2 ds 2 = g$_{µν}$ ( x ) dx $^{µ}$dxν = − Δ Σ ( dt − a sin $^{2}$θ dφ ) 2 + Σ Δ dr 2 + Σ dθ 2 + sin $^{2}$θ Σ ( a dt − ( r 2 + a $^{2}$) dφ ) 2 (1) where Σ ( r ) = r 2 + a $^{2}$cos$^{2}$θ Δ ( r ) = r 2 − 2 Mr + a 2 + Q 2 (2) and Q, a and M the charge, angular momentum per unit mass and mass of the black hole respec- tively. For the most part the explicit statement of the dependence of Eq.(2) on r will be assumed and so it will be suppressed for brevity unless otherwise stated. Together these three parame- ters form a family containing a set of all classical black holes. The coordinate system breaks down twice for this metric, firstly for the radial part when 1 g$_{rr}$ = 0 then for the time part of the met- ric when g$_{tt}$ = 0, r$_{±}$ = M ± $^{√}$M 2 − a 2 − Q 2 Where r$_{+(}$$_{−}$$_{)}$ is the outer (inner) event horizon. In order to relate local and global coordinates one must introduce a tetrad (or vierbein) formalism, which we have chosen to be e µ 0 ( x ) = $^{(}$a 2 + r 2 √ ΔΣ , 0 , 0 , − a sin( θ ) √ Σ ) e µ 1 ( x ) = ( 0 ,$^{√}$ Δ Σ , 0 , 0$^{)}$ e µ 2 ( x ) = ( 0 , 0 , 1 √ Σ , 0$^{)}$ e µ 3 ( x ) = ( − a √ ΔΣ , 0 , 0 , 1 sin( θ ) √ Σ$^{)}$ (3) u $^{t}$( x ) = N − $^{1}$cosh( ζ ) = r$^{√}$ √ √ ( a 2 + r $^{2}$) 2 − a $^{2}$Δ a $^{2}$(2 Mr − Q $^{2}$) 2 + (Δ − a $^{2}$) $^{(}$( a 2 + r $^{2}$) 2 − a $^{2}$Δ ) cosh( ζ ) u $^{ϕ}$( x ) = − N − $^{1}$N $^{ϕ}$cosh( ζ ) + sinh( ζ ) √ g$_{ϕϕ}$ = r $^{√}$( a 2 + r $^{2}$) 2 − a $^{2}$Δ    a $^{(}$2 Mr − Q 2 $^{)}$cosh( ζ ) √ a $^{2}$(2 Mr − Q $^{2}$) 2 + (Δ − a $^{2}$) $^{(}$( a 2 + r $^{2}$) 2 − a $^{2}$Δ ) + sinh( ζ )$^{}$   (5) N = 1 tt A particle in a circular orbit on the equatorial plane ( θ = π/ 2) is now considered, with a radius r( > r$_{+}$ ) and constant velocity. The four velocity of such a particle is given by ω 0 t $_{1}$( x ) = ω 1 t $_{0}$( x ) ω 1 θ $_{2}$( x ) = − ω 2 θ $_{1}$( x ) ω 1 ϕ $_{3}$( x ) = − ω 3 ϕ $_{1}$( x ) ω 1 t $_{3}$( x ) = − ω 3 t $_{1}$( x ) ω 0 ϕ $_{1}$( x ) = ω 1 ϕ $_{0}$( x ) ω 0 r $_{3}$( x ) = ω 3 r $_{0}$( x ) ω 0 r $_{0}$( x ) = ω 3 r $_{3}$( x ) (4) This describes a local inertial frame for a parti- cle, in this case they are rotating with respect to an observer at infinity. In this respect Eq.(3) and its inverse are central to relating local and global coordinates. For example the momentum in a local inertial frame p $^{a}$( x ) is e $^{a}$$_{µ}$( x ) p $^{µ}$( x ) in relation to its global definition. It is imperative that properties can be related locally and glob- ally on a manifold. Henceforth terms not shown are vanishing unless explicitly stated otherwise. A straight-forward, but tedious calculation yields the components of the connection one-form [8], ω a µ $_{b}$( x ) = e $^{a}$$_{ν}$( x ) ∇$_{µ}$ e ν b ( x ), these are a spin con- nection. These are very involved equations in the Kerr-Newman spacetime. One notes how- ever that the nonzero Schwarzschild symmetry is preserved and extended to some other pairs of elements. The following are the nonvanishing one-forms restricted to the equatorial plane, where ζ is the rapidity in the local inertial frame defined by and