# Basic Generic Properties of Regular Rotating Black Holes and Solitons

Authors: Irina Dymnikova; Evgeny Galaktionov
Journal: Advances in Mathematical Physics
 (2017)

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## Abstract

We present a systematic description of the basic generic properties of regular rotating black holes and solitons (compact nonsingular nondissipative objects without horizons related by self-interaction and replacing naked singularities). Rotating objects are described by axially symmetric solutions typically obtained by the Gürses-Gürsey algorithm, which is based on the Trautman-Newman techniques and includes the Newman-Janis complex transformation, from spherically symmetric solutions of the Kerr-Schild class specified byTtt=Trr(pr=-ρ). Regular spherical solutions of this class satisfying the weak energy condition have obligatory de Sitter center. Rotation transforms de Sitter center into the equatorial de Sitter vacuum disk. Regular solutions have the Kerr or Kerr-Newman asymptotics for a distant observer, at most two horizons and two ergospheres, and two different kinds of interiors. For regular rotating solutions originated from spherical solutions satisfying the dominant energy condition, there can exist the interior S-surface of de Sitter vacuum which contains the de Sitter disk as a bridge. In the case when a related spherical solution violates the dominant energy condition, vacuum interior of a rotating object reduces to the de Sitter disk only.


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## Body

## 1. Introduction

Presented in the current literature, regular rotating solutions [1–10] are obtained from regular spherical solutions with using the Newman-Janis complex translation [11]. In [12], it was shown that the Newman-Janis translation works for algebraically special metrics which belong to the Kerr-Schild class [13] and can be presented as gμν=ημν+2f(r)kμkν, where ημν is the Minkowski metric and kμ are principal null congruences. More general approach, with using basic properties of metrics from the Kerr-Schild class, was applied for obtaining the axially symmetric solutions in the noncommutative geometry [14].Spherical metrics of the Kerr-Schild class have the form [13] (1)ds2=grdt2-dr2gr-r2dθ2+sin2θdϕ2,where (2)gr=1-2Mrr;Mr=4π∫0rρxx2dx,and are generated by stress-energy tensors satisfying [15–18] (3)Ttt=Trr.The energy density is ρ=Ttt, the radial pressure pr=-Trr, and the transversal pressure p⊥=-Tθθ=-Tϕϕ. Equation (3) represents the radial part of the r-dependent equation of state, pr=-ρ. The contracted Bianchi identities (Tμ;νν=0) yield the second part of the r-dependent equation of state, p⊥=-ρ-(r/2)ρ′ [15, 19].All regular spherical solutions of this class, satisfying the weak energy condition (nonnegative density as measured by any local observer on a time-like curve), have obligatory de Sitter center,Tμν→ρ0δμν;g(r)→1-r2/r02 as r→0 with r02=3/(8πGρ0) [18, 20].Gürses and Gürsey have found that the algebraically special metrics of the Kerr-Schild class can be presented in the Lorentz covariant coordinate system, developed the general approach based on the complex Trautman-Newman techniques (which include the Newman-Janis translation), and derived the axially symmetric metric in the general, model-independent form. In the Boyer-Lindquist coordinates the metric reads [12] (4)ds2=2f-ΣΣdt2+ΣΔdr2+Σdθ2-4afsin2θΣdtdϕ+r2+a2+2fa2sin2θΣsin2θdϕ2,(5)Δ=r2-2fr+a2;Σ=r2+a2cos2θ.It involves a master function (6)fr=rMrwhich comes from a spherically symmetric solution (2). For f(r)=Mr-q2/2, it describes the Kerr-Newman geometry [21], where M is the mass parameter and q is the electric charge. The case q=0 corresponds to the Kerr geometry [22]. Each of these two geometries can have at most two horizons, the solutions without horizons describe naked singularities.The parameterr in (4) is defined as an affine parameter along a principal null congruence. The surfaces of constant r are the confocal ellipsoids of revolution [23] (7)r4-x2+y2+z2-a2r2-a2z2=0which degenerate, for r=0, to the equatorial disk (8)x2+y2≤a2,z=0,centered on the symmetry axis and bounded by the ring x2+y2=a2,  z=0 (in the Kerr and Kerr-Newman geometries, it comprises their ring singularities).Regular axially symmetric solutions satisfy condition (3) in the corotating reference frame [24, 25] and describe regular rotating objects, asymptotically Kerr or Kerr-Newman for a distant observer with the mass parameter M=M(r→∞). Solutions of this class describe regular rotating black holes and spinning solitons with de Sitter vacuum interiors [25–28]. Rotation transforms de Sitter center of regular spherical solutions into de Sitter vacuum disk (8). All regular solutions presented in the literature belong to this class. Most of them are devoted to study of particular solutions specified by a choice of the mass function M(r) in (2).In this paper, we present a systematic review of the basic generic properties of regular rotating black holes and spinning solitons replacing naked singularities and defined in the spirit of Coleman lumps [29] as nonsingular nondissipative objects without horizons keeping themselves together by their own self-interaction. For convenience and transparency in analysis of various aspects of generic behavior, we use the geometrized units c=G=1. Conversion factors and instructions for transition to different nongeometrized units can be found in [30].The paper is organized as follows. In Section2, we present horizons, ergospheres, and ergoregions. Section 3 is devoted to basic physical properties of regular interiors. Section 4 outlines behavior of electromagnetic fields in the case of electrically charged regular black holes and electromagnetic solitons. In Section 5, we summarize and discuss the results.


## 2. Horizons, Ergospheres, and Ergoregions

The basic features of regular rotating objects are closely related to generic properties of related regular spherical solutions (1)-(2).Horizons are defined byΔ(r)=0. The function Δ(r) can be written as (9)Δr=r2+a2-2fr=a2+r2gr.It follows that Δ=a2 at zero points of the metric function g(r), g(r)=0, and evolves from Δ=a2 as r=0 to Δ→∞ as r→∞.A spherical metric functiong(r) in (2) in the asymptotically flat case can have at most two zero points and one minimum between them [18]. Typical behavior of a spherical metric function g(r) is shown in Figure 1.Figure 1
Typical behavior of spherical metric functiong(r). Here m is the mass parameter M normalized to its certain critical value which specifies the double-horizon state.Derivatives ofΔ are Δ′=2rg(r)+r2g′(r); Δ′′=2g(r)+4rg′(r)+r2g′′(r). At r=0 derivatives take the values Δ′=0; Δ′′=2 and the function Δ has the minimum, Δ=a2. Next it grows and can have maximum at a certain value rm<r1, where r1 is the 1st zero of the function g(r). At the maximum Δ′(rm)=0 and hence g′(rm)=-2g(rm)/rm, second derivative Δ′′(rm)=-6g(rm)+rm2g′′(rm)<0. After passing the maximum, decreasing Δ achieves Δ=a2 at the 1st zero of g(r); then it will achieve this value at the 2nd zero point r2 of g(r). The function g(r)<0 between its zeros and has the minimum. In this region, g′(r) is first negative and then passes zero and becomes positive; hence, g′′≥0 everywhere between zeros of g(r), while g≤0; as a result, Δ′′≥0 everywhere in this region, so that the function Δ(r) can have only minimum and only one. At r>r2 we have g(r)>0 and g′>0 so that Δ cannot vanish. Since the function g(r) has at most two zero points, axially symmetric space-time can have at most two horizons, the event horizon r+ and the internal Cauchy horizon r-<r+ [27, 28].Ergosphere is a surface of a static limitgtt=0 given by (10)gttr,θ=r2+a2cos2θ-2fr=0.Ergoregions are defined by gtt<0 which makes possible extraction of rotational energy (see, e.g., [4] and references therein).Each point of the ergosphere belongs to some of confocal ellipsoids (7) covering the whole space as the coordinate surfaces r = const. The Cartesian coordinates satisfy z=rcos⁡θ;x2+y2=(a2+r2)sin2θ. It follows from (10) that z2=(2r2f(r)-r4)/a2 on the ergosphere.There are four cases for the existence of ergospheres and ergoregions shown in Figure2. The width of the ergosphere at a certain z is x2+y2=(a2+r2)(1-z2/r2). In the equatorial plane x2+y2=a2+r2 and z2=0→2f(r)-r2=0. For any regular density profile, the function f(r) (curves (3), (4) in Figure 2) is everywhere nonnegative and monotonically grows from f(r)=4πρ0r4/3 at r→0 [18]. Ergosphere exists when the curve u=2f(r) intersects or touches the parabola u=r2 (curves (2) in Figure 2). It is evident that in this case the curve u=2f(r) intersects also the (situated above) parabola u=r2+a2cos2θ for a given θ (curves (1)).Figure 2
Four cases for the existence of ergospheres and ergoregions.
(a)
(b)In the black hole case, ergospheres and ergoregions exist for any density profile (the curve (3a) for the case of two horizons and the curve (3b) for the double-horizon case). In the case of a soliton the existence of ergospheres depends on the density profile. Solitons can have two ergospheres and ergoregion between them (the curve (4a)), one ergosphere and ergoregion involving the whole interior (the curve (4b)), or no ergospheres [27, 28].


## 3. Internal Structure of Regular Rotating Objects

### 3.1. Density and Pressures

The anisotropic stress-energy tensor responsible for (4) can be written in the form [12] (11)Tμν=ρ+p⊥uμuν-lμlν+p⊥gμνin the orthonormal tetrad (12)uμ=1±ΔΣr2+a2δ0μ+aδ3μ,lμ=±ΔΣδ1μ,nμ=1Σδ2μ,mμ=-1Σsin⁡θasin2θδ0μ+δ3μ.The sign plus refers to the regions outside the event horizon and inside the Cauchy horizon where the vector uμ is time-like, and the sign minus refers to the regions between the horizons where the vector lμ is time-like. The vectors mμ and nμ are space-like in all regions.The eigenvalues of the stress-energy tensor (11), calculated in the corotating references frame where each of ellipsoidal layers of constant r rotates with the angular velocity ω(r)=uϕ/ut=a/(r2+a2) [24], are defined by (13)Tμνuμuν=ρr,θ;Tμνlμlν=pr=-ρ;Tμνnμnν=Tμνmμmν=p⊥r,θin the regions outside the event horizon and inside the Cauchy horizon where density is defined as the eigenvalue corresponding to the time-like eigenvector uμ.The eigenvalues of the stress-energy tensor are related to the master functionf(r) as [24] (14)κΣ2ρr,θ=2f′r-f;κΣ2p⊥r,θ=2f′r-f-f′′Σ,where κ=8πG. It follows that(15)ρr,θ=r4Σ2ρ~r;pr=-ρ;p⊥r,θ=r4Σ2-2r2Σρ~r-r32Σρ~′r,where ρ~(r) is the related spherical density. In the corotating frame, we thus have (16)p⊥+ρ=2r4Σ2-r2Σρ~r-r32Σρ~′r.


### 3.2. De Sitter Disk

Near the disk (8) the function f(r) in (4) approaches de Sitter asymptotic 2f(r)→r4/r02; r02=3/(8πGρ~0). Taking into account Σ=(r4+a2z2)r-2, we get in the equatorial plane r2/Σ→1 as z→0, and (16) reduces to [25](17)p⊥+ρ=-rρ~′r2.For the regular spherical solutions satisfying the weak energy condition ρ~′≤0, and regularity requires rρ~′(r)→0 as r→0 [18]. Then p⊥=-ρ, and the equation of state on the disk (18)p=-ρrepresents the rotating de Sitter vacuum in the corotating frame [25]. According to (15), the density in the equatorial plane is ρ(r,θ)=ρ~(r). When r→0, ρ~(r)→ρ~0, so that on the equatorial disk ρ(r,θ)=ρ~0(r).


### 3.3. Two Types of Interiors

In [24], it was suggested that rotation should inevitably lead to violation of the weak energy condition in interior regions of regular rotating structures. Violation of the weak energy condition was found for regular rotating solutions obtained with the Newman-Janis algorithm from particular spherical metrics [3, 4] and for a solution found by postulating a metric gμν and calculating Tμν from the Einstein equations [5].In our papers [27, 28] we have studied the weak energy condition for rotating regular structures on general setting and found the existence of two kinds of regular interiors, one preserving and the other violating the weak energy condition.The weak energy condition is valid if and only ifρ≥0 and p⊥+ρ≥0 [31]. The first condition is satisfied according to (15). The general equation (16) for p⊥+ρ can be written as (19)p⊥+ρ=2r2Σ2Σr4ρ~′-ρ~a2cos2θ.It implies a possibility for generic violation of the weak energy condition beyond the de Sitter vacuum surface S(r,z)=0, on which p⊥+ρ=0 and the right-hand side in (19) can change its sign. It can be expressed through the pressure of a related spherical solution, p⊥~=-ρ~-rρ~′/2, which gives (20)p⊥+ρ=rρ~′2Σ2Sr,z;Sr,z=r4-z2Pr;Pr=2a2rρ~′ρ~-p⊥~.As we see, the existence of vacuum surfaces and hence the violation of the weak energy condition beyond them is possible if and only if a related spherical solution satisfies the dominant energy condition [31] (ρ~≥pk~ in (20)). In the case when a related spherical solution violates the dominant energy condition, the weak energy condition is preserved for a rotating solution.Regular Interiors Satisfying the Weak Energy Condition. In this case ρ~<p~⊥, hence P(r)≤0, and the function S(r,z) in (20) vanishes only at approaching the disk r=0. In this case the interior region looks as shown in Figure 3 [28] where we also plotted two horizons defined by the roots of the equation r2+a2-2f(r)=0, the event and the internal horizons r=r+, r=r-, respectively, and the ergosphere satisfying r2+a2cos2θ-2f(r)=0.Figure 3
First type of the de Sitter interior for regular rotating objects.Regular Interiors Violating the Weak Energy Condition. In the case when P(r)≥0, there can in principle exist S-surface at which p⊥+ρ=0 and beyond which the weak energy condition is violated. On the S-surface z2=r4/P(r) and hence r2=|z|P(r). The squared width of the S-surface, WS2=(x2+y2)S=(a2+|z|P(r))(1-|z|/P(r)). The squared width of the ellipsoid r=|z|max=re is We2=(a2+re2)(1-z2/re2). The difference We2-WS2=(a2|z|/P(r)+re2)(1-|z|P(r)/re2). Assume that WS>We for some value of z; it means that there exists a ring specified by |z|<|z|max which belongs to the ellipsoid r=re, where these two surfaces intersect and where thus |z|P(re)/re2=1. As a result, |z|=re2/P(re)=|z|max, so that these two surfaces can only touch each other on the poles and hence never cross. It follows that the S-surface is always entirely confined within the ellipsoid defined by |z|max=re=re2/P(re) and contains the disk r=0 as a bridge.For regular spherical solutionsrρ~′→0, p~⊥→-ρ~ as r→0, and in the most general case P(r)→A2r-(n+1) with the integer n≥0 as r→0. As a result the derivative of WS(z) near z→0 behaves as z-(n+3)/(n+5) and goes to ±∞ as z→0, so that the function WS(z) has the cusp at approaching the disk and at least two symmetric (with respect to the equatorial plane) maxima between z=±|zmax| and z=0. Typical form of the de Sitter S-surface for the second type of interior is shown in Figure 4 [27, 28].Figure 4
Second type of interior for regular rotating black holes and solitons.In the cavities between its upper and down boundaries and the bridgep⊥+ρ<0, the weak energy condition is violated and cavities are filled with a phantom energy which is defined by the condition p+ρ<0 [32]; in the considered case, it is satisfied for p⊥.As we have shown, the form of the de SitterS-surfaces is generic. Here we plotted it for the particular exact solution [27, 28] which originates from the spherically symmetric solution [33] (21)ρ~=B2r2+rv22;rv=π8B2M;fr=rgπarctan⁡rrv-rrvr2+rv2,with a phenomenologically regularized Newtonian [28] or Coulomb [27] density profile, dependent on identification of the parameter B2/rv4=ρ~0 which represents the cut-off on self-interaction energy by the de Sitter vacuum density ρ~0 at r=0. The density ρ~0 is related to the mass M by the formula M=(4π/3)ρ~0r02rg=(4π/3)ρ~0r∗3. The length scale r∗=(r02rg)1/3 which appears here in the natural way is characteristic for a geometry with the de Sitter interior and the Schwarzschild exterior [15, 17, 19].Relation between the width of theS-surface in the equatorial plane WS=a and its height HS=|z|max=arv defines the form of the S-surface by the oblateness parameter η=HS/WS. For η<1 the S-surface is oblate (shown in Figure 4). It can be the case of electrically neutral quickly rotating de Sitter-Kerr black holes and solitons [28]. For η>1 the de Sitter S-surface is prolate; it may be the case of a slowly rotating black hole (more details in [27, 28]).


## 3.1. Density and Pressures

The anisotropic stress-energy tensor responsible for (4) can be written in the form [12] (11)Tμν=ρ+p⊥uμuν-lμlν+p⊥gμνin the orthonormal tetrad (12)uμ=1±ΔΣr2+a2δ0μ+aδ3μ,lμ=±ΔΣδ1μ,nμ=1Σδ2μ,mμ=-1Σsin⁡θasin2θδ0μ+δ3μ.The sign plus refers to the regions outside the event horizon and inside the Cauchy horizon where the vector uμ is time-like, and the sign minus refers to the regions between the horizons where the vector lμ is time-like. The vectors mμ and nμ are space-like in all regions.The eigenvalues of the stress-energy tensor (11), calculated in the corotating references frame where each of ellipsoidal layers of constant r rotates with the angular velocity ω(r)=uϕ/ut=a/(r2+a2) [24], are defined by (13)Tμνuμuν=ρr,θ;Tμνlμlν=pr=-ρ;Tμνnμnν=Tμνmμmν=p⊥r,θin the regions outside the event horizon and inside the Cauchy horizon where density is defined as the eigenvalue corresponding to the time-like eigenvector uμ.The eigenvalues of the stress-energy tensor are related to the master functionf(r) as [24] (14)κΣ2ρr,θ=2f′r-f;κΣ2p⊥r,θ=2f′r-f-f′′Σ,where κ=8πG. It follows that(15)ρr,θ=r4Σ2ρ~r;pr=-ρ;p⊥r,θ=r4Σ2-2r2Σρ~r-r32Σρ~′r,where ρ~(r) is the related spherical density. In the corotating frame, we thus have (16)p⊥+ρ=2r4Σ2-r2Σρ~r-r32Σρ~′r.


## 3.2. De Sitter Disk

Near the disk (8) the function f(r) in (4) approaches de Sitter asymptotic 2f(r)→r4/r02; r02=3/(8πGρ~0). Taking into account Σ=(r4+a2z2)r-2, we get in the equatorial plane r2/Σ→1 as z→0, and (16) reduces to [25](17)p⊥+ρ=-rρ~′r2.For the regular spherical solutions satisfying the weak energy condition ρ~′≤0, and regularity requires rρ~′(r)→0 as r→0 [18]. Then p⊥=-ρ, and the equation of state on the disk (18)p=-ρrepresents the rotating de Sitter vacuum in the corotating frame [25]. According to (15), the density in the equatorial plane is ρ(r,θ)=ρ~(r). When r→0, ρ~(r)→ρ~0, so that on the equatorial disk ρ(r,θ)=ρ~0(r).


## 3.3. Two Types of Interiors

In [24], it was suggested that rotation should inevitably lead to violation of the weak energy condition in interior regions of regular rotating structures. Violation of the weak energy condition was found for regular rotating solutions obtained with the Newman-Janis algorithm from particular spherical metrics [3, 4] and for a solution found by postulating a metric gμν and calculating Tμν from the Einstein equations [5].In our papers [27, 28] we have studied the weak energy condition for rotating regular structures on general setting and found the existence of two kinds of regular interiors, one preserving and the other violating the weak energy condition.The weak energy condition is valid if and only ifρ≥0 and p⊥+ρ≥0 [31]. The first condition is satisfied according to (15). The general equation (16) for p⊥+ρ can be written as (19)p⊥+ρ=2r2Σ2Σr4ρ~′-ρ~a2cos2θ.It implies a possibility for generic violation of the weak energy condition beyond the de Sitter vacuum surface S(r,z)=0, on which p⊥+ρ=0 and the right-hand side in (19) can change its sign. It can be expressed through the pressure of a related spherical solution, p⊥~=-ρ~-rρ~′/2, which gives (20)p⊥+ρ=rρ~′2Σ2Sr,z;Sr,z=r4-z2Pr;Pr=2a2rρ~′ρ~-p⊥~.As we see, the existence of vacuum surfaces and hence the violation of the weak energy condition beyond them is possible if and only if a related spherical solution satisfies the dominant energy condition [31] (ρ~≥pk~ in (20)). In the case when a related spherical solution violates the dominant energy condition, the weak energy condition is preserved for a rotating solution.Regular Interiors Satisfying the Weak Energy Condition. In this case ρ~<p~⊥, hence P(r)≤0, and the function S(r,z) in (20) vanishes only at approaching the disk r=0. In this case the interior region looks as shown in Figure 3 [28] where we also plotted two horizons defined by the roots of the equation r2+a2-2f(r)=0, the event and the internal horizons r=r+, r=r-, respectively, and the ergosphere satisfying r2+a2cos2θ-2f(r)=0.Figure 3
First type of the de Sitter interior for regular rotating objects.Regular Interiors Violating the Weak Energy Condition. In the case when P(r)≥0, there can in principle exist S-surface at which p⊥+ρ=0 and beyond which the weak energy condition is violated. On the S-surface z2=r4/P(r) and hence r2=|z|P(r). The squared width of the S-surface, WS2=(x2+y2)S=(a2+|z|P(r))(1-|z|/P(r)). The squared width of the ellipsoid r=|z|max=re is We2=(a2+re2)(1-z2/re2). The difference We2-WS2=(a2|z|/P(r)+re2)(1-|z|P(r)/re2). Assume that WS>We for some value of z; it means that there exists a ring specified by |z|<|z|max which belongs to the ellipsoid r=re, where these two surfaces intersect and where thus |z|P(re)/re2=1. As a result, |z|=re2/P(re)=|z|max, so that these two surfaces can only touch each other on the poles and hence never cross. It follows that the S-surface is always entirely confined within the ellipsoid defined by |z|max=re=re2/P(re) and contains the disk r=0 as a bridge.For regular spherical solutionsrρ~′→0, p~⊥→-ρ~ as r→0, and in the most general case P(r)→A2r-(n+1) with the integer n≥0 as r→0. As a result the derivative of WS(z) near z→0 behaves as z-(n+3)/(n+5) and goes to ±∞ as z→0, so that the function WS(z) has the cusp at approaching the disk and at least two symmetric (with respect to the equatorial plane) maxima between z=±|zmax| and z=0. Typical form of the de Sitter S-surface for the second type of interior is shown in Figure 4 [27, 28].Figure 4
Second type of interior for regular rotating black holes and solitons.In the cavities between its upper and down boundaries and the bridgep⊥+ρ<0, the weak energy condition is violated and cavities are filled with a phantom energy which is defined by the condition p+ρ<0 [32]; in the considered case, it is satisfied for p⊥.As we have shown, the form of the de SitterS-surfaces is generic. Here we plotted it for the particular exact solution [27, 28] which originates from the spherically symmetric solution [33] (21)ρ~=B2r2+rv22;rv=π8B2M;fr=rgπarctan⁡rrv-rrvr2+rv2,with a phenomenologically regularized Newtonian [28] or Coulomb [27] density profile, dependent on identification of the parameter B2/rv4=ρ~0 which represents the cut-off on self-interaction energy by the de Sitter vacuum density ρ~0 at r=0. The density ρ~0 is related to the mass M by the formula M=(4π/3)ρ~0r02rg=(4π/3)ρ~0r∗3. The length scale r∗=(r02rg)1/3 which appears here in the natural way is characteristic for a geometry with the de Sitter interior and the Schwarzschild exterior [15, 17, 19].Relation between the width of theS-surface in the equatorial plane WS=a and its height HS=|z|max=arv defines the form of the S-surface by the oblateness parameter η=HS/WS. For η<1 the S-surface is oblate (shown in Figure 4). It can be the case of electrically neutral quickly rotating de Sitter-Kerr black holes and solitons [28]. For η>1 the de Sitter S-surface is prolate; it may be the case of a slowly rotating black hole (more details in [27, 28]).


## 4. Electrically Charged Regular Black Holes and Solitons

### 4.1. Basic Equations

Objects related by the electromagnetic and gravitational interaction are governed by nonlinear electrodynamics coupled to gravity.Nonlinear electrodynamics was proposed by Born and Infeld as founded on two basic principles: to consider electromagnetic field and particles within the frame of one physical entity which is electromagnetic field and to avoid letting physical quantities become infinite [34]. In this theory, finite values of the field energy are achieved by imposing an upper limit on the electric field, but geometry remains singular.The program based on two above principles can be realized in nonlinear electrodynamics coupled to gravity (NED-GR) in the frame of the standard minimal coupling of gravitational and electromagnetic field, that is, without introducing some hypothetical nonminimal coupling which could be essential at the Planck energies, since in the modern string/M-theories nonlinear electrodynamics appears as low-energy effective limits [35, 36].Electrically charged regular objects are described by the source-free NED-GR equations. The source of the gravitational fields in the Einstein equations is the stress-energy tensor of a nonlinear electromagnetic field.For any gauge-invariant LagrangianL(F), stress-energy tensor of electromagnetic field reads (22)κTνμ=-2LFFναFμα+12δνμL,where Fμν=∂μAν-∂νAμ and LF=dL/dF. In the spherically symmetric case, it has the algebraic structure (3) and metrics belong to the Kerr-Schild class (2).Nonlinear electrodynamics minimally coupled to gravity is described by the action(23)S=116πG∫d4x-gR-LF;F=FμνFμν,where R is the scalar curvature and g is the determinant of the metric tensor. The Lagrangian L(F) is an arbitrary function of F which should have the Maxwell limit, L→F,LF→1, in the weak field regime. Variation with respect to Aμ and gμν yields the dynamic equations (24)∇μLFFμν=0;∇μ∗Fμν=0,where ∗Fμν=(1/2)ημναβFαβ;  η0123=-1/-g, and the Einstein equations Gμν=-κTμν with the electromagnetic source given by the stress-energy of a nonlinear electromagnetic field (22).


### 4.2. Generic Features of the Lagrange Dynamics

The key point is that regularity requiresF→-0 as r→0, while the Maxwell limit implies F→-0 at infinity. Indeed, in the spherically symmetric case F=-2q2/LF2r4 [37], which results in FLF2→-∞ as r→0. The structure of stress-energy tensor implies p⊥+ρ=FLF, regular solutions have obligatory de Sitter center, where p⊥+ρ=0, and hence FLF=0 [33]. Requirement of regularity demands that LF→∞ and F→-0 when r→0. Nonmonotonic behavior of the invariant F leads inevitably to branching of a Lagrangian L(F) [33, 37].This problem is solved by the correct description of the Lagrange dynamics for regular electrically charged structures by the nonuniform variational problem with proper internal boundary conditions on the surface where the invariantF has the minimum [38]. The nonuniform variational problem is described by the action (25)S=Sint+Sext=116π∫ΩintR-LintF-gd4x+∫ΩextR-LextF-gd4x.Each part of the manifold, Ωint and Ωext, is confined by the space-like hypersurfaces t=tin and t=tfin and by the time-like 3-surface at infinity, where electromagnetic fields vanish in the Maxwell limit. Internal boundary between Ωint and Ωext is defined as a time-like hypersurface Σc at which the field invariant F achieves its extremum.In the case of the minimal coupling variation in the action (25) results in the dynamical equations (24) in both Ωint and Ωext, and in the boundary conditions on the surface Σc [38] (26)∫ΣcLFintFμνint-LFextFμνext-gδAμdσν=0Lint-2LFintFint=Lext-2LFextFext.The particular solution (21) can be obtained with the NED-GR Lagrangians.L
i
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t
(
F
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=
2
(
1
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z
2
(
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z
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1
)
3 with z2=-(21-6β/3β)cos(α/3+π/3)-1+1/3β, Lext(F)=2(1-z1(β))/(z1(β)+1)3 with z1=(21-6β/3β)cos(α/3)-1+1/3β, where the invariant F is normalized on q2/rq4, rq=(π/8)(q2/m); β=-F/2,β∈(0,4/27), and α=arccos((2-18β+27β2)/2(1-6β)3/2) [38].The same behavior of the invariantF is generic for regular axisymmetric solutions, F=-0 on the disk r=0 [27] and in the Maxwell limit at r→∞. As a result, the basic generic feature of the regular electrically charged structures is the existence of a characteristic surface separating regions described by different Lagrangians of the nonuniform variational problem.


### 4.3. Dynamics of Electromagnetic Fields

Nonzero field components compatible with the axial symmetry areF01,F02,F13,F23. In geometry with the metric (4) they are related by (27)F31=asin2θF10;F23=r2+a2F02.Due to (27), (24) form the system of four equations for two independent functions [27] (28)∂∂rr2+a2sin⁡θLFF10+∂∂θsin⁡θLFF20=0,∂∂r1sin⁡θLFF31+∂∂θ1r2+a2sin⁡θLFF32=0,∂F23∂r+∂F31∂θ=0,∂F01∂θ+∂F20∂r=0.Solutions to this system should satisfy the compatibility condition [27] (29)∂∂r1LF∂LF∂θ∂∂θ1LF∂LF∂r+4a2sin2θΣ21LF2r∂LF∂r+cotθ∂LF∂θ2=0as the necessary and sufficient condition of compatibility of (28) and hence the necessary condition for the existence of solutions [27].The field invariantF=FμνFμν in the axially symmetric case reduces to (30)F=2F202a2sin2θ-F102.Equations (28) and compatibility condition (29) are satisfied by the functions [25] (31)Σ2LFF01=-qr2-a2cos2θ;Σ2LFF02=qa2rsin⁡2θ;(32)Σ2LFF31=aqsin2θr2-a2cos2θ;Σ2LFF23=aqrr2+a2sin⁡2θ,in two limiting cases: in the linear regime LF=1, when they coincide with the solutions to the Maxwell-Einstein equations [39, 40], and in the strongly nonlinear regime, when (31)-(32) satisfy system (28) as the asymptotic solutions in the limit LF→∞ [27].In terms of the 3-vectors defined as [25, 41] (33)Ej=Fj0;Dj=LFF0j;Bj=​∗Fj0;Hj=LF∗F0j;j=1,2,3the field equations (24) take the form of the source-free Maxwell equations [42] (34)∇·D=0;∇×H=∂D∂t;∇·B=0;∇×E=-∂B∂t.The electric inductionD and the magnetic induction B are related to the electric and magnetic field intensities by (35)Dj=ϵkjEk;Bj=μkjHk,where ϵjk and μjk are the tensors of the electric and magnetic permeability given by [25] (36)ϵrr=r2+a2ΔLF;ϵθθ=LF;μrr=r2+a2ΔLF;μθθ=1LF.The relation connecting density and pressure with the electromagnetic fields reads [25] (37)κp⊥+ρ=2LFF102+F202a2sin2θ.Applying (31)-(32) in the limit LF→∞, we obtain (38)κp⊥+ρ=2q2LFΣ2.It follows thatLF→∞ at the S-surface, where p⊥+ρ=0. As a result, the magnetic permeability vanishes and electric permeability goes to infinity, so that the S-surface displays the properties of a perfect conductor and ideal diamagnetic. The magnetic induction B also vanishes on the S-surface in accordance with (35), (33) and (31)-(32).Violation of the weak energy condition within the internal cavities of theS-surface leads to LF<0 in (37) and to negative values of the electric and magnetic permeability in (36). This can be avoided for the electrically charged regular structures satisfying the basic requirement of electrodynamics of continued media which is positivity of the electric permeability [42]. The compatibility conditions (29) admit solutions (31)-(32) for electromagnetic fields in two limiting regimes, which allows for extension of the equation state (p⊥+ρ) to interior cavities of S-surface in two possible cases. The first case is similar to the shell-like models ([43] and references therein) with the flat vacuum interior, zero fields, and in consequence zero density and pressures. For the NED-GR regular structures in this case the field invariant F which vanishes on the S-surface by virtue of (31)-(32) vanishes also in its interiors, and magnetic permeability is zero at and within the S-surface, but the electric permeability breaks from infinity on S-surface to zero in its interior.The second case, favored by the underlying idea of nonlinearity regularizing singularity, compatible with the existence of solutions for electromagnetic fields, and suggested by vanishing of magnetic induction on the surroundingS-surface, is the extension of LF→∞ to the whole interior of the S-surface [26, 27] leading to regular models with the de Sitter core, p=-ρ, similar to baglike models ([44] and references therein). The condition p⊥+ρ=0 and field equations are satisfied in the limit LF→∞, so that the de Sitter vacuum core has the properties of a perfect conductor and ideal diamagnetic and zero magnetic induction.


### 4.4. Nondissipative Source of Electromagnetic Fields

On the de Sitter diskr=0 where LF→∞, we obtain from (36) μrr=μθθ=LF-1=μ→0. The magnetic induction B in (35) also vanishes with taking into account (33) and (31) [25, 26]. This suggests that an uncertainty can appear in the expression for a surface current js=(1-μ)/4πμ[nB], where n is the normal to the surface, which could testify for transition to a superconducting state [42]. However, both these quantities, B and μ, depend on LF, and to decide whether some uncertainty appears, we have to calculate the exact value of a current in the region of the maximal density.The surface current on the disk is defined by4πjk=[e(k)αFαβnβ] [45], where e(k)α are the base vectors related to the intrinsic coordinates on the disk t,ϕ, 0≤ξ≤π/2; the vector nα=δα1(1+q2/a2)-1/2cos⁡ξ is the unit normal to the disk, and the symbol [·]denotes a jump across its surface in the direction orthogonal to it. Using on the disk the solutions (31)-(32) and taking into account the fact that μ=1/LF there, we obtain the exact expression for the surface current [26] (39)jϕ=-q2πa1+q2a2sin2ξμcos3ξ.Here a is the radius of the disk; intrinsic coordinate on the disk ξ changes within 0≤ξ≤π/2. The magnetic permeability μ=0 on the disk. Therefore, the current jϕ is zero throughout the disk except the ring ξ=π/2, where both terms in the second fraction go to zero independently. As a result, the surface currents on the ring can be any and amount to a nonzero total value; hence, the general condition for transition to a superconducting state [42] is satisfied.The superconducting current (39) replaces the ring singularity of the Kerr-Newman geometry and represents a nondissipative source of the exterior fields [46], which can in principle provide a practically unlimited life time of an object [26].


### 4.5. Electromagnetic Soliton

The Kerr-Newman geometry inspired a flow of models of the electron since Carter found in 1968 that the parametera couples with the mass M to give the angular momentum J=Ma and independently couples with the charge q to give an asymptotic magnetic dipole moment μ=qa, so that the gyromagnetic ratio q/M is exactly the same as predicted for a spinning particle by the Dirac equation [39]. At the same time Carter discovered the main disaster of the Kerr-Newman geometry which is the total causality violation in the case of a charged particle when there are no Killing horizons, and any point can be connected to any other point by both a future and a past directed time-like curve [39]. Existing models involving screening or covering of causally dangerous regions require introduction of cohesive forces of nonelectromagnetic origin and are typically constructed by matching the exterior Kerr-Newman solution with some hypothetic internal sources ([47, 48] and references therein).Electromagnetic soliton of NED-GR describes in general setting a regular spinning object related by electromagnetic and gravitational radiation and can be applied as the model for the extended electron without additional assumption. According to Carter [39], for the electron q=-e and a=λe/2, where λe=ħ/me is its Compton wavelength [39]. In the observer region r≫λe, the fields are described by the Kerr-Newman limit of solutions (31)-(32) which gives [26] (40)Er=-er21-ħ2me2c23cos2θ4r2;Eθ=eħ2me2c2sin⁡2θ4r3;Br=-eħmeccos⁡θr3;Bθ=-eħ2mecsin⁡θr4.The Planck constant appears due to ability of the Kerr-Newman solution, discovered by Carter, to present the electron as seen by a distant observer. In terms of the Coleman lump, (40) describes the following situation: the leading term in Er gives the Coulomb law as the classical limit ħ=0, and the higher terms represent the quantum corrections.


## 4.1. Basic Equations

Objects related by the electromagnetic and gravitational interaction are governed by nonlinear electrodynamics coupled to gravity.Nonlinear electrodynamics was proposed by Born and Infeld as founded on two basic principles: to consider electromagnetic field and particles within the frame of one physical entity which is electromagnetic field and to avoid letting physical quantities become infinite [34]. In this theory, finite values of the field energy are achieved by imposing an upper limit on the electric field, but geometry remains singular.The program based on two above principles can be realized in nonlinear electrodynamics coupled to gravity (NED-GR) in the frame of the standard minimal coupling of gravitational and electromagnetic field, that is, without introducing some hypothetical nonminimal coupling which could be essential at the Planck energies, since in the modern string/M-theories nonlinear electrodynamics appears as low-energy effective limits [35, 36].Electrically charged regular objects are described by the source-free NED-GR equations. The source of the gravitational fields in the Einstein equations is the stress-energy tensor of a nonlinear electromagnetic field.For any gauge-invariant LagrangianL(F), stress-energy tensor of electromagnetic field reads (22)κTνμ=-2LFFναFμα+12δνμL,where Fμν=∂μAν-∂νAμ and LF=dL/dF. In the spherically symmetric case, it has the algebraic structure (3) and metrics belong to the Kerr-Schild class (2).Nonlinear electrodynamics minimally coupled to gravity is described by the action(23)S=116πG∫d4x-gR-LF;F=FμνFμν,where R is the scalar curvature and g is the determinant of the metric tensor. The Lagrangian L(F) is an arbitrary function of F which should have the Maxwell limit, L→F,LF→1, in the weak field regime. Variation with respect to Aμ and gμν yields the dynamic equations (24)∇μLFFμν=0;∇μ∗Fμν=0,where ∗Fμν=(1/2)ημναβFαβ;  η0123=-1/-g, and the Einstein equations Gμν=-κTμν with the electromagnetic source given by the stress-energy of a nonlinear electromagnetic field (22).


## 4.2. Generic Features of the Lagrange Dynamics

The key point is that regularity requiresF→-0 as r→0, while the Maxwell limit implies F→-0 at infinity. Indeed, in the spherically symmetric case F=-2q2/LF2r4 [37], which results in FLF2→-∞ as r→0. The structure of stress-energy tensor implies p⊥+ρ=FLF, regular solutions have obligatory de Sitter center, where p⊥+ρ=0, and hence FLF=0 [33]. Requirement of regularity demands that LF→∞ and F→-0 when r→0. Nonmonotonic behavior of the invariant F leads inevitably to branching of a Lagrangian L(F) [33, 37].This problem is solved by the correct description of the Lagrange dynamics for regular electrically charged structures by the nonuniform variational problem with proper internal boundary conditions on the surface where the invariantF has the minimum [38]. The nonuniform variational problem is described by the action (25)S=Sint+Sext=116π∫ΩintR-LintF-gd4x+∫ΩextR-LextF-gd4x.Each part of the manifold, Ωint and Ωext, is confined by the space-like hypersurfaces t=tin and t=tfin and by the time-like 3-surface at infinity, where electromagnetic fields vanish in the Maxwell limit. Internal boundary between Ωint and Ωext is defined as a time-like hypersurface Σc at which the field invariant F achieves its extremum.In the case of the minimal coupling variation in the action (25) results in the dynamical equations (24) in both Ωint and Ωext, and in the boundary conditions on the surface Σc [38] (26)∫ΣcLFintFμνint-LFextFμνext-gδAμdσν=0Lint-2LFintFint=Lext-2LFextFext.The particular solution (21) can be obtained with the NED-GR Lagrangians.L
i
n
t
(
F
)
=
2
(
1
-
z
2
(
β
)
)
/
(
z
2
(
β
)
+
1
)
3 with z2=-(21-6β/3β)cos(α/3+π/3)-1+1/3β, Lext(F)=2(1-z1(β))/(z1(β)+1)3 with z1=(21-6β/3β)cos(α/3)-1+1/3β, where the invariant F is normalized on q2/rq4, rq=(π/8)(q2/m); β=-F/2,β∈(0,4/27), and α=arccos((2-18β+27β2)/2(1-6β)3/2) [38].The same behavior of the invariantF is generic for regular axisymmetric solutions, F=-0 on the disk r=0 [27] and in the Maxwell limit at r→∞. As a result, the basic generic feature of the regular electrically charged structures is the existence of a characteristic surface separating regions described by different Lagrangians of the nonuniform variational problem.


## 4.3. Dynamics of Electromagnetic Fields

Nonzero field components compatible with the axial symmetry areF01,F02,F13,F23. In geometry with the metric (4) they are related by (27)F31=asin2θF10;F23=r2+a2F02.Due to (27), (24) form the system of four equations for two independent functions [27] (28)∂∂rr2+a2sin⁡θLFF10+∂∂θsin⁡θLFF20=0,∂∂r1sin⁡θLFF31+∂∂θ1r2+a2sin⁡θLFF32=0,∂F23∂r+∂F31∂θ=0,∂F01∂θ+∂F20∂r=0.Solutions to this system should satisfy the compatibility condition [27] (29)∂∂r1LF∂LF∂θ∂∂θ1LF∂LF∂r+4a2sin2θΣ21LF2r∂LF∂r+cotθ∂LF∂θ2=0as the necessary and sufficient condition of compatibility of (28) and hence the necessary condition for the existence of solutions [27].The field invariantF=FμνFμν in the axially symmetric case reduces to (30)F=2F202a2sin2θ-F102.Equations (28) and compatibility condition (29) are satisfied by the functions [25] (31)Σ2LFF01=-qr2-a2cos2θ;Σ2LFF02=qa2rsin⁡2θ;(32)Σ2LFF31=aqsin2θr2-a2cos2θ;Σ2LFF23=aqrr2+a2sin⁡2θ,in two limiting cases: in the linear regime LF=1, when they coincide with the solutions to the Maxwell-Einstein equations [39, 40], and in the strongly nonlinear regime, when (31)-(32) satisfy system (28) as the asymptotic solutions in the limit LF→∞ [27].In terms of the 3-vectors defined as [25, 41] (33)Ej=Fj0;Dj=LFF0j;Bj=​∗Fj0;Hj=LF∗F0j;j=1,2,3the field equations (24) take the form of the source-free Maxwell equations [42] (34)∇·D=0;∇×H=∂D∂t;∇·B=0;∇×E=-∂B∂t.The electric inductionD and the magnetic induction B are related to the electric and magnetic field intensities by (35)Dj=ϵkjEk;Bj=μkjHk,where ϵjk and μjk are the tensors of the electric and magnetic permeability given by [25] (36)ϵrr=r2+a2ΔLF;ϵθθ=LF;μrr=r2+a2ΔLF;μθθ=1LF.The relation connecting density and pressure with the electromagnetic fields reads [25] (37)κp⊥+ρ=2LFF102+F202a2sin2θ.Applying (31)-(32) in the limit LF→∞, we obtain (38)κp⊥+ρ=2q2LFΣ2.It follows thatLF→∞ at the S-surface, where p⊥+ρ=0. As a result, the magnetic permeability vanishes and electric permeability goes to infinity, so that the S-surface displays the properties of a perfect conductor and ideal diamagnetic. The magnetic induction B also vanishes on the S-surface in accordance with (35), (33) and (31)-(32).Violation of the weak energy condition within the internal cavities of theS-surface leads to LF<0 in (37) and to negative values of the electric and magnetic permeability in (36). This can be avoided for the electrically charged regular structures satisfying the basic requirement of electrodynamics of continued media which is positivity of the electric permeability [42]. The compatibility conditions (29) admit solutions (31)-(32) for electromagnetic fields in two limiting regimes, which allows for extension of the equation state (p⊥+ρ) to interior cavities of S-surface in two possible cases. The first case is similar to the shell-like models ([43] and references therein) with the flat vacuum interior, zero fields, and in consequence zero density and pressures. For the NED-GR regular structures in this case the field invariant F which vanishes on the S-surface by virtue of (31)-(32) vanishes also in its interiors, and magnetic permeability is zero at and within the S-surface, but the electric permeability breaks from infinity on S-surface to zero in its interior.The second case, favored by the underlying idea of nonlinearity regularizing singularity, compatible with the existence of solutions for electromagnetic fields, and suggested by vanishing of magnetic induction on the surroundingS-surface, is the extension of LF→∞ to the whole interior of the S-surface [26, 27] leading to regular models with the de Sitter core, p=-ρ, similar to baglike models ([44] and references therein). The condition p⊥+ρ=0 and field equations are satisfied in the limit LF→∞, so that the de Sitter vacuum core has the properties of a perfect conductor and ideal diamagnetic and zero magnetic induction.


## 4.4. Nondissipative Source of Electromagnetic Fields

On the de Sitter diskr=0 where LF→∞, we obtain from (36) μrr=μθθ=LF-1=μ→0. The magnetic induction B in (35) also vanishes with taking into account (33) and (31) [25, 26]. This suggests that an uncertainty can appear in the expression for a surface current js=(1-μ)/4πμ[nB], where n is the normal to the surface, which could testify for transition to a superconducting state [42]. However, both these quantities, B and μ, depend on LF, and to decide whether some uncertainty appears, we have to calculate the exact value of a current in the region of the maximal density.The surface current on the disk is defined by4πjk=[e(k)αFαβnβ] [45], where e(k)α are the base vectors related to the intrinsic coordinates on the disk t,ϕ, 0≤ξ≤π/2; the vector nα=δα1(1+q2/a2)-1/2cos⁡ξ is the unit normal to the disk, and the symbol [·]denotes a jump across its surface in the direction orthogonal to it. Using on the disk the solutions (31)-(32) and taking into account the fact that μ=1/LF there, we obtain the exact expression for the surface current [26] (39)jϕ=-q2πa1+q2a2sin2ξμcos3ξ.Here a is the radius of the disk; intrinsic coordinate on the disk ξ changes within 0≤ξ≤π/2. The magnetic permeability μ=0 on the disk. Therefore, the current jϕ is zero throughout the disk except the ring ξ=π/2, where both terms in the second fraction go to zero independently. As a result, the surface currents on the ring can be any and amount to a nonzero total value; hence, the general condition for transition to a superconducting state [42] is satisfied.The superconducting current (39) replaces the ring singularity of the Kerr-Newman geometry and represents a nondissipative source of the exterior fields [46], which can in principle provide a practically unlimited life time of an object [26].


## 4.5. Electromagnetic Soliton

The Kerr-Newman geometry inspired a flow of models of the electron since Carter found in 1968 that the parametera couples with the mass M to give the angular momentum J=Ma and independently couples with the charge q to give an asymptotic magnetic dipole moment μ=qa, so that the gyromagnetic ratio q/M is exactly the same as predicted for a spinning particle by the Dirac equation [39]. At the same time Carter discovered the main disaster of the Kerr-Newman geometry which is the total causality violation in the case of a charged particle when there are no Killing horizons, and any point can be connected to any other point by both a future and a past directed time-like curve [39]. Existing models involving screening or covering of causally dangerous regions require introduction of cohesive forces of nonelectromagnetic origin and are typically constructed by matching the exterior Kerr-Newman solution with some hypothetic internal sources ([47, 48] and references therein).Electromagnetic soliton of NED-GR describes in general setting a regular spinning object related by electromagnetic and gravitational radiation and can be applied as the model for the extended electron without additional assumption. According to Carter [39], for the electron q=-e and a=λe/2, where λe=ħ/me is its Compton wavelength [39]. In the observer region r≫λe, the fields are described by the Kerr-Newman limit of solutions (31)-(32) which gives [26] (40)Er=-er21-ħ2me2c23cos2θ4r2;Eθ=eħ2me2c2sin⁡2θ4r3;Br=-eħmeccos⁡θr3;Bθ=-eħ2mecsin⁡θr4.The Planck constant appears due to ability of the Kerr-Newman solution, discovered by Carter, to present the electron as seen by a distant observer. In terms of the Coleman lump, (40) describes the following situation: the leading term in Er gives the Coulomb law as the classical limit ħ=0, and the higher terms represent the quantum corrections.


## 5. Summary and Discussion

All regular rotating objects described by the axially symmetric solutions obtained from spherical solutions with using the Newman-Janis translation are asymptotically described by the Kerr or Kerr-Newman metrics and contain de Sitter vacuum in their deepest interior (the diskr=0).Regular rotating back holes can have at most two horizons. Geometry of the rotating black holes and solitons includes ergoregions where processes of extraction of rotational energy can occur which can explain energetic activity of a wide class of cosmic objects. For black holes, ergospheres and ergoregions exist for any density profile. In the case of a soliton, the existence of ergospheres depends on the density profile. Solitons can have two ergospheres and ergoregion between them, one ergosphere and ergoregion involving the whole interior, or no ergospheres.Regular rotating black holes and solitons have two types of interior. The fist type of interior reduces to the de Sitter vacuum diskr=0. The weak energy condition is satisfied for regular objects with the interiors of the first type. The second type of interiors exists if the related spherical solution satisfies the dominant energy condition. This type of interior is presented by de Sitter vacuum S-surface specified by p=-ρ, which contains de Sitter disk as the bridge. In the internal cavities of the S-surface the weak energy condition is violated.The basic generic property of regular neutral objects described by the de Sitter-Kerr solutions is the existence of a phantom energy in the second type interiors [28].Phantom energy, which inevitably has negative density for a certain class of observers, was introduced [32] in order to model the observed acceleration of our universe. In the most of models phantom energy originates from scalar field(s) with negative kinetic energy [49] and may involve extra dimensions (for a review [50]). For regular rotating black holes and solitons with second type interiors phantom equation of state appears without involvement of additional entities in the internal regions of strong gravitational field.Regular rotating electrically charged black holes and spinning solitons are described by nonlinear electrodynamics coupled to gravity. For a distant observer, electromagnetic and gravitational fields asymptotically coincide with the Kerr-Newman fields. The nondissipative source of electromagnetic fields (which in turn form a source of gravitational fields) is a superconducting current (replacing a ring singularity) predicted in the model-independent way by dynamical equations governing regular objects related by electromagnetic and gravitational interactions.All regular electrically charged rotating objects contain de Sitter vacuum diskr=0 which have the properties of the ideal conductor and ideal diamagnetic. For the objects with the second type of interiors, these properties are characteristic for the whole S-surface. The violation of the weak energy condition in its internal cavities leads to negative values of the electric and magnetic permeability. For objects satisfying the basic requirement of electrodynamics of continued media (positivity of electric permeability), this can be avoided by extension of the equation of state p=-ρ to the whole interior, confined by the S-surface, in agreement with the conditions for the existence and admissible behavior of solutions for electromagnetic fields.Mass of regular objects with the de Sitter interior is related to breaking of space-time symmetry from the de Sitter group [18, 25, 33, 51]. De Sitter vacuum appears in the particle theory as a false vacuum state p=-ρ of the Higgs field responsible for a particle mass. This relation allows us to explain the observable effect of the negative mass-square differences for neutrinos by applying de Sitter group for space-time symmetry in the interaction vertex and calculating particles masses as the eigenvalues of the Casimir operator in de Sitter space [52].Experimental data reveal with a5σ significance the existence of a minimal length scale le=1.57×10-17 cm at the energy E=1.253 TeV in the annihilation reaction e+e-→γγ(γ) [48]. It corresponds to the minimum in the χ2-fit and characterizes the region of the closest approach of annihilating particles specified by the finite length le which cannot be made smaller. Hypotheses of quantum electrodynamics applied in the χ2-test assume a scattering center as a point. If the electron is an extended object, its structure would modify the QED cross-section if the test distances are smaller than its characteristic size. The results indicate decreasing cross-section with respect to that predicted by QED and testify for extended particles rather than point-like. The reaction e+e-→γγ(γ) is purely electromagnetic and can be considered as the process of interaction of extended particles related by electromagnetic and gravitational interactions. The definite feature of the annihilation process is that at its final stage a region of interaction is neutral and spineless. It can be roughly modeled by a spherical lump with de Sitter vacuum interior [16, 18]. For all structures with the de Sitter interior, there exists the characteristic zero gravity surface rs≃(r02rg)1/3 at which the strong energy condition (ρ+∑‍pk≥0 [31]) is violated and beyond which the gravitational acceleration becomes repulsive [18]. The gravitational radius rg related to the energy E=1.253 TeV and de Sitter radius r0 related to the Higgs vacuum expectation value responsible for the electron mass at the scale EEW=246 GeV give r∗≃0.86×10-16 cm. The scale le=1.57×10-17 cm fits inside a region where gravity is repulsive and can be thus understood as a distance at which electromagnetic attraction is balanced by the gravitational repulsion of the interior de Sitter vacuum [48].



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*Source: 1035381-2017-10-16.xml*