# Total Conserved Charges of Kerr-Newman Spacetimes in Gravity Theory Using a Poincaré Gauge Version of the Teleparallel Equivalent of General Relativity

Authors: Gamal G. L. Nashed
Journal: Advances in High Energy Physics
 (2013)

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## Abstract

The total conserved charges of several tetrad spacetimes, generating the Kerr-Newman (KN) metric, are calculated using the approach of invariant conserved currents generated by an arbitrary vector field that reproduces a diffeomorphism on the spacetime. The accompanying charges of some tetrads give the known value of energy and angular momentum, while those of other tetrads give, in addition to the unknown format charges, a divergent entity. Therefore, regularized expressions are considered also to get the commonly known form of conserved charges of KN.


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## Body

## 1. Introduction

To find new black hole solutions in the Einstein gravitational theory, one needs to couple the Einstein Hilbert action to matter fields that have associated conserved charges. The charges must be those of point particles, or one will obtain solutions describing extended objects instead of black holes. Thus, one needs to consider vector fields, and the simplest one is an Abelian vector fieldAμ. Axially symmetric solutions of the Einstein field equations are used to describe a wide range of black holes appearing in the universe. The most promising of these solutions is the Kerr spacetime that describes an axially symmetric, rotating black hole [1]. Generalizations of the Kerr black holes are the charged Kerr-Newman, Kerr-de Sitter spacetime that incorporates a nonvanishing cosmological constant, Kerr-Taub-NUT spacetime that includes the NUT charge, or some combination of these. All of these spacetimes could be seen as special cases of the family of electrovac spacetimes of Petrov type D provided by the Plebański-Demiański class of solutions [2]. They are distinguished by seven parameters: the mass, the rotation around the symmetry axis, the electric and magnetic charges, the NUT charge, the cosmological constant, and the acceleration of the gravitating source.The definition of conserved charges in general relativity (GR) is an important and a delicate issue to some extent, which concerns the definition of the energy-momentum tensor of the gravitational field. Perturbatively, GR gives the unique energy-momentum tensor [3, 4]. Many researchers (starting from Einstein himself) have tried in vain to find a fully general-covariant energy-momentum tensor for the gravitational field that is reducible to the weak-field limit. Therefore, one has to restrict with energy-momentum pseudotensors for the gravitational field, which are covariant only under a limited set of coordinate transformations. This, in fact, would be one of the properties of the gravitational field linked to the principle of equivalence of gravitation and inertia that says that all the physical effects from the gravitational field can be locally eradicated by selecting a locally inertial coordinate system [5].The main result of the lack of a totally general-covariant energy-momentum tensor for the gravitational field is the nonlocalizability of the gravitational energy; just the total energy of a spacetime is well defined (and conserved), since the integral of the energy-momentum pseudotensor over a finite volume will be dependent on the choice of coordinates. Some researcher find this is unacceptable, and, therefore, the search for the general-covariant tensor goes on.It is well established in the laws of physics that symmetry principles and conservation laws play key roles in understanding physical phenomena [6–8]. Various physical problems can be solved remarkably easier, and one might gain deeper insight of their nature when symmetry is taken into consideration. Some fields of study in modern physics have developed relatively quickly through the understanding of the principles of symmetry, for instance, the gauge symmetries in quantum field theory and elementary particle physics [9–11].The existence of symmetries in a physical system means that there exists one or more transformations that leave the physical system invariant. Since physical systems can be fully described by their Lagrangians/Hamiltonians, then it is natural to expect the symmetry transformations to be canonical ones. The number of symmetry transformations that can be generated from a system depends on the number of conserved quantities associated with that system [6, 7, 12].A number of methods are currently used in the calculations of energy and conserved charges that provide reliable results. Gibbons et al. [5] compute the energy of Kerr-AdS black holes firstly indirectly, through integrating the first law, then using the conformal definition of Ashtekar et al. [13, 14], and they indicate that both of them agree. In addition to the Regge-Teitelboim method [15], many others are present: the approach of Abbott and Deser [16–18], the spinor definition [19, 20] based on the electric Weyl tensor, covariant phase space methods [21–24], cohomological techniques [25, 26], the KBL approach [27–29], Noether methods [30–36], the counter term subtraction method [37, 38] (more references on this in [23], for example), improved surface integrals [39, 40], and regularization of the Euclidean action [41, 42]. Various examples proposing a universal approach for carefully revising geometric field theories in the sense of the language of Cartan connections are given [43].The aim of this work is to apply the definition of conserved currents and charges for models with quasi-invariant Lagrangians (Lagrangians that change by a total derivative under local Lorentz transformations) to KN spacetimes, which are considered as exact solutions to the Einstein field equations. In Section2, the language of exterior forms is used to give the scheme approach to the teleparallel approach. In Section 2, an axially symmetric spacetime, KN, in TEGR is given. The total conserved currents of this spacetime are calculated, and an unacceptable form of angular momentum is obtained as a result. In Section 3, regularized conserved charges are provided and are used to recalculate the conserved charges of the first KN spacetime. Also in Section 3, a second KN spacetime is provided, and calculation of the total conserved charges is given. Unfortunately, the conserved quantity is divergent in azimuthal direction [44–47]. Even when the regularized conserved charges are used, to recalculate the conserved charges of the second coframe, curious result is obtained in azimuthal direction. In Section 4, conserved charges using the Poincaré gauge (PG) version of TEGR are employed. The PG version is used to recalculate the conserved charges of the secondKN spacetime, and a consistent result is derived. In Section 4, a third KN spacetime is given to calculate its total conserved charges. The conserved quantity of this coframe, when it is calculated using the total conserved charges, is divergent in the azimuthal direction [48, 49]. Using the PG version, the total charges of the third KN spacetime are recalculated, and a satisfactory result is obtained. Also in Section 4, fourth and fifth KN spacetimes are provided, and the PG version is used to calculate their total conserved charges. The final section is devoted to the main results.


### 1.1.  Notation

The Latin indicesi,j,…, are used for local holonomic spacetime coordinates, and the Greek indices α,β,…, label (co)frame components. Particular frame components are denoted by hats, 0^, 1^, and so forth. As usual, the exterior product is denoted by ∧, while the interior product of a vector ξ and a p-form Ψ is denoted by ξ⌋Ψ. The vector basis dual to the frame 1-forms ϑα is denoted by eα, and they satisfy eα⌋ϑβ=δαβ. Using local coordinates xi, we have ϑα=hiαdxi and eα=hαi∂i where hiα and hαi are the covariant and contravariant components of the tetrad field. We define the volume 4-form by η=def.ϑ0^∧ϑ1^∧ϑ2^∧ϑ3^. Furthermore, with the help of the interior product, we define
(1)ηα=def.eα⌋η=13!ϵαβγδϑβ∧ϑγ∧ϑδ,
where ϵαβγδ is completely antisymmetric with ϵ0123=1. One has
(2)ηαβ=def.eβ⌋ηα=12!ϵαβγδϑγ∧ϑδ,ηαβγ=def.eγ⌋ηαβ=11!ϵαβγδϑδ,
which are bases for 3-, 2-, and 1-forms, respectively. Finally,
(3)ηαβμν=def.eν⌋ηαβμ=eν⌋eμ⌋eβ⌋eα⌋η,
is the Levi-Civita tensor density. The η-forms satisfy the useful identities as follows:
(4)ϑβ∧ηα=def.δαβη,ϑβ∧ημν=def.δνβημ-δμβην,ϑβ∧ηαμν=def.δαβημν+δμβηνα+δνβηαμ,ϑβ∧ηαγμν=def.δνβηαγμ-δμβηαγν+δγβηαμν-δαβηγμν.
The line element ds2=def.gαβϑα⊗ϑβ is defined by the spacetime metric gαβ.


## 1.1.  Notation

The Latin indicesi,j,…, are used for local holonomic spacetime coordinates, and the Greek indices α,β,…, label (co)frame components. Particular frame components are denoted by hats, 0^, 1^, and so forth. As usual, the exterior product is denoted by ∧, while the interior product of a vector ξ and a p-form Ψ is denoted by ξ⌋Ψ. The vector basis dual to the frame 1-forms ϑα is denoted by eα, and they satisfy eα⌋ϑβ=δαβ. Using local coordinates xi, we have ϑα=hiαdxi and eα=hαi∂i where hiα and hαi are the covariant and contravariant components of the tetrad field. We define the volume 4-form by η=def.ϑ0^∧ϑ1^∧ϑ2^∧ϑ3^. Furthermore, with the help of the interior product, we define
(1)ηα=def.eα⌋η=13!ϵαβγδϑβ∧ϑγ∧ϑδ,
where ϵαβγδ is completely antisymmetric with ϵ0123=1. One has
(2)ηαβ=def.eβ⌋ηα=12!ϵαβγδϑγ∧ϑδ,ηαβγ=def.eγ⌋ηαβ=11!ϵαβγδϑδ,
which are bases for 3-, 2-, and 1-forms, respectively. Finally,
(3)ηαβμν=def.eν⌋ηαβμ=eν⌋eμ⌋eβ⌋eα⌋η,
is the Levi-Civita tensor density. The η-forms satisfy the useful identities as follows:
(4)ϑβ∧ηα=def.δαβη,ϑβ∧ημν=def.δνβημ-δμβην,ϑβ∧ηαμν=def.δαβημν+δμβηνα+δνβηαμ,ϑβ∧ηαγμν=def.δνβηαγμ-δμβηαγν+δγβηαμν-δαβηγμν.
The line element ds2=def.gαβϑα⊗ϑβ is defined by the spacetime metric gαβ.


## 2. Brief Review of Teleparallel Gravity and Conserved Currents

Teleparallel geometry can be viewed as a gauge theory of translation [50–62]. The coframe ϑα plays the role of the gauge translational potential of the gravitational field. GR can be reformulated as the teleparallel theory. Geometrically, teleparallel gravity can be considered as a special case of the metric-affine gravity in which ϑα and the local Lorentz connection are subject to the distant parallelism constraint Rαβ=0 [63–71]. In this geometry, the torsion 2-form
(5)Tα=Dϑα=dϑα+Γβα∧ϑβ=12Tμναϑμ∧ϑν=12Tijαdxi∧dxj
arises as the gravitational gauge field strength, Γαβ is the Weitzenböck 1-form connection, d is the exterior derivative, and D is the exterior covariant derivative. The torsion Tα can be decomposed into three irreducible pieces [72]: the tensor part, the trace, and the axial trace given, respectively, by
(6)(1)Tα=def.Tα-T(2)α-T(3)α,with(2)Tα=def.13ϑα∧T,whereT=(eβ⌋Tβ),eα⌋T=Tμαμ,vectorsoftraceoftorsion(3)Tα=def.13eα⌋P,withP=(ϑβ∧Tβ),eα⌋P=Tμνλημνλα,axialoftraceoftorsion.
The Lagrangian of the TEGR has the form
(7)V=-12κTα∧*((1)Tα-2T(2)α-12T(3)α).κ=8πG/c^3, G is the Newtonian constant, c is the speed of light, and * denotes the Hodge duality in the metric gαβ which is assumed to be flat Minkowski metric gαβ=oαβ=diag(+1,-1,-1,-1) that is used to raise and lower local frame (Greek) indices. (The effect of adding the non-Riemannian parity odd pseudoscalar curvature to the Hilbert-Einstein-Cartan scalar curvature was studied by many authors (cf. [73–77] and references therein).)The variation of the total action with respect to the coframe gives the field equations in the form(8)DHα-Eα=Σα,whereΣα=def.δLmattterδϑα
is the symmetric energy-momentum tensor 3-form of matter which is considered as the source. In accordance with the general Lagrange-Noether scheme [59, 78], one derives from (7) the translational momentum 2-form and the canonical energy-momentum 3-form as follows:
(9)Hα=def.-∂V∂Tα=1κ*((1)Tα-2T(2)α-12T(3)α),(10)Eα=def.∂V∂ϑα=eα⌋V+(eα⌋Tβ)∧Hβ.
Due to geometric identities [72], the Lagrangian (7) can be recast as
(11)V=-12Tα∧Hα.
The presence of the connection field Γαβ plays an important regularizing role due to the following.First. The theory becomes explicitly covariant under the local Lorentz transformations of the coframe; that is, the Lagrangian (7) is invariant under the change of variables
(12)ϑ′α=Λαβϑβ,Γα′β=ΛμαΓμν(Λ-1)βν-(Λ-1)βγd(Λ)γα.
Due to the noncovariant transformation law of Γαβ, see (12), if a connection vanishes in a given frame, it will not vanish in any other frame related to the first by a local Lorentz transformation. When Γαβ=0for all frames, which is the tetrad gravity, the Lagrangian (7) is invariant under the local Lorentz group.Second. Γαβ plays an important role in the teleparallel framework. This role represents the inertial effects which arise from the choice of the reference system [79]. The contributions of this inertial in many cases lead to unphysical results for the total energy of the system. Therefore, the role of the teleparallel connection is to separate the inertial contribution from the truly gravitational one. Since the teleparallel curvature is zero, the connection is a pure gauge; that is,
(13)Γαβ=def.(Λβγ)-1d(Λγα).
The Weitzenböck connection always has the form (13). The translational momentum has the form [72, 80]
(14)H~α=12κΓ~βγ∧ηαβγ,E~α=12[(eα⌋dϑβ)∧H~β-dϑβ∧(eα⌋H~β)],Γαβ=def.Γ~αΓ~β-Kαβ,
where Γ~αΓ~β is the purely Riemannian connection and Kμν is the contorsion 1-form which is related to the torsion through the relation
(15)Tα=def.Kαβ∧ϑβ.The teleparallel model (7) belongs to the class of quasi-invariant theories. In fact, one can verify that under a change of the coframe ϑ′β=(Λ(x)αβ)ϑ′β, the Lagrangian changes by a total derivative as follows:
(16)V~(ϑ′)=V~(ϑ)-12κd[(Λ-1)αβdΛβγ∧ηγα].
In addition to (16), it is easy to verify that (14) changes like
(17)H~α′(ϑ′)=(Λ-1)βαH~β(ϑ)-12κd[(Λ-1)βα(Λ-1)νγdΛγμ∧ηβμν],E~α′(ϑ′)=(Λ-1)βαE~β(ϑ)+d(Λ-1)βα∧H~β(ϑ)-12κd[(Λ-1)βα(Λ-1)νγdΛγμ∧ηβμν].The total conserved charge in the tetrad gravity theory is given by [48, 49]
(18)𝒬~(ξ,ϑ)=∫∂S‍ξαH~α=12κ∫∂S‍ξαΓ~βγ∧ηαβγ,
where ξα=ξ⌋ϑα. Under a local Lorentz transformation, (18) transforms as
(19)𝒬~′(ξ,ϑ)=𝒬~(ξ,ϑ)-12κ∫∂S‍ξα(Λ-1)νγdΛγμ∧ηαμν=12κ∫∂S‍ξα(Γ~βγ-Γ-βγ)∧ηαμν,
where Γ-μν=(Λ-1)γνdΛγμ. The vector ξ=ζi∂i does not depend on the choice of the frame, while its components, that is, ξα, transform as a vector. Now let use apply (18) to different coframes.


## 3. Total Conserved Charges of the Kerr-Newman Spacetimes

### 3.1. First Coframe

The covariant form of the first charged rotating tetrad, that is, KN, field having axial symmetry in spherical coordinates(t,r,θ,ϕ) can be written as(20)(hαi)I=(𝒜ℬ𝒞000-(2Mr-q2)asinθcosθ𝒜𝒞-𝒜ℬsinθcosϕ-sinθsinϕ𝒜-𝒞𝒜sinθcosθ(2Mr-q2)asin2θ𝒜𝒞-𝒜ℬcosθcosϕ-cosθsinϕ𝒜𝒞𝒜sin2θ0𝒜ℬsinϕ-cosϕ𝒜0).𝒜, ℬ, and 𝒞 are three functions of r and θ having the form
(21)𝒜=r2+a2cos2θ,ℬ=r2-2Mr+a2+q2,𝒞=(r2+a2)(r2+a2cos2θ)+(2Mr-q2)a2sin2θ,
where M, a, and q are mass, rotation and charge parameters, respectively [44–47]. An asymptotically flat spacetime is considered in this study, and a boundary condition, that for r→∞ the tetrad (20) approaches the tetrad of Minkowski spacetime in Cartesian coordinates, is imposed. The metric tensor gij=def.oμνhμihνj associated with the tetrad field (20) has the form
(22)ds2=(1-[2Mr-q2]𝒜)dt2-𝒜ℬdr2-𝒜dθ2-{(r2+a2)+[2Mr-q2]a2sin2θ𝒜}sin2θdϕ2-2[2Mr-q2]asin2θ𝒜dtdϕ,
which is the KN metric written in the Boyer-Lindquist coordinates [44–47].In spherical local coordinates, the first rotating frame is taken to be described by the coframe(23)ϑKNIα=(Λαγ)ϑIγ,whereϑIγ=(hγi)Idxi.The local Lorentz transformation,Λαγ, is given by the matrix [44–47]
(24)(Λαγ)=(10000sinθcosϕcosθcosϕ-sinϕ0sinθsinϕcosθsinϕcosϕ0cosθ-sinθ0).
Using (23) and (24), one gets
(25)ϑKNI0=-𝒜ℬ𝒞dt,ϑKNI1=𝒜ℬdr,ϑKNI2=𝒜dθ,ϑKNI3=sinθ{𝒞dϕ+[2Mr-q2]dt}𝒜𝒞.The nonvanishing components of the Riemannian connection, of the first coframe, have the form(26)Γ~1^0^=1𝒜2𝒞{asin2θ{M(3r4+r2a2+a2cos2θ[r2-a2])1𝒜2𝒞asin2θcc-rq2𝒜+(r2+a2)}dϕ1A2CC-(r2+a2){M(r2-a2cos2θ)-rq2}dt},Γ~1^2^=-a2sinθcosθdr+rℬdθ𝒜ℬ,Γ~1^3^=sinθℬ𝒞𝒜2({r𝒜2-a2sin2θ[M(r2-a2cos2θ)-q2r]}dϕsinθℬ𝒞𝒜2c+[Ma(r2-a2cos2θ)-q2r]cdt),Γ~2^0^=-(2Mr-q2)a2ℬsinθcosθ𝒞𝒜2(asin2θdϕ+dt),Γ~2^3^=cosθ𝒞𝒜2({𝒜2(r2+a2)+[2Mr-q2]a2sin2θcosθ𝒞𝒜2-cl×(2r2+a2(1+cos2θ))}dϕcosθ𝒞𝒜2-c-[2Mr-q2]a(r2+a2)dt),Γ~3^0^=asinθ2ℬ𝒞𝒜{[2M(3r4+r2a2+a2cos2θ[r2-a2])asinθ2ℬ𝒞𝒜cc-q2{4r3+2ra2(1+cos2θ)}]drasinθ2ℬ𝒞𝒜c-(2Mr-q2)a2sinθcosθℬdθ}.
Using (25), the nonvanishing components of the vector ξα have the form
(27)ξ0=𝒜ℬ𝒞ζ0,ξ1=𝒜ℬζ1,ξ2=𝒜ζ2,ξ3={𝒞ζ3+(2Mr-q2)aζ0}sinθ𝒜𝒞.
If we take tetrad (20), as well as the trivial Weitzenböck connection, Γαβ=0, we finally get the nonvanishing components of the translation momentumthat is, H~α^,
(28)H~0^=-sinθ(dθ∧dϕ)(4Mr+a2sin2θ-2q2)4πr+⋯,H~3^=-asin2θ(dθ∧dϕ)(2r2+6Mr-a2cos2θ-4q2)4πr2+⋯,
where ⋯ means terms which are multiplied by dθ∧dr, dθ∧dt,dr∧dϕ, and so forth. By using the identities of [36], that is, (A18), one can directly prove that, for solutions with vanishing torsion, the Killing equation ℒζϑα=0 implies also that ℒζΓαβ=0. Therefore, for the Kerr-Newman solution we have ℒζΓαβ=0 for ζ=ξ0∂0+ξ3∂ϕ, with constants ξ0 and ξ3. For a vector field ξ=ξαeα=ζi∂i with constant holonomic components, ζi, in the coordinate system used in (20), the direct evaluation of the integral (18) yields the following infinite total conserved charge:
(29)𝒬=∫∂S‍ξαH~α=(M-q22r)ζ0-(r3+M)aζ3.For the coframeϑKNIα=(Λαγ)ϑIγ determined by (25), the conserved charges corresponding to the diffeomorphism generated by the shift along the time coordinate has a usual value M-q2/2r of the total energy of the configuration. Whereas, for the vector field along the azimuthal coordinate we get (-ra/3-Ma), which is a nonfamiliar term [80]. This is because tetrad (20) is nonholonomic. Another reason is that the Riemannian connection Γ~(ϑ′) does not vanish either at spatial infinity or when the physical quantities, M=0, a=0, and q=0, are vanishing. The nonvanishing of the Riemannian connection may be responsible for the divergence of the integral of the conserved charges.


## 3.1. First Coframe

The covariant form of the first charged rotating tetrad, that is, KN, field having axial symmetry in spherical coordinates(t,r,θ,ϕ) can be written as(20)(hαi)I=(𝒜ℬ𝒞000-(2Mr-q2)asinθcosθ𝒜𝒞-𝒜ℬsinθcosϕ-sinθsinϕ𝒜-𝒞𝒜sinθcosθ(2Mr-q2)asin2θ𝒜𝒞-𝒜ℬcosθcosϕ-cosθsinϕ𝒜𝒞𝒜sin2θ0𝒜ℬsinϕ-cosϕ𝒜0).𝒜, ℬ, and 𝒞 are three functions of r and θ having the form
(21)𝒜=r2+a2cos2θ,ℬ=r2-2Mr+a2+q2,𝒞=(r2+a2)(r2+a2cos2θ)+(2Mr-q2)a2sin2θ,
where M, a, and q are mass, rotation and charge parameters, respectively [44–47]. An asymptotically flat spacetime is considered in this study, and a boundary condition, that for r→∞ the tetrad (20) approaches the tetrad of Minkowski spacetime in Cartesian coordinates, is imposed. The metric tensor gij=def.oμνhμihνj associated with the tetrad field (20) has the form
(22)ds2=(1-[2Mr-q2]𝒜)dt2-𝒜ℬdr2-𝒜dθ2-{(r2+a2)+[2Mr-q2]a2sin2θ𝒜}sin2θdϕ2-2[2Mr-q2]asin2θ𝒜dtdϕ,
which is the KN metric written in the Boyer-Lindquist coordinates [44–47].In spherical local coordinates, the first rotating frame is taken to be described by the coframe(23)ϑKNIα=(Λαγ)ϑIγ,whereϑIγ=(hγi)Idxi.The local Lorentz transformation,Λαγ, is given by the matrix [44–47]
(24)(Λαγ)=(10000sinθcosϕcosθcosϕ-sinϕ0sinθsinϕcosθsinϕcosϕ0cosθ-sinθ0).
Using (23) and (24), one gets
(25)ϑKNI0=-𝒜ℬ𝒞dt,ϑKNI1=𝒜ℬdr,ϑKNI2=𝒜dθ,ϑKNI3=sinθ{𝒞dϕ+[2Mr-q2]dt}𝒜𝒞.The nonvanishing components of the Riemannian connection, of the first coframe, have the form(26)Γ~1^0^=1𝒜2𝒞{asin2θ{M(3r4+r2a2+a2cos2θ[r2-a2])1𝒜2𝒞asin2θcc-rq2𝒜+(r2+a2)}dϕ1A2CC-(r2+a2){M(r2-a2cos2θ)-rq2}dt},Γ~1^2^=-a2sinθcosθdr+rℬdθ𝒜ℬ,Γ~1^3^=sinθℬ𝒞𝒜2({r𝒜2-a2sin2θ[M(r2-a2cos2θ)-q2r]}dϕsinθℬ𝒞𝒜2c+[Ma(r2-a2cos2θ)-q2r]cdt),Γ~2^0^=-(2Mr-q2)a2ℬsinθcosθ𝒞𝒜2(asin2θdϕ+dt),Γ~2^3^=cosθ𝒞𝒜2({𝒜2(r2+a2)+[2Mr-q2]a2sin2θcosθ𝒞𝒜2-cl×(2r2+a2(1+cos2θ))}dϕcosθ𝒞𝒜2-c-[2Mr-q2]a(r2+a2)dt),Γ~3^0^=asinθ2ℬ𝒞𝒜{[2M(3r4+r2a2+a2cos2θ[r2-a2])asinθ2ℬ𝒞𝒜cc-q2{4r3+2ra2(1+cos2θ)}]drasinθ2ℬ𝒞𝒜c-(2Mr-q2)a2sinθcosθℬdθ}.
Using (25), the nonvanishing components of the vector ξα have the form
(27)ξ0=𝒜ℬ𝒞ζ0,ξ1=𝒜ℬζ1,ξ2=𝒜ζ2,ξ3={𝒞ζ3+(2Mr-q2)aζ0}sinθ𝒜𝒞.
If we take tetrad (20), as well as the trivial Weitzenböck connection, Γαβ=0, we finally get the nonvanishing components of the translation momentumthat is, H~α^,
(28)H~0^=-sinθ(dθ∧dϕ)(4Mr+a2sin2θ-2q2)4πr+⋯,H~3^=-asin2θ(dθ∧dϕ)(2r2+6Mr-a2cos2θ-4q2)4πr2+⋯,
where ⋯ means terms which are multiplied by dθ∧dr, dθ∧dt,dr∧dϕ, and so forth. By using the identities of [36], that is, (A18), one can directly prove that, for solutions with vanishing torsion, the Killing equation ℒζϑα=0 implies also that ℒζΓαβ=0. Therefore, for the Kerr-Newman solution we have ℒζΓαβ=0 for ζ=ξ0∂0+ξ3∂ϕ, with constants ξ0 and ξ3. For a vector field ξ=ξαeα=ζi∂i with constant holonomic components, ζi, in the coordinate system used in (20), the direct evaluation of the integral (18) yields the following infinite total conserved charge:
(29)𝒬=∫∂S‍ξαH~α=(M-q22r)ζ0-(r3+M)aζ3.For the coframeϑKNIα=(Λαγ)ϑIγ determined by (25), the conserved charges corresponding to the diffeomorphism generated by the shift along the time coordinate has a usual value M-q2/2r of the total energy of the configuration. Whereas, for the vector field along the azimuthal coordinate we get (-ra/3-Ma), which is a nonfamiliar term [80]. This is because tetrad (20) is nonholonomic. Another reason is that the Riemannian connection Γ~(ϑ′) does not vanish either at spatial infinity or when the physical quantities, M=0, a=0, and q=0, are vanishing. The nonvanishing of the Riemannian connection may be responsible for the divergence of the integral of the conserved charges.


## 4. Total Charge of KN Spacetime Using Regularized Conserved Invariant Charge

One possible solution of the above unfamiliar result is the use of regularized form of total charges(30)𝒬~(ξ,ϑ)=12κ∫∂S‍ξα(Γ~βγ-Γβγ)∧ηαβγ,
where Γβγ has the form
(31)Γαβ=(Λ-1)βγdΛγα.The most appropriate local Lorentz transformation which serves for this purpose has the form (24). The nonvanishing components of Γβγ have the form
(32)Γ1^2^=-dθ,Γ1^3^=-sinθdϕ,Γ2^3^=-cosθdϕ.
Using (26), (27), and (32) in (30) and the fact that the vector field ξ is with constant holonomic components, we get the total conserved quantities in the form
(33)𝒬~(ξ,ϑ)=∫∂S‍ξα(Γ~βγ-Γβγ)∧ηαβγ=(M-q22r)ζ0-Maζ3.
It is observed that the last term in (30) acts as a regularizing term in removing divergence.


### 4.1. Second Coframe

The covariant form of the second KN tetrad field can be written as(34)(hαi)II=(-a2sin2θ-𝒜1ℬ𝒜00-a𝒜1sin2θ(ℬ-𝒜1)𝒜-a(ℬ-𝒜1)sinθsinϕ𝒜rsinθcosϕℬ𝒜1cosθcosϕ-sinθsinϕ(a2sin2θℬ-𝒜13/2)𝒜a(ℬ-𝒜1)sinθcosϕ𝒜rsinθsinϕℬ𝒜1cosθsinϕ-sinθcosϕ(a2sin2θℬ-𝒜13/2)𝒜0𝒜1ℬcosθ-rsinθ0),where𝒜1 has the form
(35)𝒜1=r2+a2.
Tetrad (34) has the same associated metric of tetrad (20). The second rotating frame is described by the coframe components
(36)ϑKNIIα=(Λαγ)ϑIIγ,whereϑIIγ=(hγi)IIdxi.
Using (24) and (34), one can get
(37)ϑKNII0=-a𝒜1sin2θ(ℬ-𝒜1)dϕ+(a2sin2θ-𝒜1ℬ)dt𝒜,ϑKNII1=-(rsin2θ+𝒜1cos2θ)dr+sinθcosθℬ[𝒜1-r]dθℬ,ϑKNII2=-sinθcosθ[r-𝒜1]dr+ℬ[rsin2θ+cos2θ𝒜1]dθℬ,ϑKNII3=-sinθ[𝒜13/2-a2sin2θℬ]dϕ+a[ℬ-𝒜1]dt𝒜.
The two frames (25) and (37) are related through the local Lorentz transformation; that is,
(38)ϑKN1α=(Λ1αγ)ϑKN2γ,
where (Λ1αγ) has the form(39)(Λ1αγ)=(-100-(𝒜2𝒜3-r5+2r4M-r3q2-ra4cos2θ)asinθr2(r4-2r3M+r2q2+a4cos2θ)0-10000-10(𝒜2-r)asinθr𝒜200-1),where(40)𝒜2=r2-2M+q2,𝒜3=[r4+a4cos2θ].Coframe (37) has the following asymptotic nonvanishing components of Riemannian connection up to O(1/r4): (41)Γ~1^0^≅-[4Mr-3q2]asin2θdϕ-2[Mr-q2]dt2r3+O(1r4),Γ~1^2^≅-[2r2-2Mr+q2]dθ2r3+(1r4),Γ~1^3^≅-sinθ(r[2r2-2Mr+q2]dϕ+2Macdt)2r3+(1r4),Γ~2^0^≅[2Mr-q2]asinθcosθdϕ2r3+(1r4),Γ~2^3^≅-cosθ[2r3dϕ-4Madt]2r3+(1r4).
(Terms like Ma2, M2, Mq2, …, are neglected in these calculations.) The asymptotic nonvanishing components of the vector ξα have the form
(42)ξ0≅(2r2-2Mr+q2)ζ0+2Marsin2θζ32r2+(1r3),ξ1≅-(2r2+Mr-a2sin2θ-q2)ζ1+a2sinθcosθζ22r2ζ1+(1r3),ξ2≅-2r2+a2cos2θ2rζ2+(1r3),ξ3=sinθ[2Maζ0-(2r3+ra2)ζ3]2r2+(1r3).Using coframe (37) as well as the trivial Weitzenböck connection, one can get asymptotically the nonvanishing components of the translation momentum, that is, H~α^,
(43)H~0^≅sinθ16πr[4Mr-4r2-a2-2q2](dθ∧dϕ)+⋯+O(1r3),H~3^≅asin2θ(Mr-q2)8πr2(dθ∧dϕ)+⋯+O(1r3).
The direct evaluation of the integral (18), using (42) and (43) and assuming the fact that the vector field ξ is with constant holonomic components, yields the following infinite total conserved charge:
(44)𝒬=∫∂S‍ξαH~α=-(r-2M-q2r+a24r)ζ0-aMζ3.
For the tetrad ϑKNIIα=(Λαγ)ϑIIγ determined by (37), the conserved charge corresponding to the diffeomorphism generated by the shift along the time coordinate has a divergent value -(r-2M-q2/r+a2/4r) of the total energy of the configuration whereas, for the vector field along the azimuthal coordinate, we get -aM, which is a well-known value [80]. It is worth to mention that when one uses (19) to calculate the total conserved quantities related to coframe (37), one also does not get the standard value; that is,
(45)𝒬~=(M-q22r+a26r)ζ0-(2M+r3)aζ3.
The only gain obtained from the use of (19), when it is used to calculate the total charge, is in fact that it removes the divergence from the time coordinate and gives the correct value of energy along the time coordinate; however, the value of the angular momentum along the azimuthal coordinate becomes unfamiliar and divergent. Therefore, we are going to use other conserved charges to overcome the previous problem.


## 4.1. Second Coframe

The covariant form of the second KN tetrad field can be written as(34)(hαi)II=(-a2sin2θ-𝒜1ℬ𝒜00-a𝒜1sin2θ(ℬ-𝒜1)𝒜-a(ℬ-𝒜1)sinθsinϕ𝒜rsinθcosϕℬ𝒜1cosθcosϕ-sinθsinϕ(a2sin2θℬ-𝒜13/2)𝒜a(ℬ-𝒜1)sinθcosϕ𝒜rsinθsinϕℬ𝒜1cosθsinϕ-sinθcosϕ(a2sin2θℬ-𝒜13/2)𝒜0𝒜1ℬcosθ-rsinθ0),where𝒜1 has the form
(35)𝒜1=r2+a2.
Tetrad (34) has the same associated metric of tetrad (20). The second rotating frame is described by the coframe components
(36)ϑKNIIα=(Λαγ)ϑIIγ,whereϑIIγ=(hγi)IIdxi.
Using (24) and (34), one can get
(37)ϑKNII0=-a𝒜1sin2θ(ℬ-𝒜1)dϕ+(a2sin2θ-𝒜1ℬ)dt𝒜,ϑKNII1=-(rsin2θ+𝒜1cos2θ)dr+sinθcosθℬ[𝒜1-r]dθℬ,ϑKNII2=-sinθcosθ[r-𝒜1]dr+ℬ[rsin2θ+cos2θ𝒜1]dθℬ,ϑKNII3=-sinθ[𝒜13/2-a2sin2θℬ]dϕ+a[ℬ-𝒜1]dt𝒜.
The two frames (25) and (37) are related through the local Lorentz transformation; that is,
(38)ϑKN1α=(Λ1αγ)ϑKN2γ,
where (Λ1αγ) has the form(39)(Λ1αγ)=(-100-(𝒜2𝒜3-r5+2r4M-r3q2-ra4cos2θ)asinθr2(r4-2r3M+r2q2+a4cos2θ)0-10000-10(𝒜2-r)asinθr𝒜200-1),where(40)𝒜2=r2-2M+q2,𝒜3=[r4+a4cos2θ].Coframe (37) has the following asymptotic nonvanishing components of Riemannian connection up to O(1/r4): (41)Γ~1^0^≅-[4Mr-3q2]asin2θdϕ-2[Mr-q2]dt2r3+O(1r4),Γ~1^2^≅-[2r2-2Mr+q2]dθ2r3+(1r4),Γ~1^3^≅-sinθ(r[2r2-2Mr+q2]dϕ+2Macdt)2r3+(1r4),Γ~2^0^≅[2Mr-q2]asinθcosθdϕ2r3+(1r4),Γ~2^3^≅-cosθ[2r3dϕ-4Madt]2r3+(1r4).
(Terms like Ma2, M2, Mq2, …, are neglected in these calculations.) The asymptotic nonvanishing components of the vector ξα have the form
(42)ξ0≅(2r2-2Mr+q2)ζ0+2Marsin2θζ32r2+(1r3),ξ1≅-(2r2+Mr-a2sin2θ-q2)ζ1+a2sinθcosθζ22r2ζ1+(1r3),ξ2≅-2r2+a2cos2θ2rζ2+(1r3),ξ3=sinθ[2Maζ0-(2r3+ra2)ζ3]2r2+(1r3).Using coframe (37) as well as the trivial Weitzenböck connection, one can get asymptotically the nonvanishing components of the translation momentum, that is, H~α^,
(43)H~0^≅sinθ16πr[4Mr-4r2-a2-2q2](dθ∧dϕ)+⋯+O(1r3),H~3^≅asin2θ(Mr-q2)8πr2(dθ∧dϕ)+⋯+O(1r3).
The direct evaluation of the integral (18), using (42) and (43) and assuming the fact that the vector field ξ is with constant holonomic components, yields the following infinite total conserved charge:
(44)𝒬=∫∂S‍ξαH~α=-(r-2M-q2r+a24r)ζ0-aMζ3.
For the tetrad ϑKNIIα=(Λαγ)ϑIIγ determined by (37), the conserved charge corresponding to the diffeomorphism generated by the shift along the time coordinate has a divergent value -(r-2M-q2/r+a2/4r) of the total energy of the configuration whereas, for the vector field along the azimuthal coordinate, we get -aM, which is a well-known value [80]. It is worth to mention that when one uses (19) to calculate the total conserved quantities related to coframe (37), one also does not get the standard value; that is,
(45)𝒬~=(M-q22r+a26r)ζ0-(2M+r3)aζ3.
The only gain obtained from the use of (19), when it is used to calculate the total charge, is in fact that it removes the divergence from the time coordinate and gives the correct value of energy along the time coordinate; however, the value of the angular momentum along the azimuthal coordinate becomes unfamiliar and divergent. Therefore, we are going to use other conserved charges to overcome the previous problem.


## 5. Total Conserved Charge Using the PG Version of TEGR and Discussion on the Choice of the Frame

Obukhov et al. [48, 49] show that teleparallel gravity can be naturally defined as a particular case of PG gravity [63], and from the Lagrangian of this theory, that is, the Lagrangian of PG gravity, they derived the invariant conserved charges for the teleparallel model to have the form
(46)𝒬~1(ξ,ϑ)=12κ∫∂S‍[ξα(Γ~βγ-Γβγ)∧ηαβγ-Ξαβηαβ],
where Ξαβ is defined as
(47)Ξαβ=def.ξ⌋Γαβ+Θαβ,Γαβ=(ΛI-1)αγdΛIγβ,Θαβ=e[α⌋ℓξϑβ],
where ΛIγβ is an appropriate choice of local Lorentz transformation. (We will denote the antisymmetric part by the square bracket [], A[μν]=(1/2)(Aμν-Aνμ).) (The Lie derivative is given on exterior forms by ℓξ=dξ⌋+ξ⌋d.)  Obukhov et al. [48, 49] show that the last term in (46) acts as a regularized term for the calculation of the total conserved charge.Equation (46) is employed to calculate the total conserved charges (Table 1) associated with frame (38). The appropriate matrix of local Lorentz transformation, (ΛIαγ), has the form
(48)(ΛIαγ)=def.(100asinθr-asinθsinϕrsinθcosϕcosθcosϕ-sinϕasinθcosϕrsinθsinϕcosθsinϕcosϕ0cosθ-sinθ0).
Using (48), we get the nonvanishing components of Γαβ(49)Γ0^1^=-asin2θdϕr,Γ0^2^=-asinθcosθdϕr,Γ0^3^=--a(rcosθdθ-sinθdr)r2,Γ1^2^=-dθ,Γ1^3^=-sinθdϕ,Γ2^3^=-cosθdϕ,
and the nonvanishing components of Θαβ have the form
(50)Θ01=-2asin2θζ3r,Θ02=-asin2θζ3r,Θ03=2a(rcosθζ2-sinθζ1)r2,Θ12=-2ζ2,Θ13=-2sinθζ3,Θ23=-2cosθζ3.
Finally, the nonvanishing components of Ξαβ have the form
(51)Ξ01=-aζ3sin2θr,Ξ02=-aζ3sinθcosθr,Ξ13=-ζ3sinθ,Ξ23=-ζ3cosθ.
Using (41), (42), (49), and (51) in (46), we finally get the total conserved charge of coframe (37) in the form
(52)𝒬~1(ξ,ϑ)≅12κ∫∂S‍[ξα(Γ~βγ-Γβγ)∧ηαβγ+Ξαβηαβ]=(M-q22r)ζ0-Maζ3.
Equation (52) shows that the total energy and the total angular momentum of coframe (37) have their commonly known form.Table 1
Comparison between the results of the total conserved charges and the other definitions.
Spacetime
Conserved charge in the tetrad gravity
Regularized conserved charge
Invariant conserved charge
Definition of conserved charge
𝒬
(
ξ
,
ϑ
)
=
∫
∂
S
‍
ξ
α
H
~
α
=
1
2
κ
∫
∂
S
‍
ξ
α
Γ
~
β
γ
∧
η
α
β
γ
𝒬
~
(
ξ
,
ϑ
)
=
1
2
κ
∫
∂
S
‍
ξ
α
(
Γ
~
β
γ
-
Γ
β
γ
)
∧
η
α
β
γ
𝒬
1
~
(
ξ
,
ϑ
)
=
1
2
κ
∫
∂
S
‍
[
ξ
α
(
Γ
~
β
γ
-
Γ
β
γ
)
∧
η
α
β
γ
+
Ξ
α
β
η
α
β
]
First coframe
(
M
-
q
2
2
r
)
ζ
0
-
(
r
3
+
M
)
a
ζ
3
(
M
-
q
2
2
r
)
ζ
0
-
M
a
ζ
3
Second coframe
-
(
r
-
2
M
-
q
2
r
+
a
2
4
r
)
ζ
0
-
a
M
ζ
3
(
M
-
q
2
2
r
+
a
2
6
r
)
ζ
0
-
(
2
M
+
r
)
a
3
ζ
3
(
M
-
q
2
2
r
)
ζ
0
-
M
a
ζ
3
Third coframe
(
M
-
q
2
2
r
)
ζ
0
-
4
M
a
3
ζ
3
(
M
-
q
2
2
r
)
ζ
0
-
(
4
M
-
r
3
)
a
ζ
3
(
M
-
q
2
2
r
)
ζ
0
-
M
a
ζ
3
Fourth coframe
(
M
-
q
2
2
r
)
ζ
0
-
(
2
M
-
r
)
a
3
ζ
3
(
M
-
q
2
2
r
)
ζ
0
-
2
M
a
3
ζ
3
(
M
-
q
2
2
r
)
ζ
0
-
M
a
ζ
3
Fifth coframe
(
M
-
q
2
2
r
)
ζ
0
-
(
M
-
r
3
)
a
ζ
3
(
M
-
q
2
2
r
)
ζ
0
-
M
a
3
ζ
3
(
M
-
q
2
2
r
)
ζ
0
-
M
a
ζ
3


### 5.1. Third Coframe

The covariant form of the third KN tetrad can be written as(53)(hαi)III=(ℬ𝒜00-asin2θℬ𝒜asinθsinϕ𝒜sinθcosϕ𝒜ℬcosθcosϕ𝒜sinθsinϕ(r2+a2)𝒜-asinθcosϕ𝒜sinθsinϕ𝒜ℬcosθsinϕ𝒜-sinθcosϕ(r2+a2)𝒜0cosθ𝒜ℬ-sinθ𝒜0).Tetrad field (53) has the same associated metric of tetrad field (20). Using the spherical local coordinates (t,r,θ,ϕ), the third rotating frame is described by the coframe components
(54)ϑKNIIIα=(Λαγ)ϑIIIγ,whereϑIIIα=(hαi)IIIdxi.
Using (24) and (53) we get
(55)ϑIII0^=-ℬ𝒜(cdt+asin2θdϕ),ϑIII1^=𝒜ℬdr,ϑIII2^=𝒜dθ,ϑIII3^=sinθ[(r2+a2)dϕ+adt]𝒜.The two frames (25) and (55) are related through local Lorentz transformation; that is,
(56)ϑKNIα=(Λ2αγ)ϑKNIIIγ,
where (Λ2αγ) has the form
(57)(Λ2αγ)=((r2+a2)𝒞00aℬsinθ𝒞01000010aℬsinθ𝒞00(r2+a2)𝒞).
The nonvanishing components of the corresponding Riemannian connection of the coframe (55) read
(58)Γ~1^0^=-(×(𝒜2)-1(asin2θ{r2(r+M)+a2cos2θ(r-M)-rq2}dϕ-{M(r2-a2cos2θ)-rq2}dt)×(𝒜2)-1),Γ~1^2^=-a2sinθcosθdr+rℬdθ𝒜ℬ,Γ~1^3^=-rsinθℬdϕ𝒜,Γ~2^0^=asinθcosθℬdϕ𝒜,Γ~2^3^=-cosθ{𝒞dϕ-(2Mr-q2)acdt}𝒜2,Γ~3^0^=rasinθdr-cosθℬdϕ𝒜ℬ.The nonvanishing components of the vectorξα have the form
(59)ξ0=-ℬ𝒜(ζ0+asin2θζ3),ξ1=𝒜ℬζ1,ξ2=𝒜ζ2,ξ3=sinθ𝒜(aζ0+[r2+a2]ζ3).
If we take coframe (55), as well as the trivial Weitzenböck connection, one can get asymptotically the nonvanishing components of the translation momentum
(60)H~0^≅-sinθ(2Mr-q2)(dθ∧dϕ)4rπ+⋯+O(1r2),H~3^=O(1r2).
The direct evaluation of integral (18) yields the following anomalous conserved charge:
(61)𝒬=∫∂S‍ξαH~α=(M-q22r)ζ0-4aMζ33.It is worth mentioning that when one uses (19) to calculate the conserved quantities related to coframe (55), one can get (-(4M-r)aζ3)/3 in the azimuthal direction, and the conserved quantity along the time coordinate does not change. Therefore, we are going to use (46) to calculate the total conserved quantities related to coframe (55). The appropriate matrix of local Lorentz transformation is given by (48). Using the data calculated for the second coframe, that is, using (50), (51), (58), and (59) in (46), we get the conserved charge related to coframe (55) as given by (52).


### 5.2. Fourth Rotating Frame

The covariant form of the fourth rotating tetrad field having axial symmetry in spherical coordinates can be written as(62)(hαi)4=(A1A2A3A4B1sinθcosϕB2sinθcosϕB3cosθcosϕB4sinϕsinθC1sinθsinϕC2sinθsinϕC3cosθsinϕC4cosϕsinθD1cosθD2cosθD3sinθD4cosθ),whereAi, Bi, Ci, and Di read
(63)A1=1-[Mr-q2/2]𝒜,A2=[Mr-q2/2]ℬ,A3=0,A4=[Mr-q2/2]asin2θ𝒜,B1=[Mr-q2/2]𝒜,B2=1ℬcosϕ(rα-[Mr-q22]cosϕ),B3=αcosϕ,B4=β-(([Mr-q2/2]asin2θcosϕ)/𝒜)sinϕ,C1=[Mr-q2/2]𝒜,C2=1Υsinϕ(rβ-[Mr-q22]sinϕ),C3=βsinϕ,C4=-α+([Mr-q2/2]asin2θsinϕ/𝒜)cosϕ,D1=[Mr-q2/2]𝒜,D2=1+[Mr-q2/2]ℬ,D3=-r,D4=-[Mr-q2/2]asin2θ𝒜,
where α  and  β are defined by
(64)α=rcosϕ+asinϕ,β=rsinϕ-acosϕ.Using the spherical local coordinates(t,r,θ,ϕ) the fourth rotating frame is described by the coframe components
(65)ϑKNIVα=(Λαγ)ϑIVγ,whereϑIVγ=(hγi)IVdxi,
Using (24) and (62), we get
(66)ϑIV0^=A1cdt+A2dr+A3dθ+A4dϕ,ϑIV1^=B1sinθcosϕcdt+B2sinθcosϕdr+B3cosθcosϕdθ+B4sinθsinϕdϕ,ϑIV2^=C1sinθsinϕcdt+C2sinθsinϕdr+C3cosθsinϕdθ+C4sinθcosϕdϕ,ϑIV3^=D1cosθcdt+D2cosθdr+D3sinθdθ+D4cosθdϕ.
The local Lorentz transformation Λαγ is given by the matrix (24). The two frames (25) and (66) are related through local Lorentz transformation; that is,
(67)ϑKNIα=(Λ3αγ)ϑKNIVα,
where (Λ3αγ) has the form(68)(Λ3αγ)=(ℱ1𝒜ℬ2ℱ2𝒞-M1ℱ3𝒜ℬsinθcosθℱ2𝒞-M1ℱ4𝒜ℬℱ2𝒞M1ℱ5𝒜ℬsinθℱ2𝒞-M1𝒜ℬ-sinθcosθℱ62𝒜ℬℱ72𝒜ℬsinθℱ82𝒜ℬ0ℱ9𝒜-sinθcosθℱ10𝒜cosθℱ11𝒜-M1asinθ𝒜𝒞-cosθℱ122𝒜𝒞-sinθℱ132𝒜𝒞ℱ142𝒜𝒞),with(69)M1=[Mr-q22],ℱ1=2r4-2Mr3+2r2a2cos2θ+2r2a2-4Ma2rcos2θ+2Mra2+2a4cos2θ+q2(r2+a2cos2θ),ℱ2=r4-2Mr3+r2a2cos2θ+r2a2-2Ma2rcos2θ+a4cos2θ+q2𝒜,ℱ3=r2(sin2ϕ-1)-a2(sin2ϕ+1)-2racos2ϕ,ℱ4=(r2+a2)(sin2ϕsin2θ+cos2θ)+2arsin2θcos2ϕ,ℱ5=-(r2+a2)cos2ϕ+2arsin2ϕ,ℱ6=2r(r-M)(1-sin2ϕ)+2a2+2arcos2ϕ+q2(1+sin2ϕ),ℱ7=(M2r-2r2-q2)(sin2ϕsin2θ+cos2θ)-2arsin2θcos2ϕ-2a2cos2θ,ℱ8=(2r2-2Mr+q2)cos2ϕ+2racos2ϕ,ℱ9=r(sin2θ+sin2ϕcos2θ)-acos2θcos2ϕ,ℱ10=r(1-sin2ϕ)+acos2ϕ,ℱ11=rcos2ϕ+asin2ϕ,ℱ12=2r3cos2ϕ+asin2ϕ(2r2+[2Mr-q2]sin2θ+2a2cos2θ)-a([2Mr-q2]sin2θ-2arcos2θcos2ϕ),ℱ13=2r3cos2ϕ+asin2ϕ(2r2+[2Mr-q2]sin2θ+a2cos2θ)+a([2Mr-q2]cos2θ+acos2θcos2ϕ),ℱ14=2r3sin2ϕ-acos2ϕ(2r2+[2Mr-q2]sin2θ+a2cos2θ)+2a2rsin2ϕcos2θ.
The nonvanishing components of the Riemannian connection of the coframe (66) up to order O(1/r3) read
(70)Γ~1^0^≅[M-q22r]×((2r2)-1(sin2θsin2θ[(1-sin2ϕ)(dr+cdt)+rcos2ϕdϕ]+r(sin2θ+sin2ϕcos2θ)dθ)×(2r2)-1)+O(1r3),Γ~1^2^≅(((2r-2[M-q22r]sin2ϕ)dθ+[M-q22r]×sin2θcos2ϕdϕ[M-q22r])×(2r)-1)+O(1r3),Γ~1^3^≅-12r2sinθ×(asin2θdr+2[M-q22r]rsin2θcos2ϕdθ+sin2θ(3r2-r[M-q22r]sin2θ[1-sin2ϕ])dϕ)+O(1r3),Γ~2^0^≅-[M-q22r]×(((cos2θ+sin2θsin2ϕ)(dr+cdt)+rsin2θ2×(1-sin2ϕ)dθ+rsin2θcos2ϕdϕrsin2θ2)×(r2)-1)+O(1r3),Γ~2^3^≅-12r2(2asinθdr-2[M-q22r]rcosθcos2ϕdθ+2sinθ(3r2-[M-q22r]r[sin2θ+sin2ϕcos2θ])dϕ)+O(1r3),Γ~3^0^≅-[M-q22r]((r2)-1(sinθcos2ϕ(dr+cdt)-r{cosθcos2ϕdθ+sinθsin2ϕdϕ})×(r2)-1)+O(1r3).The nonvanishing components of the vectorξα up to order O(1/r) have the form
(71)ξ0≅12r{2(M-r)ζ0+2Mζ1-2aMsin2θζ3},ξ1≅-1r{Mζ0+(M+r)ζ1+asin2θ(r-M)ζ3},ξ2≅-ζ2r-asinθcosθζ3,ξ3≅1r(asinθζ1+arcosθζ2-r2sinθζ3).
Using coframe (66) as well as the trivial Weitzenböck connection, the nonvanishing components of the translation momentum read
(72)H~0^≅-(M-q2/2r)sinθ4π(dθ∧dϕ)+⋯+O(1r2),H~1^≅(M-q2/2r)sinθ4π(dθ∧dϕ)+⋯+O(1r2),H~2^≅a2sin2θcosθ4π(dθ∧dϕ)+⋯+O(1r2),H~3^=-asin2θ4π(dθ∧dϕ)+⋯+O(1r2).
The direct evaluation of the integral (18) for vector fields ξ with constant components ζ yields the following infinite total conserved charge:
(73)𝒬=∫∂S‍ξαH~α=(M-q22r)ζ0-(2M-r)aζ33.
When we apply (19) to calculate the total conserved quantity of the coframe (66), we get
(74)𝒬~=(M-q22r)ζ0-2aMζ33,
which is also not the standard result. Using the same arguments discussed for the second and third coframes, one can get the correct value of the total conserved charges when (46) is employed.


### 5.3. Fifth Coframe

The covariant form of the fifth KN tetrad field having axial symmetry in spherical coordinates may be written as(75)(hαi)V=(-ℱ𝒜00-(2Mr-q2)asin2θ𝒜ℱ0𝒜ℬsinθcosϕsinθsinϕ𝒜𝒜ℬℱsinθcosθ0𝒜ℬcosθcosϕcosθsinϕ𝒜-𝒜ℬℱsin2θ0-𝒜ℬsinϕcosϕ𝒜0),whereℱ=r2-2Mr+a2cos2θ+q2.Tetrad (75) has the same associated metric of tetrad (20). Using the spherical local coordinates (t,r,θ,ϕ), the fifth rotating frame is described by the following coframe components:
(76)ϑKNVα=(Λαγ)ϑVγ,whereϑVγ=(hγi)Vdxi.
Using (24) and (76), the coframe of the fifth KN read
(77)ϑV0^=-(2Mr-q2)asin2θdϕ+ℱdt𝒜ℱ,ϑV1^=𝒜ℬdr,ϑV2^=𝒜dθ,ϑV3^=sinθ𝒜ℬℱdϕ.
The two frames (25) and (77) are related through the local Lorentz transformation; that is,
(78)ϑKNIα=(Λ4αγ)ϑKNVγ,
where (Λ4αγ) has the form
(79)(Λ4αγ)=(-𝒜ℬ𝒞ℱ00-(2Mr-q2)asinθ𝒞ℱ01000010(2Mr-q2)asinθ𝒞ℱ00𝒜ℬ𝒞ℱ).
Coframe (77) has the following nonvanishing components of Riemannian connection:
(80)Γ~1^0^=ℬ2𝒜2ℱ{asin2θ(2Mr2-2Ma2cos2θ+2rq2)dϕ-{2M(r2-a2cos2θ)-2rq2}dt},Γ~1^2^=-a2sinθcosθdr+rℬdθ𝒜ℬ,Γ~1^3^=-sinθℱ𝒜2×({r𝒜2-M[r2[2r2+a2{1+cos2θ}]-a4sin2θcos2θ]+q2r(r2+a2)}dϕ-a{M(r2-a2cos2θ)-rq2}dt),Γ~2^0^=(2Mr-q2)asinθcosθℱ𝒜2([r2+a2]dϕ+adt),Γ~2^3^=-cosθℬℱ𝒜2×({𝒜2+(2Mr-q2)a2(sin2θ)}dϕ+a(2Mr-q2)cdt),Γ~3^0^=(a{sinθ(Mr2-Ma2cos2θ-rq2)dr-(2Mr-q2)cosθℬdθ})×(ℬ𝒜{𝒜-(2Mr-q2)})-1.
The nonvanishing components of the vector ξα have the form
(81)ξ0=(2Mr-q2)aζ3sin2θ+(r2-2Mr-a2cos2θ-q2)ζ0𝒜ℬ,ξ1=𝒜ℬζ1,ξ2=𝒜ζ2,ξ3=𝒜(r2-2Mr+a2+q2)ℬζ3.If we take coframe (77), as well as the trivial Weitzenböck connection, we finally get the translation momentum, that is, H~α^,
(82)H~0^=sinθ8πr[4Mr-a2(1-3cos2θ)-2q2](dθ∧dϕ)+⋯+O(1r2),H~3^=asin2θ(r2-Mr+q2)4πr2(dθ∧dϕ)+⋯+O(1r3).
The direct evaluation of the integral (18) for vector fields ξ with constant components ζ yields the following infinite total conserved charges:
(83)𝒬=∫∂S‍ξαH~α=(M-q22r)ζ0-(M-r3)aζ3.
When we use (19) to calculate the total conserved charge related to coframe (77), one also did not get the standard value; that is,
(84)𝒬~=(M-q22r)ζ0-aMζ33.
Using the same arguments discussed for the pervious coframes, one can get the correct value of the total conserved charge when (46) is hired.


## 5.1. Third Coframe

The covariant form of the third KN tetrad can be written as(53)(hαi)III=(ℬ𝒜00-asin2θℬ𝒜asinθsinϕ𝒜sinθcosϕ𝒜ℬcosθcosϕ𝒜sinθsinϕ(r2+a2)𝒜-asinθcosϕ𝒜sinθsinϕ𝒜ℬcosθsinϕ𝒜-sinθcosϕ(r2+a2)𝒜0cosθ𝒜ℬ-sinθ𝒜0).Tetrad field (53) has the same associated metric of tetrad field (20). Using the spherical local coordinates (t,r,θ,ϕ), the third rotating frame is described by the coframe components
(54)ϑKNIIIα=(Λαγ)ϑIIIγ,whereϑIIIα=(hαi)IIIdxi.
Using (24) and (53) we get
(55)ϑIII0^=-ℬ𝒜(cdt+asin2θdϕ),ϑIII1^=𝒜ℬdr,ϑIII2^=𝒜dθ,ϑIII3^=sinθ[(r2+a2)dϕ+adt]𝒜.The two frames (25) and (55) are related through local Lorentz transformation; that is,
(56)ϑKNIα=(Λ2αγ)ϑKNIIIγ,
where (Λ2αγ) has the form
(57)(Λ2αγ)=((r2+a2)𝒞00aℬsinθ𝒞01000010aℬsinθ𝒞00(r2+a2)𝒞).
The nonvanishing components of the corresponding Riemannian connection of the coframe (55) read
(58)Γ~1^0^=-(×(𝒜2)-1(asin2θ{r2(r+M)+a2cos2θ(r-M)-rq2}dϕ-{M(r2-a2cos2θ)-rq2}dt)×(𝒜2)-1),Γ~1^2^=-a2sinθcosθdr+rℬdθ𝒜ℬ,Γ~1^3^=-rsinθℬdϕ𝒜,Γ~2^0^=asinθcosθℬdϕ𝒜,Γ~2^3^=-cosθ{𝒞dϕ-(2Mr-q2)acdt}𝒜2,Γ~3^0^=rasinθdr-cosθℬdϕ𝒜ℬ.The nonvanishing components of the vectorξα have the form
(59)ξ0=-ℬ𝒜(ζ0+asin2θζ3),ξ1=𝒜ℬζ1,ξ2=𝒜ζ2,ξ3=sinθ𝒜(aζ0+[r2+a2]ζ3).
If we take coframe (55), as well as the trivial Weitzenböck connection, one can get asymptotically the nonvanishing components of the translation momentum
(60)H~0^≅-sinθ(2Mr-q2)(dθ∧dϕ)4rπ+⋯+O(1r2),H~3^=O(1r2).
The direct evaluation of integral (18) yields the following anomalous conserved charge:
(61)𝒬=∫∂S‍ξαH~α=(M-q22r)ζ0-4aMζ33.It is worth mentioning that when one uses (19) to calculate the conserved quantities related to coframe (55), one can get (-(4M-r)aζ3)/3 in the azimuthal direction, and the conserved quantity along the time coordinate does not change. Therefore, we are going to use (46) to calculate the total conserved quantities related to coframe (55). The appropriate matrix of local Lorentz transformation is given by (48). Using the data calculated for the second coframe, that is, using (50), (51), (58), and (59) in (46), we get the conserved charge related to coframe (55) as given by (52).


## 5.2. Fourth Rotating Frame

The covariant form of the fourth rotating tetrad field having axial symmetry in spherical coordinates can be written as(62)(hαi)4=(A1A2A3A4B1sinθcosϕB2sinθcosϕB3cosθcosϕB4sinϕsinθC1sinθsinϕC2sinθsinϕC3cosθsinϕC4cosϕsinθD1cosθD2cosθD3sinθD4cosθ),whereAi, Bi, Ci, and Di read
(63)A1=1-[Mr-q2/2]𝒜,A2=[Mr-q2/2]ℬ,A3=0,A4=[Mr-q2/2]asin2θ𝒜,B1=[Mr-q2/2]𝒜,B2=1ℬcosϕ(rα-[Mr-q22]cosϕ),B3=αcosϕ,B4=β-(([Mr-q2/2]asin2θcosϕ)/𝒜)sinϕ,C1=[Mr-q2/2]𝒜,C2=1Υsinϕ(rβ-[Mr-q22]sinϕ),C3=βsinϕ,C4=-α+([Mr-q2/2]asin2θsinϕ/𝒜)cosϕ,D1=[Mr-q2/2]𝒜,D2=1+[Mr-q2/2]ℬ,D3=-r,D4=-[Mr-q2/2]asin2θ𝒜,
where α  and  β are defined by
(64)α=rcosϕ+asinϕ,β=rsinϕ-acosϕ.Using the spherical local coordinates(t,r,θ,ϕ) the fourth rotating frame is described by the coframe components
(65)ϑKNIVα=(Λαγ)ϑIVγ,whereϑIVγ=(hγi)IVdxi,
Using (24) and (62), we get
(66)ϑIV0^=A1cdt+A2dr+A3dθ+A4dϕ,ϑIV1^=B1sinθcosϕcdt+B2sinθcosϕdr+B3cosθcosϕdθ+B4sinθsinϕdϕ,ϑIV2^=C1sinθsinϕcdt+C2sinθsinϕdr+C3cosθsinϕdθ+C4sinθcosϕdϕ,ϑIV3^=D1cosθcdt+D2cosθdr+D3sinθdθ+D4cosθdϕ.
The local Lorentz transformation Λαγ is given by the matrix (24). The two frames (25) and (66) are related through local Lorentz transformation; that is,
(67)ϑKNIα=(Λ3αγ)ϑKNIVα,
where (Λ3αγ) has the form(68)(Λ3αγ)=(ℱ1𝒜ℬ2ℱ2𝒞-M1ℱ3𝒜ℬsinθcosθℱ2𝒞-M1ℱ4𝒜ℬℱ2𝒞M1ℱ5𝒜ℬsinθℱ2𝒞-M1𝒜ℬ-sinθcosθℱ62𝒜ℬℱ72𝒜ℬsinθℱ82𝒜ℬ0ℱ9𝒜-sinθcosθℱ10𝒜cosθℱ11𝒜-M1asinθ𝒜𝒞-cosθℱ122𝒜𝒞-sinθℱ132𝒜𝒞ℱ142𝒜𝒞),with(69)M1=[Mr-q22],ℱ1=2r4-2Mr3+2r2a2cos2θ+2r2a2-4Ma2rcos2θ+2Mra2+2a4cos2θ+q2(r2+a2cos2θ),ℱ2=r4-2Mr3+r2a2cos2θ+r2a2-2Ma2rcos2θ+a4cos2θ+q2𝒜,ℱ3=r2(sin2ϕ-1)-a2(sin2ϕ+1)-2racos2ϕ,ℱ4=(r2+a2)(sin2ϕsin2θ+cos2θ)+2arsin2θcos2ϕ,ℱ5=-(r2+a2)cos2ϕ+2arsin2ϕ,ℱ6=2r(r-M)(1-sin2ϕ)+2a2+2arcos2ϕ+q2(1+sin2ϕ),ℱ7=(M2r-2r2-q2)(sin2ϕsin2θ+cos2θ)-2arsin2θcos2ϕ-2a2cos2θ,ℱ8=(2r2-2Mr+q2)cos2ϕ+2racos2ϕ,ℱ9=r(sin2θ+sin2ϕcos2θ)-acos2θcos2ϕ,ℱ10=r(1-sin2ϕ)+acos2ϕ,ℱ11=rcos2ϕ+asin2ϕ,ℱ12=2r3cos2ϕ+asin2ϕ(2r2+[2Mr-q2]sin2θ+2a2cos2θ)-a([2Mr-q2]sin2θ-2arcos2θcos2ϕ),ℱ13=2r3cos2ϕ+asin2ϕ(2r2+[2Mr-q2]sin2θ+a2cos2θ)+a([2Mr-q2]cos2θ+acos2θcos2ϕ),ℱ14=2r3sin2ϕ-acos2ϕ(2r2+[2Mr-q2]sin2θ+a2cos2θ)+2a2rsin2ϕcos2θ.
The nonvanishing components of the Riemannian connection of the coframe (66) up to order O(1/r3) read
(70)Γ~1^0^≅[M-q22r]×((2r2)-1(sin2θsin2θ[(1-sin2ϕ)(dr+cdt)+rcos2ϕdϕ]+r(sin2θ+sin2ϕcos2θ)dθ)×(2r2)-1)+O(1r3),Γ~1^2^≅(((2r-2[M-q22r]sin2ϕ)dθ+[M-q22r]×sin2θcos2ϕdϕ[M-q22r])×(2r)-1)+O(1r3),Γ~1^3^≅-12r2sinθ×(asin2θdr+2[M-q22r]rsin2θcos2ϕdθ+sin2θ(3r2-r[M-q22r]sin2θ[1-sin2ϕ])dϕ)+O(1r3),Γ~2^0^≅-[M-q22r]×(((cos2θ+sin2θsin2ϕ)(dr+cdt)+rsin2θ2×(1-sin2ϕ)dθ+rsin2θcos2ϕdϕrsin2θ2)×(r2)-1)+O(1r3),Γ~2^3^≅-12r2(2asinθdr-2[M-q22r]rcosθcos2ϕdθ+2sinθ(3r2-[M-q22r]r[sin2θ+sin2ϕcos2θ])dϕ)+O(1r3),Γ~3^0^≅-[M-q22r]((r2)-1(sinθcos2ϕ(dr+cdt)-r{cosθcos2ϕdθ+sinθsin2ϕdϕ})×(r2)-1)+O(1r3).The nonvanishing components of the vectorξα up to order O(1/r) have the form
(71)ξ0≅12r{2(M-r)ζ0+2Mζ1-2aMsin2θζ3},ξ1≅-1r{Mζ0+(M+r)ζ1+asin2θ(r-M)ζ3},ξ2≅-ζ2r-asinθcosθζ3,ξ3≅1r(asinθζ1+arcosθζ2-r2sinθζ3).
Using coframe (66) as well as the trivial Weitzenböck connection, the nonvanishing components of the translation momentum read
(72)H~0^≅-(M-q2/2r)sinθ4π(dθ∧dϕ)+⋯+O(1r2),H~1^≅(M-q2/2r)sinθ4π(dθ∧dϕ)+⋯+O(1r2),H~2^≅a2sin2θcosθ4π(dθ∧dϕ)+⋯+O(1r2),H~3^=-asin2θ4π(dθ∧dϕ)+⋯+O(1r2).
The direct evaluation of the integral (18) for vector fields ξ with constant components ζ yields the following infinite total conserved charge:
(73)𝒬=∫∂S‍ξαH~α=(M-q22r)ζ0-(2M-r)aζ33.
When we apply (19) to calculate the total conserved quantity of the coframe (66), we get
(74)𝒬~=(M-q22r)ζ0-2aMζ33,
which is also not the standard result. Using the same arguments discussed for the second and third coframes, one can get the correct value of the total conserved charges when (46) is employed.


## 5.3. Fifth Coframe

The covariant form of the fifth KN tetrad field having axial symmetry in spherical coordinates may be written as(75)(hαi)V=(-ℱ𝒜00-(2Mr-q2)asin2θ𝒜ℱ0𝒜ℬsinθcosϕsinθsinϕ𝒜𝒜ℬℱsinθcosθ0𝒜ℬcosθcosϕcosθsinϕ𝒜-𝒜ℬℱsin2θ0-𝒜ℬsinϕcosϕ𝒜0),whereℱ=r2-2Mr+a2cos2θ+q2.Tetrad (75) has the same associated metric of tetrad (20). Using the spherical local coordinates (t,r,θ,ϕ), the fifth rotating frame is described by the following coframe components:
(76)ϑKNVα=(Λαγ)ϑVγ,whereϑVγ=(hγi)Vdxi.
Using (24) and (76), the coframe of the fifth KN read
(77)ϑV0^=-(2Mr-q2)asin2θdϕ+ℱdt𝒜ℱ,ϑV1^=𝒜ℬdr,ϑV2^=𝒜dθ,ϑV3^=sinθ𝒜ℬℱdϕ.
The two frames (25) and (77) are related through the local Lorentz transformation; that is,
(78)ϑKNIα=(Λ4αγ)ϑKNVγ,
where (Λ4αγ) has the form
(79)(Λ4αγ)=(-𝒜ℬ𝒞ℱ00-(2Mr-q2)asinθ𝒞ℱ01000010(2Mr-q2)asinθ𝒞ℱ00𝒜ℬ𝒞ℱ).
Coframe (77) has the following nonvanishing components of Riemannian connection:
(80)Γ~1^0^=ℬ2𝒜2ℱ{asin2θ(2Mr2-2Ma2cos2θ+2rq2)dϕ-{2M(r2-a2cos2θ)-2rq2}dt},Γ~1^2^=-a2sinθcosθdr+rℬdθ𝒜ℬ,Γ~1^3^=-sinθℱ𝒜2×({r𝒜2-M[r2[2r2+a2{1+cos2θ}]-a4sin2θcos2θ]+q2r(r2+a2)}dϕ-a{M(r2-a2cos2θ)-rq2}dt),Γ~2^0^=(2Mr-q2)asinθcosθℱ𝒜2([r2+a2]dϕ+adt),Γ~2^3^=-cosθℬℱ𝒜2×({𝒜2+(2Mr-q2)a2(sin2θ)}dϕ+a(2Mr-q2)cdt),Γ~3^0^=(a{sinθ(Mr2-Ma2cos2θ-rq2)dr-(2Mr-q2)cosθℬdθ})×(ℬ𝒜{𝒜-(2Mr-q2)})-1.
The nonvanishing components of the vector ξα have the form
(81)ξ0=(2Mr-q2)aζ3sin2θ+(r2-2Mr-a2cos2θ-q2)ζ0𝒜ℬ,ξ1=𝒜ℬζ1,ξ2=𝒜ζ2,ξ3=𝒜(r2-2Mr+a2+q2)ℬζ3.If we take coframe (77), as well as the trivial Weitzenböck connection, we finally get the translation momentum, that is, H~α^,
(82)H~0^=sinθ8πr[4Mr-a2(1-3cos2θ)-2q2](dθ∧dϕ)+⋯+O(1r2),H~3^=asin2θ(r2-Mr+q2)4πr2(dθ∧dϕ)+⋯+O(1r3).
The direct evaluation of the integral (18) for vector fields ξ with constant components ζ yields the following infinite total conserved charges:
(83)𝒬=∫∂S‍ξαH~α=(M-q22r)ζ0-(M-r3)aζ3.
When we use (19) to calculate the total conserved charge related to coframe (77), one also did not get the standard value; that is,
(84)𝒬~=(M-q22r)ζ0-aMζ33.
Using the same arguments discussed for the pervious coframes, one can get the correct value of the total conserved charge when (46) is hired.


## 6. Discussion and Conclusion

Within the framework of MAG, the total Lagrangian is formed from geometrical part plus matter part; that is,ℒtotal=V(gαβ,ϑα,Qαβ,Tα,Rαβ)+Lmatter(gαβ,ϑα,Ψ,DΨ) with Qαβ is the nonmetricity and Ψ is the matter fields. Baekler and Hehl [81] have obtained a stationary axially symmetric exact solution of the vacuum field equation for a specific gravitational Lagrangian. Their black hole solution embodies a Kerr-de Sitter metric and the post-Riemannian structures of torsion and nonmetricity and is characterized by mass, angular momentum, and shear charge which measure the violation of the Lorentz invariance. When the cosmological constant vanishes, that is, λ=0, the solution given by (61) derived in [81] will be identical with the third coframe defined by ϑR3α=(Λ1αγ)(hγi)3dxi.Careful comparison between purely tetrad formulation and PG theory reveals an interesting observation: both approaches are not identical. Namely, in the formulation of pure tetrad, one is working with the coframeϑα as the only field variable. It is determined completely (up to local Lorentz transformation) from the equations of motion. However, the resulting conserved current and charge are not invariant under local Lorentz transformations. Moreover, in general, the total conserved quantities are divergent. Therefore, one must select a tetrad field that meets certain conditions in order to obtain physically acceptable charges. The situation in the PG theory is to some extent complementary. Namely, the total conserved current and charge are explicitly invariant under both diffeomorphisms and local Lorentz transformations. However, for their computation, one needs, beside the tetrad, to know the connection and the Lagrange multiplier that meet their requirements. Each of these variables is not determined through the field equations in a unique local Lorentz covariant way. The lack of uniqueness in the Lagrange multiplier can be avoided through the imposition of generalized symmetry conditions on the field configurations. But in the selection of the flat connection, there still remains a freedom compatible to the freedom in the choice of the coframe in the tetrad formulation.The main results of this study are as follows:(i)
we use five coframes; their associated metrics grant the same spacetime, that is, KN spacetime;(ii)
one of these coframes, first coframe, has its total conserved charge divergent when the conserved charge in the tetrad gravity theory is used ([48, 49] Equation (4·11)). This is because of the fact that this coframe is nonholonomic and its Weitzenböck connection is not vanishing neither when r→∞ nor when the physical quantities are vanishing;(iii)
when a regularized conserved charge is used, within purely tetrad formulation, the divergent quantity related to the first coframe, emerged in the time coordinate direction, is removed, and consistent results of total energy and angular momentum are achieved;(iv)
the total conserved charges of the second coframe lack the standard form. This is because of the arguments mentioned above regarding the first coframe. Even when the regularized expression is used, the conserved charge is not the familiar one. Therefore, another definition for the total conserved charge ([48, 49] Equation (4·25)), “PG version of conserved charge,” is used and the desired outcome is achieved;(v)
the total charges of the third, fourth, and fifth coframes are calculated by using the conserved and regularized conserved charge, and it turns out that they suffer from the same disadvantage of the second coframe. When the Poincaré conserved charge is used, satisfactory outcomes are obtained;(vi)
we may at this point suggest that in the context of tetrad theory of gravitation, there are many definitions of the total conserved of energy and angular momentum. The most suitable one relies on the employment of the coframe;(vii)
Nester et al. [82–84] considered the quasilocal center of mass in tetrad gravity. They used the covariant Hamiltonian formalism, which is given by the quasilocal quantities Hamiltonian term limits, along with the symplectic covariant expressions of the limits of the Hamiltonian. They show that the Hamiltonian boundary term of the tetrad theory plays a significant role in angular momentum and plays a key role in obtaining the correct center-of-mass moment;(viii)
Blagojević [85] has assumed that spacetime behaves asymptotically as Minkowski space M4 and has obtained the corresponding global Poincaré generators. The surface terms related to the improved form of these generators appeared to represent the relevant conserved charges energy, momentum, and angular momentum. Mielke and Wallner [86] discussed the Lagrangian form of the energy-momentum of some exact solutions in the teleparallel limit of the PG theory;(ix)
the results achieved in the present study can be used to justify some proposals employed in the literature for the energy-momentum in TEGR [82–84, 87–89] and to extend the concepts of energy-momentum and angular momentum from TEGR to the general teleparallel theory.



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