# Energy-Momentum for a Charged Nonsingular Black Hole Solution with a Nonlinear Mass Function

Authors: Irina Radinschi; Theophanes Grammenos; Farook Rahaman; Andromahi Spanou; Sayeedul Islam; Surajit Chattopadhyay; Antonio Pasqua
Journal: Advances in High Energy Physics
 (2017)

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## Abstract

The energy-momentum of a new four-dimensional, charged, spherically symmetric, and nonsingular black hole solution constructed in the context of general relativity coupled to a theory of nonlinear electrodynamics is investigated, whereby the nonlinear mass function is inspired by the probability density function of the continuous logistic distribution. The energy and momentum distributions are calculated by use of the Einstein, Landau-Lifshitz, Weinberg, and Møller energy-momentum complexes. In all these prescriptions, it is found that the energy distribution depends on the massM and the charge q of the black hole, an additional parameter β coming from the gravitational background considered, and the radial coordinate r. Further, the Landau-Lifshitz and Weinberg prescriptions yield the same result for the energy, while, in all the aforesaid prescriptions, all the momenta vanish. We also focus on the study of the limiting behavior of the energy for different values of the radial coordinate, the parameter β, and the charge q. Finally, it is pointed out that, for r→∞ and q=0, all the energy-momentum complexes yield the same expression for the energy distribution as in the case of the Schwarzschild black hole solution.


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## Body

## 1. Introduction

The problem of the energy-momentum localization in general relativity has been investigated over the years by using various and different powerful tools such as superenergy tensors [1–4], quasilocal expressions [5–9], and the mostly known pseudotensorial energy-momentum complexes introduced by Einstein [10, 11], Landau and Lifshitz [12], Papapetrou [13], Bergmann and Thomson [14], Møller [15], Weinberg [16], and Qadir and Sharif [17].As it is well-known, the main difficulty which arises consists in developing a properly defined expression for the energy density of the gravitational background. Until today, no generally accepted meaningful definition for the energy of the gravitational field has been established. However, despite this difficulty, many physically reasonable results have been obtained by applying the aforesaid definitions for the energy-momentum localization. At this point, one cannot but notice the existing agreement between the pseudotensorial prescriptions and the quasilocal mass definition elaborated by Penrose [18] and further developed by Tod [19].Although the dependence on the coordinate system continues to be the main “weakness” of these tools, a number of physically interesting results have been obtained for gravitating systems in(3+1), (2+1), and (1+1) space-time dimensions by using the energy-momentum complexes [20–50]. In fact, the Møller energy-momentum complex is the only computational tool independent of coordinates. In the context of other pseudotensorial prescriptions, in order to calculate the energy and momentum distributions, one introduces Schwarzschild Cartesian and Kerr-Schild coordinates.An alternative option for avoiding the problem of the coordinate system dependence is provided by the teleparallel theory of gravity [51, 52], whereby one notices the considerable similarity of results obtained by this approach with results achieved by using the energy-momentum complexes [53–57].Finally, closing this short introduction to the topic of the energy-momentum localization, it is necessary to point out the broadness of the ongoing attempts in order to define properly and, actually, rehabilitate the concept of the energy-momentum complex [58–61].The outline of the present paper is the following. In Section2, we introduce the new static and charged, spherically symmetric, nonsingular black hole solution under study. Section 3 is devoted to the presentations of the Einstein, Landau-Lifshitz, Weinberg, and Møller energy-momentum complexes used for the calculations. In Section 4, the computations of the energy and momentum distributions are presented. In the discussion given in Section 5, we comment on our results and explore some limiting and particular cases. We have used geometrized units (c=G=1), while the signature is (+,-,-,-). The calculations for the Einstein, Landau-Lifshitz, and Weinberg energy-momentum complexes are performed by use of the Schwarzschild Cartesian coordinates. Greek indices range from 0 to 3, while Latin indices run from 1 to 3.


## 2. The New Charged Nonsingular Black Hole Solution with a Nonlinear Mass Function

The determination of nonsingular black hole solutions by coupling gravity to nonlinear electrodynamics has attracted interest long ago (for a review, see, e.g., [62] for spherically symmetric solutions or [63] and references therein for charged axisymmetric solutions). Recently, Balart and Vagenas [64] constructed a number of new charged, nonsingular, and spherically symmetric, four-dimensional black hole solutions with a nonlinear electrodynamics source. Indeed, start with the static and spherically symmetric space-time geometry described by the line element:(1)ds2=-frdt2+1frdr2+r2dθ2+sin2⁡θdϕ2,with the metric function(2)fr=1-2Mrσβrσ∞β,where the distribution function σ(βr) depends on the mass M, the charge q, the radial coordinate r, and the parameter β∈R+, and σ∞=σ(r→∞) is a normalization factor. Thus one has a nonlinear mass function of the following form:(3)mr=Mσβrσ∞β,which, at infinity, becomes M. It is shown in [64] that for specific distribution functions σ(r) the curvature invariants (R, RμνRμν, RκλμνRκλμν) and the associated nonlinear electric field are nonsingular everywhere.Based on these results, we have already studied [65] the problem of the localization of energy for a function σ(r) resembling the form of the Fermi-Dirac distribution. Here, following up that work, we adopt another distribution function given in [64] that is inspired by the form of the probability density function of the continuous logistic distribution [66], such that(4)fr=1-2Mr4exp⁡-2q2/βMr1+exp⁡-2q2/βMr2β,β∈R+with the nonlinear mass function given by (3).The associated nonsingular space-time exhibits two horizons, while the nonlinear and nonsingular electric field that asymptotically goes toq/r2 reads now(5)Er=q8r2sech⁡q22βMr21+β×1+β-βcosh⁡2q2βMr+7βMr2q2sinh⁡2q2βMr.When β→0, the metric function (4) takes the form f(r)=1-2M/r; that is, we get the Schwarzschild black hole geometry.Thus, in what follows, we are going to investigate the problem of energy-momentum localization for a charged and nonsingular black hole solution with the space-time described by (1), (4) and the nonlinear mass function:(6)mr=M4exp⁡-2q2/βMr1+exp⁡-2q2/βMr2β.


## 3. Einstein, Landau-Lifshitz, Weinberg, and Møller Energy-Momentum Complexes

The definition of the Einstein energy-momentum complex [10, 11] for a (3+1)-dimensional gravitating system is given by(7)θνμ=116πhν,λμλ,where the von Freud superpotentials hνμλ are given as(8)hνμλ=1-ggνσ-ggμσgλκ-gλσgμκ,κand satisfy the required antisymmetric property(9)hνμλ=-hνλμ.The components θ00 and θi0 correspond to the energy and the momentum densities, respectively. In the Einstein prescription, the local conservation law holds:(10)θν,μμ=0.Thus, the energy and the momenta can be computed by(11)Pν=∭θν0dx1dx2dx3.Applying Gauss’ theorem, the energy-momentum is(12)Pν=116π∬hν0inidS,where ni represents the outward unit normal vector on the surface dS.The Landau-Lifshitz energy-momentum complex [12] is defined as(13)Lμν=116πS,ρσμνρσ,where the Landau-Lifshitz superpotentials are given by(14)Sμνρσ=-ggμνgρσ-gμρgνσ.The L00 and L0i components represent the energy and the momentum densities, respectively. In the Landau-Lifshitz prescription, the local conservation law reads(15)L,νμν=0.By integrating Lμν over the 3-space, one obtains for the energy-momentum:(16)Pμ=∭Lμ0dx1dx2dx3.By using Gauss’ theorem, we have(17)Pμ=116π∬S,νμ0iνnidS=116π∬Uμ0inidS.The Weinberg energy-momentum complex [16] is given by the following expression:(18)Wμν=116πD,λλμν,where Dλμν are the corresponding superpotentials:(19)Dλμν=∂hκκ∂xλημν-∂hκκ∂xμηλν-∂hκλ∂xκημν+∂hκμ∂xκηλν+∂hλν∂xμ-∂hμν∂xλ,hμν=gμν-ημν.Here the W00 and W0i components correspond to the energy and the momentum densities, respectively. In the Weinberg prescription, the local conservation law reads(20)W,νμν=0.The integration of Wμν over the 3-space yields for the energy-momentum:(21)Pμ=∭Wμ0dx1dx2dx3.Applying Gauss’ theorem and integrating over the surface of a sphere of radius r, one obtains for the energy-momentum distribution the following expression:(22)Pμ=116π∬Di0μnidS.The Møller energy-momentum complex [15] is given by the following expression:(23)Jνμ=18πMν,λμλ,where the Møller superpotentials Mνμλ are(24)Mνμλ=-g∂gνσ∂xκ-∂gνκ∂xσgμκgλσand satisfy the necessary antisymmetric property:(25)Mνμλ=-Mνλμ.Møller’s energy-momentum complex also satisfies the local conservation law(26)∂Jνμ∂xμ=0,with J00 and Ji0 representing the energy and the momentum densities, respectively. In the Møller prescription, the energy-momentum is given by(27)Pν=∭Jν0dx1dx2dx3.With the aid of Gauss’ theorem, one gets(28)Pν=18π∬Mν0inidS.


## 4. Energy and Momentum Distributions for the New Charged Nonsingular Black Hole Solution

In order to calculate the energy and momenta by using the Einstein energy-momentum complex, it is required to transform the metric given by the line element (1) in Schwarzschild Cartesian coordinates. We obtain the line element in the following form:(29)ds2=frdt2-dx2+dy2+dz2-f-1r-1r2xdx+ydy+zdz2.The components of the superpotentialhν0i in Schwarzschild Cartesian coordinates are(30)h101=h102=h103=0,h201=h202=h203=0,h301=h302=h303=0.The remaining, nonvanishing, components of the superpotentials in the Einstein prescription are as follows:(31)h001=2xr22Mr4exp⁡-2q2/βMr1+exp⁡-2q2/βMr2β,h002=2yr22Mr4exp⁡-2q2/βMr1+exp⁡-2q2/βMr2β,h003=2zr22Mr4exp⁡-2q2/βMr1+exp⁡-2q2/βMr2β.From the line element (29), the expression (12), and the superpotentials (31), we obtain for the energy distribution in the Einstein prescription (see Figure 1) the following:(32)EE=M4exp⁡-2q2/βMr1+exp⁡-2q2/βMr2β.By using (12) and (30), we find that all the momenta vanish:(33)Px=Py=Pz=0.Figure 1
Energy distribution obtained in the Einstein prescription for different values ofβ.In order to apply the Landau-Lifshitz energy-momentum complex, we use theUμ0i quantities defined in (17) and we find the following nonvanishing components:(34)U001=2xr22M/r4exp⁡-2q2/βMr/1+exp⁡-2q2/βMr2β1-2M/r4exp⁡-2q2/βMr/1+exp⁡-2q2/βMr2β,U002=2yr22M/r4exp⁡-2q2/βMr/1+exp⁡-2q2/βMr2β1-2M/r4exp⁡-2q2/βMr/1+exp⁡-2q2/βMr2β,U003=2zr22M/r4exp⁡-2q2/βMr/1+exp⁡-2q2/βMr2β1-2M/r4exp⁡-2q2/βMr/1+exp⁡-2q2/βMr2β.Now, replacing (34) in (17), we obtain the energy distribution in the Landau-Lifshitz prescription:(35)ELL=M4exp⁡-2q2/βMr/1+exp⁡-2q2/βMr2β1-2M/r4exp⁡-2q2/βMr/1+exp⁡-2q2/βMr2β,while all the momenta vanish:(36)Px=Py=Pz=0.In the Weinberg prescription, the nonvanishing superpotential components are as follows:(37)D100=2xr22M/r4exp⁡-2q2/βMr/1+exp⁡-2q2/βMr2β1-2M/r4exp⁡-2q2/βMr/1+exp⁡-2q2/βMr2β,D200=2yr22M/r4exp⁡-2q2/βMr/1+exp⁡-2q2/βMr2β1-2M/r4exp⁡-2q2/βMr/1+exp⁡-2q2/βMr2β,D300=2zr22M/r4exp⁡-2q2/βMr/1+exp⁡-2q2/βMr2β1-2M/r4exp⁡-2q2/βMr/1+exp⁡-2q2/βMr2β.Substituting the expressions obtained in (37) into (22), we get for the energy distribution inside a 2-sphere of radius r the following expression:(38)EW=M4exp⁡-2q2/βMr/1+exp⁡-2q2/βMr2β1-2M/r4exp⁡-2q2/βMr/1+exp⁡-2q2/βMr2β.In the Weinberg prescription, all the momenta vanish:(39)Px=Py=Pz=0.One can see from (35) and (38) that the energy in the Landau-Lifshitz prescription is identical with the energy in the Weinberg prescription.Finally, in the Møller prescription, we find only one nonvanishing superpotential:(40)M001=2Msin⁡θ4exp⁡-2q2/βMr1+exp⁡-2q2/βMr2β1-q2Mr32q2/βMr1-exp⁡-2q2/βMr1+exp⁡-2q2/βMr.Using the above expression for the superpotential and with the aid of the metric coefficient (4) and the expression for energy given by (28), we obtain the energy distribution in the Møller prescription (see Figure 2):(41)EM=M4exp⁡-2q2/βMr1+exp⁡-2q2/βMr2β1-q2β2Mr1-exp⁡-2q2/βMr1+exp⁡-2q2/βMr,while all the momenta vanish:(42)Pr=Pθ=Pϕ=0.Figure 2
Energy distribution obtained in the Møller prescription for different values ofβ.


## 5. Discussion

Following up our previous results [65], we have studied the problem of energy-momentum localization for a new charged, nonsingular and spherically symmetric, static black hole solution in (3+1) dimensions with a nonlinear mass function recently constructed by Balart and Vagenas [64]. To this purpose, we have applied the Einstein, Landau-Lifshitz, Weinberg, and Møller pseudotensorial prescriptions. The calculations have shown that, in all the four prescriptions, the momenta vanish, while the energy depends (see Table 1) on the black hole’s mass and charge, the radial coordinate, and a parameter β∈R+ that is a scaling factor of r (in essence a dilation factor, as it is always positive) inspired by the form of the logistic distribution and marks the space-time geometry considered. In fact, for each value of β, one can numerically determine the values of the two existing horizon radii (an inner and an outer) obtained from the metric function. It is pointed out that the Landau-Lifshitz and the Weinberg prescriptions yield the same energy distribution.Table 1
Energy distributions calculated by use of the energy-momentum complexes of Einstein, Landau-Lifshitz, Weinberg, and Møller.
Prescription
Energy
Einstein
E
E
=
M
4
exp
⁡
-
2
q
2
/
β
M
r
1
+
exp
⁡
-
2
q
2
/
β
M
r
2
β
Landau-Lifshitz
E
L
L
=
M
4
exp
⁡
-
2
q
2
/
β
M
r
/
1
+
exp
⁡
-
2
q
2
/
β
M
r
2
β
1
-
2
M
/
r
4
exp
⁡
-
2
q
2
/
β
M
r
/
1
+
exp
⁡
-
2
q
2
/
β
M
r
2
β
Weinberg
E
W
=
M
4
exp
⁡
-
2
q
2
/
β
M
r
/
1
+
exp
⁡
-
2
q
2
/
β
M
r
2
β
1
-
2
M
/
r
4
exp
⁡
-
2
q
2
/
β
M
r
/
1
+
exp
⁡
-
2
q
2
/
β
M
r
2
β
.
Møller
E
M
=
M
4
exp
⁡
-
2
q
2
/
β
M
r
1
+
exp
⁡
-
2
q
2
/
β
M
r
2
β
×
1
-
q
2
β
2
M
r
1
-
exp
⁡
-
2
q
2
/
β
M
r
1
+
exp
⁡
-
2
q
2
/
β
M
rWe have also examined the limiting behavior of the energy in the casesr→∞, q=0, β→0, and β→∞. For β→0, the metric function f(r) becomes 1-2M/r, while, for β→∞, f(r) becomes 1-(2M/r)[exp⁡(-q2/2Mr)]. The corresponding energies are presented in Table 2, where one can see that for q=0 as well as at infinity the Einstein and Møller prescriptions yield the same result which is also obtained for the classical Schwarzschild black hole solution, namely, the ADM mass M. In the case of the Landau-Lifshitz and Weinberg prescriptions, the energy equals the ADM mass M at infinity r→∞, while, in the chargeless case q=0, these two energy-momentum complexes give for energy the expression M/(1-2M/r). These results coincide with those obtained by Virbhadra’s approach in Schwarzschild Cartesian coordinates [67]. As it is pointed out at the end of Section 2, for β→0 we get the classical Schwarzschild black hole metric. Hence, the corresponding energies given in Table 2 for β→0 are those obtained in the four prescriptions for the Schwarzschild black hole. It is noteworthy that for β→∞ a factor of 2 appears in the exponential in all four prescriptions. In fact, the same dependence on this factor of 2 is obtained for the Einstein and Møller energies in [65], where a different metric function f(r) is considered.Table 2
Limiting cases for the energy.
Prescription
Energy forr→∞
Energy forq=0
Energy forβ→0
Energy forβ→∞
Einstein
M
M
M
M
exp
⁡
-
q
2
2
M
r
Landau-Lifshitz
M
M
1
-
2
M
/
r
M
1
-
2
M
/
r
M
exp
⁡
-
q
2
/
2
M
r
1
-
2
M
/
r
exp
⁡
-
q
2
/
2
M
r
Weinberg
M
M
1
-
2
M
/
r
M
1
-
2
M
/
r
M
exp
⁡
-
q
2
/
2
M
r
1
-
2
M
/
r
exp
⁡
-
q
2
/
2
M
r
Møller
M
M
M
M
-
q
2
2
r
exp
⁡
-
q
2
2
M
rOf particular interest is the behavior of the energy near the origin, namely, forr→0. In the case of the Einstein prescription, the energy tends to zero (see Figure 3). However, the energy obtained by the application of the Landau-Lifshitz, the Weinberg and the Møller energy-momentum complexes shows a rather pathological behavior. In the first two cases the energy is jumping between infinitely positive and negative values at some radial distances in the range 0<r<5 for different values of the parameter β, while for significantly larger values of r(r>50) the energy falls off rapidly to a constant value for various values of the parameter β. The energy calculated by the Møller prescription becomes clearly negative in the range 0<r<0.2 for different values of the parameter β, while the position where the energy retains a positive value and then keeps increasing monotonically is shifted nearer to the origin as β becomes smaller (see Figure 4). This strange behavior of the energy distribution may enhance the argumentation (see, e.g., [67]) according to which the Einstein energy-momentum complex is indeed a more reliable tool for the study of the gravitational energy-momentum localization as it yields physically meaningful results. Thus, it may gain a preference among the different pseudotensorial energy-momentum complexes.Figure 3
Energy distribution near zero obtained in the Einstein prescription for different values ofβ.Figure 4
Energy distribution near zero obtained in the Møller prescription for different values ofβ.



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