical Schwarzschild coordinates in (B.1) are extended through the origin. We have above 2r m≥ (below ( 2r m≤ )) horizon ( ) ( )( ) ( ) ( )( ) ( )( ) ( ) { } ( ) ( ) ( ) ( ) ( ) ( ) ( )( ) 2 2 3 3 11 2 2 3 2 2if 2 , 0 if 2 where , 2 , , 2 , | 2 . 2, 2 if 2 2 0 if 2, 2 2 = , 0,2 , r m r mr mh r h rr rr m h r B m R B m R x m x R r r mr m r mh r h r h rr m r r mr m m r h r B m r + + + + −− + − − −  − − +− ≥  = = −    ≤   ∈ = ∈ ≤ ≤ − − > − ≤ = = = −   ≥∞ =   − +  ∈                     G G ( ) { } ( ) ( ) ( ) ( )( ) 3 1 3 2 2 where 0,2 | 0 2 , 2 , 0,22 2, 2 B m x x m r r m rh r B mr m r mr m − −− − = ∈ < ≤   − <  = ∈−    − +∞ =        G (B.4) Inserting (B.4) into (B.2) we obtain a generalized object modeling the singular Schwarzschild metric above (below) gorizon, i.e., ( ) ( )( ) ( )( ) ( ) ( )( ) ( )( ) 12 2 2 2 2 12 2 2 2 2 d d d d , d d d d s h r t h r r r s h r t h r r r −+ + + −− − −  = − + Ω   = − + Ω            (B.5) The generalized Ricci tensor above horizon β α +  R may now be calculated componentwise using the classical formulae ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) 0 1 0 1 2 3 22 3 1 2 2 1 . h h r h h r r ε ε + + + + + + + +  ′′ ′   = = +       ′ +    = = +                R R R R (B.6) From (B.4) by differentiation we obtain ( ) ( ) ( ) 1 22 2 1 2 22 2 22 , 2 r mr mh r rr r m +  − +−  ′ = − +  − +     J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 430 Journal of High Energy Physics, Gravitation and Cosmology ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) 1 22 2 2 2 1 2 22 2 1 22 2 2 2 1 22 2 1 22 2 1 2 22 1 2 2 22 1 2 2 1. 2 r h h r m r mr mr rrr r m r m r mr m r rr m r m r m + +′ + +   − + − +−  = − + + −    − +    − + − +−  = − + + −  − +  − = − +  − +            ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) 1 22 2 1 2 22 2 2 1 2 3 2 1 22 2 22 2 2 2 1 22 2 1 2 322 2 22 2 21 2 2 2 2 2 22 . 2 r mr mh r rr r m r m r m r r m r r m r r m r mr m rr r m ′ ′    − +−    ′′ = − +      − +        − − = − + +      − + − + − +       − +−  + −  − +          ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) 2 2 2 1 2 3 2 1 22 2 22 2 2 2 1 22 2 1 2 322 2 1 22 2 1 2 22 2 2 21 2 2 2 2 2 22 2 222 2 r h r h r m r mr r r m r r m r r m r mr m rr r m r mr mr rr r m + +′′ ′+  − −= − + +       − + − + − +       − +−  + −    − +     − +−  + − +    − +              ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) 2 1 2 3 2 1 22 2 22 2 2 1 22 2 1 22 2 1 22 2 1 22 2 2 1 2 3 22 22 2 2 2 2 2 2 2 22 2 2 22 2 2 2 . 2 2 r r mr r m r m r m r m r mr m rr m r mr m rr m r r mr r m r m ε ε ε − − = − + +      − + − + − +       − +−  + −  − +   − +−  − +  − +  − = − +    − + − +          (B.7) J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 431 Journal of High Energy Physics, Gravitation and Cosmology angular components of the Ricci tensor (using the abbreviation ( ) ( ) π 2π 0 0 sin d dr xθ θ φΦ = Φ∫ ∫   (B.8) and let ( )xΦ  be the function ( ) ( )( )32 0, 2 ,mx S B m R+Φ ∈  , where by ( )( )32 0, 2 ,mS B m R+ we denote the class of the functions ( )xΦ  with compact support such that: (i) ( )( ) ( ) { }0 02 , | 2x B m R x R x m+Φ ⊂ ⊂ ≥ ≥  supp 2) ( ) ( )r C∞Φ ∈  . Then for any function ( ) ( )( )32 0, 2 ,mx S B m R+Φ ∈  we get: ( ) ( ) ( ) ( ) ( ) ( )( ) ( ) ( ) ( ) ( ) 2 3 2 3 3 3 2 1 22 22 2 d d 1 d 2 d d . 2 K K R m R R m m x x x x r h h r r r m r r r r r m + + + +   Φ   = Φ  ′= + + Φ   − = − Φ + Φ    − +   ∫ ∫ ∫ ∫ ∫      R R         (B.9) By replacement 2r m u− = , from (B.9) we obtain ( ) ( ) ( ) ( ) ( ) ( ) ( ) 2 3 2 3 3 3 2 2 1 22 2 0 0 d d 2 d 2 d . K K R m R m x x x x u u m u u m u u + + − −   Φ   = Φ  Φ + = − + Φ + + ∫ ∫ ∫ ∫        R R (B.10) By replacement u η=  , from (B.10) we obtain the expression ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) 3 23 3 3 23 2 2 2 1 22 0 0 d d 2 d 2 d . 1 K K R m R m x x x x m η η η η η η + + + + − −    = Φ = = Φ      Φ + = − × − Φ +  +    ∫ ∫ ∫ ∫               I R I R (B.11) From Equation (B.11) we get ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) 2 3 2 1 220 2 2 1 1 220 2 2 2 1 1 220 2 1 d 0! 1 1 d 1! 1 2 22 1 1 1 d , 1 1 R m R m R m m R m R mm η η η η ξ η η η η ξ η η η − + + − −  Φ  = = − −  +      − − Φ  +    − −  = − Φ + − −        − − Φ  +   ∫ ∫ ∫     I I            (B.12) J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 432 Journal of High Energy Physics, Gravitation and Cosmology where we have expressed the function ( )2mηΦ +  as ( ) ( ) ( ) ( ) ( ) ( ) ( )10 2 12 , ! ! 2 , 1 0, 1 l n l n n l m m l n m n η η η ξ ξ θ η θ − = Φ Φ + = + Φ + > > = ∑      (B.13) with ( ) ( ) d dl l lξ ξΦ Φ  . Equations (B.12)-(3.13) give ( ) ( ) ( ) ( ) ( ) ( ) 2 3 20 0 0 2 2 1 1 20 2 0 2 2lim lim lim 2 1 1 lim 1 d 0. 1 1 R m R m R mm η ξ η η η + + → → → − →   − −   = = − Φ + − −             + − − Φ =  +    ∫              I I (B.14) Since ( )( ) ( )32 2 ,mS B m R D+′ ′⊂  , where ( ) { }32 , | 2B m R x m x R+ = ∈ ≤ ≤ from Equation (B.14) we get: ( ) ( ) 3 330 0 2 220 0 lim lim 0, lim lim 0. w w ε + + → → + + → →  − = =   − = =       R I R I (B.15) For ( ) ( )1 01 0,+ +        R R we get: ( ) ( ) ( ) ( ) ( ) ( )( ) ( ) ( ) ( ) ( ) ( ) 1 3 1 0 3 0 2 2 2 1 2 3 22 22 22 2 d 2 d 2 d 2 d . 2 2 K K R m R m x x x x r h r h r r r r mr r r r m r m + + + +   Φ   = Φ  ′′ ′= + Φ   − = − + Φ      − + − +     ∫ ∫ ∫ ∫             R R (B.16) where use is made of the relation ( ) ( ) 2 3 2 1 22 2 0 0 d dlim 1 1 1 s s s u η η η η→∞    − = −  + +  ∫ ∫ (B.17) Finally we obtain ( ) 1 0 1 00 0 lim lim 2 .w w m m+ + → →    − = − = − Φ        R R (B.18) The Colombeau generalized Ricci tensor below horizon β β α α − −   =    R R may now be calculated componentwise using the classical formulae ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) 0 1 0 1 2 3 22 3 1 2 , 2 1 . h h r h h r r − − − − − − − −   ′′ ′   = = +         ′ +    = = +                   R R R R (B.19) J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 433 Journal of High Energy Physics, Gravitation and Cosmology From (B.4) we obtain ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) 2 2 1 22 2 1/2 22 2 1 22 2 22 = , 2 . 22 , 2 21 1 1. 2 m rr mh r h r h r r m r r r mr mh r h r rr r m r mr h h r h h r m − − + − + − − + +  − +−  = − = − <       − +−  ′ ′= − = −  − +  −′ ′+ + = − + − = +  − +                 ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) 1 22 2 1 2 322 2 2 2 2 1 2 3 22 22 2 2 22 . 2 2 2 2 . 2 2 r mr mh r h r rr r m r h r h r h r h r r mr r m r m − + − − + +  − +−  ′′ ′′= − = − +  − +  ′′ ′ ′′ ′+ = − − − = −    − + − +                  (B.20) Investigating the weak limit of the angular components of the Ricci tensor (using the abbreviation ( ) ( ) π 2π 0 0 sin d dr xθ θ φΦ = Φ∫ ∫   and let ( )xΦ  be the function ( ) ( )( )32 , 0, 2mx S B m− −Φ ∈  , where by ( )( )32 , 0, 2mS B m− − we denote the class of the functions ( )xΦ  with compact support ( )0,2K B m−⊂ , ( ) { }0,2 | 0 2B m x x m− = ≤ ≤  such that: (i) ( )( ) { }| 0 2x x x mΦ ⊂ ≤ ≤  supp (ii) ( ) ( ).r C∞Φ ∈  Then for any function ( ) ( )( )32 , 0, 2mx S B m− −Φ ∈  we get ( ) ( ) ( ) ( ) ( ) ( )( ) ( ) ( ) ( ) ( ) 2 3 2 3 3 3 2 0 2 2 1/22 20 0 d d 1 d 2= d d . 2 K K m m m x x x x r h h r r r m r r r r r m − − − −   Φ   = Φ  ′= + + Φ   − Φ + Φ    − +   ∫ ∫ ∫ ∫ ∫      R R         (B.21) By replacement 2r m u− = , from Equation (B.21) we obtain ( ) ( ) ( ) ( ) ( ) ( ) ( ) 2 3 2 3 3 3 0 0 1 22 22 2 d d 2 d 2 d . K K m m x x x x u u m u u m u u − − − −   Φ   = Φ  Φ + = + Φ + + ∫ ∫ ∫ ∫   R R      (B.22) J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 434 Journal of High Energy Physics, Gravitation and Cosmology By replacement u η=  , from (B.22) we obtain ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) 3 23 3 3 23 2 0 0 1 222 2 d d 2 d 2 d , 1 K K m m x x x x m m η η η η η η − − − − − −    = Φ = = Φ      Φ + = × + Φ +  +    ∫ ∫ ∫ ∫    I R I R           (B.23) which is calculated to give ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) 0 3 2 1 222 02 1 1 222 2 02 1 1 222 2 1 d 0! 1 1 d 1! 1 2 22 1 1 1 d , 1 1 m m m m m mm η η η η ξ η η η η ξ η η η − − − − −  Φ  = = +  +      + + Φ  +      = Φ − + +        + + Φ  +   ∫ ∫ ∫     I I            (B.24) where we have expressed the function ( )2mηΦ +  as ( ) ( ) ( ) ( ) ( ) ( ) ( ) 1 0 2 12 , ! ! 2 , 1 0, 1 ln l n n l m m l n m n η η η ξ ξ θ η θ − =  Φ Φ + = + Φ   + > > = ∑      (B.25) with ( ) d dl l lrΦ Φ  . Equation (B.25) gives ( ) ( ) ( ) ( ) ( ) ( ) 2 3 20 0 0 02 1 1 20 22 2 2lim lim lim 2 1 1 lim 1 d 0. 2 1m m mm η ξ η η η − − → → → → −      = = Φ − + +             + + Φ =  +    ∫              I I (B.26) Since ( )( ) ( )32 0, 2mS B m D−′ ′⊂  , where ( ) { }30, 2 | 0 2B m x x m− = ∈ ≤ ≤ from Equation (B.26) we obtain ( ) ( ) 3 330 0 2 220 0 lim lim 0. lim lim 0. w w − − → → − − → →   − = =     − = =        R I R I (B.27) For ( ) ( )1 01 0,− −        R R we get: ( ) ( ) ( ) ( ) 1 3 1 0 3 0 2 d 2 d K K x x x x − −   Φ   = Φ  ∫ ∫ R R     J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 435 Journal of High Energy Physics, Gravitation and Cosmology ( ) ( )( ) ( ) ( ) ( ) ( ) ( ) 2 2 0 22 1 2 3 22 22 20 2 d 2 d . 2 2 m m r h r h r r r r mr r r r m r m ′′− −′= + Φ   − = − Φ      − + − +     ∫ ∫        (B.28) By replacement 2r m u− = , from (B.28) we obtain ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( )( ) ( ) ( ) ( ) ( ) ( ) 1 03 3 1 21 0 2 2 0 20 1 2 3 22 2 2 22 2 d 2 d 2 d 22= 2 d . m m I x x I x x r h r h r r u u mu m u m u u u + − + − − − −    = Φ = = Φ    ′′ ′= + Φ  ++ − Φ +  + +   ∫ ∫   R R            (B.29) By replacement u η=  , from (B.29) we obtain ( ) ( ) ( ) ( ) ( ) ( )( ) ( ) 1 3 1 0 3 0 0 2 2 2 d 2 d 2 d K K m x x x x r h r h r r − − − − −   Φ   = Φ  ′′ ′= + Φ ∫ ∫ ∫  R R          ( ) ( ) ( ) ( ) 2 20 1 2 3 22 2 2 2 2 22 22 2 d m mm m η ηη η η η η−  ++ = − Φ +  + +   ∫           ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) 20 0 1 2 1 22 2 2 2 2 22 2 4 3 3 20 0 3 2 3 22 2 2 2 2 22 2 30 0 1 2 3 22 22 2 20 1 222 2 d 2 d 2 2 d 2 d 2 2 d 2 d 1 1 2 d 2 d 2 1 m m m m m m m m m m m m m m m m m m η η η η η η η η η η η η η η η η η η η η η ε η η η η η η η η − − − − − − − Φ + Φ + = + + + Φ + Φ + − − + + Φ + Φ + = − + + Φ + Φ + + − + ∫ ∫ ∫ ∫ ∫ ∫ ∫                                    ( ) 0 3 222 . 1m η−       +   ∫  (B.30) which is calculated to give ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) 0 2 0 1 1 2 3 22 22 2 2 1 2 1 2 3 22 2 0 2 12 d 0! 1 1 1 d . 1! 1 1 l m m m m O η η η η η ξ η η η η − − −  Φ  = = −  + +     + Φ − +  + +  ∫ ∫          I I (B.31) J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 436 Journal of High Energy Physics, Gravitation and Cosmology where we have expressed the function ( )2mηΦ +  as ( ) ( ) ( ) ( ) ( ) ( ) ( ) 1 0 2 12 , ! ! 2 , 1 0, 1 ln l n n l m m l n m n αβ αβη η η ξ ξ θ η θ − = Φ Φ + = + Φ + > > = ∑      (B.32) with ( ) ( ) d dl l lξ ξΦ Φ  . Equation (B.32) gives ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) 0 2 0 1 1 2 3 20 0 0 2 22 0 0 2 1 2 3 20 2 2 2 1lim lim 2 lim d 0! 1 1 d d2 2 lim 2 2 . 1 1 m s s s m m m m m m η η η η η η η η η − − → → → − → − −   Φ  = = −  + +        = Φ − = Φ  + +   ∫ ∫ ∫    I I       (B.33) where use is made of the relation ( ) ( ) 0 0 2 1 2 3 22 2 d dlim 1. 1 1s s su η η η η→∞ − −    − =  + +  ∫ ∫ (B.34) Thus ( ) 1 0 1 00 0 lim lim 2 .w w m m− − → →    − = − = Φ        R R (B.35) Appendix C We calculate now the distributional Colombeau scalars ( )( ) ( ) ( )( ), , , ,r r rμν μνε εε ε εR R R and ( ) ( )( ), ,r r ρσμν ρσμν ε ε εR R , in terms of Colombeau generalized functions ( )( ) ( )( ) ( )( ) ( )( ), , ,A r B r C r D rε ε ε εε ε ε ε is given above in Appendix B at Schwarzschild horizon.We choose now ( ) ( ) ( ) ( )11, 1 , 0,B r C r A r D rε ε ε ε−= = − + = (C.1) and rewrite Equation (A.1) in the following equivalent form ( ) ( )( ) ( )( )2 2 1 2 2 2d d d d ,s A r t A r r rε ε εε ε ε −= − + + Ω (C.2) where ( )A rε is given above by using Equations (B.2)-(B.4). Thus we obtain ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) 21 2 2 22 2 3 2 2 2 3 2 3 223 2 3 2 3 223 2 2 , 1, 0, 2 2 , 2 2 16 24 12 4 2 2 4 2 4 . 2 A r r r m A B C D m r m A r r r m m m m r mr m r r A r r r m m r m r m r r m ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε − ′= − − + ∆ = + + = ∆ = − − ′ = − + − + − − + + ′′ =  − +  − + − =  − +  (C.3) From Equation (A.2) and Equation (C.3) we obtain J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 437 Journal of High Energy Physics, Gravitation and Cosmology ( )( ) ( ) 2 2 2 1 2 2 2, 2 3 2 1 12 2 2 2 12 2 A A B A C D A B r r A B A B A Br B A B A B B A B A B A AA A A r A Ar ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε ε εε ε ε ε ε ε ε −   ′ ′ ′ ′′ ′′ ∆ + = − − + + − −    ∆ ∆   ′ ′ ′ ′ ′ ′    ∆ + − + +    ∆         −′ ′′   = − − −       R ( ) ( ) ( )( ) ( ) ( ) 2 2 23 2 223 2 3 2 2 2 3 2 3 223 2 4 2 2 8 2 22 2 2 2 16 24 12 4 2 . 2 A A A r r r m r m r r m rr r m m m m r mr m r r r r m ε ε ε ε ε ε ε ε ε ε ε − ′ ′′= − − + −     − = + − + −  − +    − + − − + +  −     − +    (C.4) Finally we obtain the following expression for the distributional Colombeau scalar ( )( ),r εεR ( )( ) ( ) ( ) ( )( ) ( ) ( ) ( ) 23 2 23 2 3 2 2 3 223 2 8 2 , 2 2 2 4 2 42 . 2 m r m r r r m r r m m r m r m r r r m ε ε ε ε ε ε ε ε ε −  − = + − +   − +    − + − − − −    − +    R (C.5) Remark C.1. Note that from Equation (C.5) follows that: 2r m≠ ( )( ), 0r εε ≈ R , see Definition 1.5.2. (i). We assume now that ( ) 2r mε ε ≈  and therefore from Equation (C.5) we obtain ( )( ) ( ) 2 2 3 223 2 4, . 8 2 mr m r m ε ε ε ε ε ε ε     ≈    − +    R (C.6) Remark C.2. Note that from Equation (C.6) at horizon 2r m= follows that: ( )( ) ( ) ( ) 2 2 1 1 3 23 2 4, 4 , 8 mr m mε ε ε εε ε ε − −    = = ≈ ∞       R (C.7) see Definition 1.5.2. (ii). Remark C.3. Note that from Equation (C.5) follows that: ( ) ( ) 0 -lim , ~ 2 .w r r m ε ε δ → −R (C.8) J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 438 Journal of High Energy Physics, Gravitation and Cosmology Remark C.4. Let ( )2 0r mε ε − ≈   , then from Equation (A1.3) and Equation (C.6) we obtain ( )( ) ( ) 2 2 3 223 2 4, . 8 2 mr m r m ε ε ε ε ε ε ε        ≈       − +     R (C.9) From Equation (A.2) and Equation (C.3) we obtain ( ) ( )( ) ( ) ( ) ( ) ( ) ( ) ( ) 2 2 2 2 22 3 2 3 22 2 3 2 3 2 3 22 23 2 , , 11 1 12 2 2 1 1 22 2 2 2 4 2 4 22 2 22 r r A A A A r rr m r mr m r r r r m m r m r m m r m r r mr r m μν μν ε ε ε ε ε εε ε ε ε ε ε ε εε    − +   ′ ′′ ′= + + + +                 −   = + − + +     + −      − + − − + −    + − − +   R R .   (C.10) Remark C.5. Note that from Equation (C.10) follows that: ( ) ( )( ) ( ) ( ) 2 6 2 , , , 12 , 2s s r m r r K r rK r r m r μν μν ε ε ε≈ ⇒ ≈/ = =   R R (C.11) see Definition 1.5.2. (i). We assume now that ( ) 2r mε ε ≈  and therefore from Equation (C.10) we obtain ( ) ( )( ) ( ) ( ) 4 324 2 , , 4 2 sr r K r m r m μν ε μν ε ε ε ε ε ε ε ε     ≈ +    + −    R R (C.12) Remark C.6. Note that from Equation (C.10) at horizon 2r m= follows that: ( ) ( )( ) 4 2 1, , , 4 r r m μν μν ε ε ε ε ε  = ≈ ∞    R R (C.13) see Definition 1.5.2. (ii). Remark C.7. Let ( )2 0r mε ε − ≈   , then from Equation (A1.3) and Equation (C.12) we obtain ( ) ( )( ) ( ) ( )( ) 4 324 2 , , 4 2 sr r K r m r m μν ε μν ε ε ε ε ε ε ε ε        ≈ +      + −     R R (C.14) From Equation (A.2) and Equation (C.3) we obtain J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 439 Journal of High Energy Physics, Gravitation and Cosmology ( ) ( )( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) 2 22 2 2 2 22 2 4 2 3 22 2 3 2 623 2 , , 12 4 1 2 14 4 1 4 2 4 8 2 22 r r A A A A r rr A A A r r m r m r m m r m r r mr r m ρσμν ρσμν ε ε ε ε ε εε ε ε ε ε εε ε ε ε ε ε     ′ ′    ′′= + + − +                      ′  ′′= + + −           − + − − = −    − − +      R R ( )( ) 2 2 2 21 2 4 4 1 2 .r r m r ε ε−  +  + + − + (C.15) Remark C.8. Note that from Equation (C.15) follows that: ( ) ( )( ) ( )2 , , ,r m r r K rρσμν ρσμν εε ε≈ ⇒ ≈/   R R (C.16) see Definition 1.5.2. (i). We assume now that ( ) 2r mε ε ≈  and therefore from Equation (C.10) we obtain ( ) ( )( ) ( ) ( )( ) 4 324 2 , , 4 2 sr r K r m r m ρσμν ε ρσμν ε ε ε ε ε ε ε ε     ≈ +   + −    R R (C.17) Remark C.9. Let ( )2 0r mε ε − ≈   then from Equation (A1.3) and Equation (C.12) we obtain ( ) ( )( ) ( ) ( )( ) 4 324 2 , , 4 2 sr r K r m r m ρσμν ε ρσμν ε ε ε ε ε ε ε ε      = +    + −    R R (C.18) Remark C.10. Note that from Equation (C.15) at horizon r = 2m follows that: ( ) ( )( ), , ,r rρσμν ε ρσμν ε εε ε  ≈ ∞  R R (C.19) see Definition 1.5.2. (ii). Remark C.11. We assume now there exist a fundamental generalized length ( )lε ε ( ) ( ] ( ) ( ] ( ) ( ] 0,0, 0, , 1, , l a l a ε ε ηε η ε ε η ε η ∈∈ ∈ = =  (C.20) such that ( ) ( ) ( )r l aε ε εε ερ ε− ≥ = It meant there exist a thickness ( )horth lε ε= of BH horizon. We introduce a norm horth of a thickness horth by formula ( ]0,suphorth lεε η η∈= = (C.21) where parameter η is a classical thickness of BH horizon. By using (C.20) we get the estimate J. Foukzon et al. DOI: 10.4236/jhepgc.2018.42023 440 Journal of High Energy Physics, Gravitation and Cosmology ( ) ( )( ) ( ) ( )( ) ( ] ( ) ( ) ( ] ( ) ( ] ( ) ( ] ( ) 4 324 2 0, 24 2 0, 2 2 2 22 2 0, 0, 24 2 , , 4 2 1 4 2 2 2 1 1 4 1 s s s r r K r m r m K r m r m r m r m K r m a ρσμν ε ρσμν ε ε ε ε ε η ε ε ε η ε ε ε η ε η ε ε ε ε ε ε ε ε ε ∈ ∈ ∈ ∈        ≈ +      − +          = +    − +             × ×      − + − +          ≤ +  +  R R ( ) ( ] ( ) ( ) ( ] 24 2 0, 2 24 2 2 0, 4 2 1 1 28 1 s r m m r m K r r mm a ε ε η η ε ∈ − ∈       − +       ≤ +  − +    (C.22)