7 ∓ Φ about the 2-axis at φ = ± Φ respectively, As in [1], is found to describe the state, where Since the trivial rotation has been removed it is clear that a real deterioration of the perfect correlation between the spins is being observed, We adopt the Doran [4] metric to remove the co- ordinate singularities of the metric. The observer can now fall through the apparent singularities of the Kerr-Newman spacetime observed by an observer at infinity. For this observer the line element is given by however only local unitary operations have been applied and the entanglement is invariant under unitary operations. Hence this must be an af- fect of the acceleration and gravity. If the pure state can be recovered then quantum computa- tions may still be done while in the presence of a gravitational field. In particular the respective observers at φ = ± Φ must take measurements at an angle ∓ Θ in their local inertial frames. Since ϑ $^{a}$$_{b}$( x ) = χ $^{a}$$_{b}$( x ) a parallel transport would not reproduce this angle. Hence by transforming in the appropriate direction the full EPR correla- tion may still be recovered. Now it was found that Δ is positive for r → ∞ to a radius r$_{0}$ very close to the outer horizon r$_{+}$ . As r becomes smaller than r$_{0}$ and furthermore r ↓ r$_{+}$ , Δ → −∞ and thus to extract the perfect EPR correlation each observer would require in- finite accuracy in the measurement that even a small error would lead to a mixed state element. In the ( t, r, θ, φ ) coordinates the vierbein inher- ited the r$_{+}$ and r$_{−}$ coordinate singularities, the above ( T, R, θ, φ ) also act as the metric does at those radii, and since the metric is singularity free there so is the vierbein. Now similarly to Eq.(5) we take a four velocity of the form, and the time coordinate coincides with the proper time for the free fall observer. The vier- bein is now chosen to be, where | p a $_{±}$, ↑ ; ± Φ 〉 ′ = cos( Φ 2 ) | p a $_{±}$, ↑ ; ± Φ 〉 ± sin( Φ 2 ) | p a $_{±}$, ↓ ; ± Φ 〉 , (35) (36) | p a $_{±}$, ↓ ; ± Φ 〉 ′ = ∓ sin( Φ 2 ) | p a $_{±}$, ↑ ; ± Φ 〉 + cos( Φ 2 ) | p a $_{±}$, ↓ ; ± Φ 〉 , (37) 1 √ 2$^{[}$ cos(Δ) $^{(}$| p a $_{+}$, ↑ ; Φ 〉 ′ | p a $_{−}$, ↓ ; − Φ 〉 ′ − | p a $_{+}$, ↓ ; Φ 〉 ′ | p a $_{−}$, ↑ ; − Φ 〉 ′ ) + sin(Δ) $^{(}$| p a $_{+}$, ↑ ; Φ 〉 ′ | p a $_{−}$, ↑ ; − Φ 〉 ′ + | p a $_{+}$, ↓ ; Φ 〉 ′ | p a $_{−}$, ↓ ; − Φ 〉 ′ ) ] (38) Δ = Θ − Φ = Φ$^{[}$ r sinh( ζ ) ϑ 1 3 − 1$^{]}$ (39) Ω = $^{(}$R 2 + a 2 ) 1 2 b = ( 2 MR − Q $^{2}$) 1 2 Ω Σ = $^{(}$R 2 + a $^{2}$cos$^{2}$( θ ) ) 1 / 2 (41) ˜ e µ 0 ( x ) = (1 , 0 , 0 , 0) ˜ e µ 1 ( x ) = ( b Ω Σ , Σ Ω , 0 , − a b sin $^{2}$( θ ) Ω Σ$^{)}$ ˜ e µ 2 ( x ) = (0 , 0 , Σ , 0) ˜ e µ 3 ( x ) = (0 , 0 , 0 , Ω sin ( θ )) (42) ds 2 = − dT 2 +$^{[}$ Σ Ω dR + b Ω Σ $^{(}$dT − a sin $^{2}$( θ ) dφ ) ] 2 + Σ $^{2}$dθ2 + Ω $^{2}$sin$^{2}$( θ ) dφ 2 (40) IV. THE INFALLING OBSERVER