<?xml version="1.0" encoding="UTF-8"?><!DOCTYPE article  PUBLIC "-//NLM//DTD Journal Publishing DTD v3.0 20080202//EN" "http://dtd.nlm.nih.gov/publishing/3.0/journalpublishing3.dtd"><article xmlns:mml="http://www.w3.org/1998/Math/MathML" xmlns:xlink="http://www.w3.org/1999/xlink" dtd-version="3.0" xml:lang="en" article-type="research article"><front><journal-meta><journal-id journal-id-type="publisher-id">JHEPGC</journal-id><journal-title-group><journal-title>Journal of High Energy Physics, Gravitation and Cosmology</journal-title></journal-title-group><issn pub-type="epub">2380-4327</issn><publisher><publisher-name>Scientific Research Publishing</publisher-name></publisher></journal-meta><article-meta><article-id pub-id-type="doi">10.4236/jhepgc.2022.81011</article-id><article-id pub-id-type="publisher-id">JHEPGC-114441</article-id><article-categories><subj-group subj-group-type="heading"><subject>Articles</subject></subj-group><subj-group subj-group-type="Discipline-v2"><subject>Physics&amp;Mathematics</subject></subj-group></article-categories><title-group><article-title>
 
 
  Soliton-Like Spherical Symmetric Solutions to the Electromagnetic and Scalar Nonlinear Induction Field Equations in the General Relativity Theory
 
</article-title></title-group><contrib-group><contrib contrib-type="author" xlink:type="simple"><name name-style="western"><surname>Arnaud</surname><given-names>E. Yamadjako</given-names></name><xref ref-type="aff" rid="aff1"><sup>1</sup></xref><xref ref-type="corresp" rid="cor1"><sup>*</sup></xref></contrib><contrib contrib-type="author" xlink:type="simple"><name name-style="western"><surname>Alain</surname><given-names>Adomou</given-names></name><xref ref-type="aff" rid="aff2"><sup>2</sup></xref></contrib><contrib contrib-type="author" xlink:type="simple"><name name-style="western"><surname>Yélomè</surname><given-names>J. F. Kpomahou</given-names></name><xref ref-type="aff" rid="aff3"><sup>3</sup></xref></contrib><contrib contrib-type="author" xlink:type="simple"><name name-style="western"><surname>Jonas</surname><given-names>Edou</given-names></name><xref ref-type="aff" rid="aff1"><sup>1</sup></xref></contrib><contrib contrib-type="author" xlink:type="simple"><name name-style="western"><surname>Siaka</surname><given-names>Massou</given-names></name><xref ref-type="aff" rid="aff1"><sup>1</sup></xref></contrib></contrib-group><aff id="aff1"><addr-line>Department of Physics, University of Abomey-Calavi, Abomey-Calavi, Benin</addr-line></aff><aff id="aff3"><addr-line>Department of Industrial and Technical Sciences, ENSET-Lokossa, UNSTIM, Abomey, Benin</addr-line></aff><aff id="aff2"><addr-line>3National Higher Institute of Industrial Technology, National University of Sciences, Technologies, Engineering and Mathematics of Abomey, UNSTIM, Abomey, Benin</addr-line></aff><pub-date pub-type="epub"><day>17</day><month>11</month><year>2021</year></pub-date><volume>08</volume><issue>01</issue><fpage>147</fpage><lpage>163</lpage><history><date date-type="received"><day>11,</day>	<month>November</month>	<year>2021</year></date><date date-type="rev-recd"><day>3,</day>	<month>January</month>	<year>2022</year>	</date><date date-type="accepted"><day>6,</day>	<month>January</month>	<year>2022</year></date></history><permissions><copyright-statement>&#169; Copyright  2014 by authors and Scientific Research Publishing Inc. </copyright-statement><copyright-year>2014</copyright-year><license><license-p>This work is licensed under the Creative Commons Attribution International License (CC BY). http://creativecommons.org/licenses/by/4.0/</license-p></license></permissions><abstract><p>
 
 
  In this paper, we have used the static spherical symmetric metric. The parameter of the nonlinearity fields is included in the arbitrary function characterizing the interaction between the electromagnetic and scalar fields. Taking into account the own gravitational field of elementary particles, we have obtained exact static spherical symmetric solutions to the electromagnetic and scalar field equations of nonlinear induction. Considering all forms of the solution of Liouville equation, we proved that the metric functions are regular with localized energy density. Moreover, the total energy of the nonlinear induction fields is bounded and the total charge of the elementary particles has a finite value (soliton-like). In the flat space-time, soliton-like solutions exist. 
 
</p></abstract><kwd-group><kwd>Interaction</kwd><kwd> Scalar</kwd><kwd> Electromagnetic</kwd><kwd> Gravitational Fields</kwd><kwd> Description</kwd><kwd> Configuration</kwd><kwd> Elementary Particles</kwd></kwd-group></article-meta></front><body><sec id="s1"><title>1. Introduction</title><p>In classical physics, elementary particles are considered as material points. Moreover, in the Standard Model (SM), the Grand Unification Theories (GUT), the Super Symmetry Super Strings (SUSY), the theory of gravitation is absent [<xref ref-type="bibr" rid="scirp.114441-ref1">1</xref>]. From experimental results and in [<xref ref-type="bibr" rid="scirp.114441-ref2">2</xref>], elementary particles are extended objects with a complex spatial configuration. The theories or models (SM, GUT, SUSY) do not therefore solve the problem of the description of the configuration of elementary particles. This description, with all their physical characteristics is only possible in the framework of field interaction theory and in quantum mechanics [<xref ref-type="bibr" rid="scirp.114441-ref3">3</xref>]. In particle physics, soliton-like solutions to nonlinear differential field equations are used as models to describe the complex spatial configuration of elementary particles [<xref ref-type="bibr" rid="scirp.114441-ref4">4</xref>] [<xref ref-type="bibr" rid="scirp.114441-ref5">5</xref>].</p><p>The soliton is a particular solution of nonlinear differential equations, spatially localized and of exceptional stability [<xref ref-type="bibr" rid="scirp.114441-ref6">6</xref>] [<xref ref-type="bibr" rid="scirp.114441-ref7">7</xref>]. The notion of soliton has given the opening to a series of scientific works. For example, the basis of soliton was elaborated in [<xref ref-type="bibr" rid="scirp.114441-ref8">8</xref>] [<xref ref-type="bibr" rid="scirp.114441-ref9">9</xref>]. The resolution of the KdV equation in [<xref ref-type="bibr" rid="scirp.114441-ref10">10</xref>] leads to the theoretical interpretation of J. S. Russell observation [<xref ref-type="bibr" rid="scirp.114441-ref11">11</xref>]. The work of [<xref ref-type="bibr" rid="scirp.114441-ref12">12</xref>] [<xref ref-type="bibr" rid="scirp.114441-ref13">13</xref>] [<xref ref-type="bibr" rid="scirp.114441-ref14">14</xref>] and the Carter-Penrose diagram, are references for studying the singularity of static spherical and symmetric solutions. In [<xref ref-type="bibr" rid="scirp.114441-ref15">15</xref>], the authors generalized the solutions to the Born-Infeld nonlinear electrodynamics equation based on the results of [<xref ref-type="bibr" rid="scirp.114441-ref16">16</xref>]. In [<xref ref-type="bibr" rid="scirp.114441-ref17">17</xref>], the resolution to the equation of scalar, electromagnetic and gravitational fields leads to the obtaining of static spherical symmetry solutions. The authors affirmed the existence of a system of particle-antiparticle pairs. In [<xref ref-type="bibr" rid="scirp.114441-ref18">18</xref>], exact Kink-Like static plane symmetric solutions to the self-consistent system of electromagnetic, scalar and gravitational field equations are obtained. It was shown that under certain choice of the interaction Lagrangian, the solutions are regular and have localized energy (like-soliton). In [<xref ref-type="bibr" rid="scirp.114441-ref19">19</xref>], the authors determined, soliton-like solutions to the nonlinear electromagnetic field equation interacting with the scalar field in the spherical and/or cylindrical symmetric metric in the presence of the own gravitational field of elementary particle by studying only the special case where S ( k , ξ ) = ξ . The authors found that with the calibrated invariance function P ( I ) = P 0 ( λ I − N ) 2 and under the condition λ I &gt; N , the component of metric tensor g 00 is regular and the total energy of the nonlinear induction fields is finite in the configuration where the mass and charge are zero. The solution obtained describes a massive system ( A ( 0 ) = m q ) but the total charge of elementary particles Q has not been examined. In [<xref ref-type="bibr" rid="scirp.114441-ref20">20</xref>] [<xref ref-type="bibr" rid="scirp.114441-ref21">21</xref>] [<xref ref-type="bibr" rid="scirp.114441-ref22">22</xref>] [<xref ref-type="bibr" rid="scirp.114441-ref23">23</xref>] static spherical symmetric soliton-like solutions to the spinoriel and gravitational field equations were established using several bilinear invariants.</p><p>The objective of this research work is to determine the exact static spherical symmetric soliton-like solutions to the electromagnetic and scalar nonlinear induction field equations taking into account the own gravitational field of elementary particles, describing a massless system, considering all forms of the function S ( k , ξ ) , using the calibrated invariance function P ( I ) = P 0 ( N − λ I ) 2 , under the condition λ I &lt; N . To achieve this, Section 2 of this work gives a brief overview of the basic equations. In Section 3, the established solutions are presented. A discussion and a comparative study are made in Section 4. The role of the own gravitational field of elementary particles is studied in Section 5. Section 6 is dedicated to the conclusion and future work.</p></sec><sec id="s2"><title>2. Basic Equations</title><p>In general relativity, Einstein’s equation is:</p><p>G μ ν = − χ T μ ν , (1)</p><p>where ( G μ ν ) is the Einstein tensor, ( χ ) is the Einstein gravitational constant and ( T μ ν ) is the energy-momentum metric tensor. The static spherical symmetric metric is defined by:</p><p>d s 2 = e 2 γ d t 2 − e 2 α d ξ 2 − e 2 β [ d θ 2 + sin 2 ( θ ) d φ 2 ] , (2)</p><p>where the functions α , β and γ depend only on the radial component ξ = 1 r and obey the coordinate relation [<xref ref-type="bibr" rid="scirp.114441-ref24">24</xref>]:</p><p>α = 2 β + γ . (3)</p><p>From (1), (2) and (3), the non-zero components of Einstein’s tensor equation are [<xref ref-type="bibr" rid="scirp.114441-ref24">24</xref>]:</p><p>G 0 0 = e − 2 α ( 2 β ″ − 2 γ ′ β ′ − β ′ 2 ) − e − 2 β = − χ   T 0 0 (4)</p><p>G 1 1 = e − 2 α ( 2 γ ′ β ′ + β ′ 2 ) − e − 2 β = − χ   T 1 1 (5)</p><p>G 2 2 = e − 2 α ( β ″ + γ ″ − 2 γ ′ β ′ − β ′ 2 ) = − χ T 2 2 (6)</p><p>G 2 2 = G 3 3 (7)</p><p>T 2 2 = T 3 3 (8)</p><p>where (‘) denotes the first derivative with respect to ξ .</p><p>The Lagrangian of the electromagnetic and scalar nonlinear fields in interaction, taking into account the own gravitational field of the elementary particles has considered in the form:</p><p>L = R 2   χ − 1 4 F i j F i j + 1 2 φ , i φ , i ψ ( I ) , (9)</p><p>where I = A i   A i is the chronometric invariant; A i ( A ( ξ ) ,0,0,0 ) is the 4-vector potential; ψ ( I ) = 1 + λ ϕ ( I ) is an arbitrary function characterizing the interaction between the electromagnetic and scalar nonlinear fields, λ represents the parameter of the nonlinearity</p><p>In the absence of a current source, the scalar and electromagnetic field equations corresponding to the Lagrangian (9) take the form [<xref ref-type="bibr" rid="scirp.114441-ref19">19</xref>]:</p><p>1 − g ∂ ∂ ξ ν [ − g g ν μ φ , μ ψ ( I ) ] = 0, (10)</p><p>1 − g ∂ ∂ ξ μ [ − g F ν μ ] − φ , i φ , i ψ I ( I ) A ν = 0. (11)</p><p>The energy-momentum metric tensor is defined by:</p><p>T μ ν = φ , μ φ , ν ψ ( I ) − F μ i F ν i + φ , i φ , i ψ I ( I ) A ν A μ     − δ μ ν [ − 1 4 F i j F i j + 1 2 ( φ , i φ , i ) ψ ( I ) ] . (12)</p><p>From (12), its non-zero components are:</p><p>T 0 0 = 1 2 e − 2 α [ e − 2 γ ( A ′ ) 2 + C 2 P ( I ) + 2 e − 2 γ C 2 P I ( I ) ( A ) 2 ] (13)</p><p>T 1 1 = 1 2 e − 2 α [ − C 2 P ( I ) + e − 2 γ ( A ′ ) 2 ] ; (14)</p><p>T 1 1 = − T 2 2 = − T 3 3 . (15)</p><p>The relation (10) has a solution:</p><p>d φ d ξ = C ψ ( I ) = C P ( I ) . (16)</p><p>The electromagnetic field (11) becomes:</p><p>( e − 2 γ A ′ ) ′ − C 2 e − 2 γ P I ( I ) A = 0. (17)</p><p>The sum of (5) and (6), reduce to the Liouville equation [<xref ref-type="bibr" rid="scirp.114441-ref24">24</xref>]:</p><p>( β + γ ) ′ ​ ′ = e 2 ( β + γ ) , (18)</p><p>which is integrated giving:</p><p>e − ( β + γ ) = S ( k , ξ ) = ( sinh k ξ k , k &gt; 0 ξ , k = 0 sin k ξ k , k &lt; 0 (19)</p><p>The sum of (4) and (5), leads to:</p><p>β ″ − e 2 ( β + γ ) = − χ 2 e − 2 γ [ − C 2 P ( I ) + e − 2 γ ( A ′ ) 2 ] . (20)</p><p>From (17), (18) and (20), we draw:</p><p>γ ″ = 1 2 χ ( A A ′ e − 2 γ ) ′ . (21)</p><p>The first integration of (21) gives:</p><p>γ ′ ( ξ ) = 1 2 χ ( A A ′ e − 2 γ ) + Y ,   Y = const . (22)</p><p>For Y = 0 , the solution of (22) is:</p><p>e 2 γ = χ A 2 2 + H ,   H = const . (23)</p><p>The relation (23) introduced in (17) gives:</p><p>&#177; ( ξ + ξ 0 ) = ∫ d A ( χ A 2 2 + H ) C 2 P ( I ) + K ,   ξ 0 = const,   K = const . (24)</p><p>From the regularity conditions established in [<xref ref-type="bibr" rid="scirp.114441-ref19">19</xref>] and [<xref ref-type="bibr" rid="scirp.114441-ref25">25</xref>], we fix H = 1 , K = 0 and assume ξ 0 = 0 . Thus, the relations (23) and (24) become:</p><p>e 2 γ = χ A 2 2 + 1 (25)</p><p>and</p><p>&#177; C ξ = ∫ d A ( χ A 2 2 + 1 ) P ( I ) . (26)</p><p>Using the explicit form of the calibrated invariance function P ( I ) , we will determine respectively the expressions of scalar potential A ( ξ ) and of the component g 00 ( ξ ) of the metric tensor from the relations (26) and (25). Exploiting (19), we will express the other metric functions g 11 ( ξ ) , g 22 ( ξ ) , g 33 ( ξ ) and rewrite the analytical expression of the energy density T 0 0 ( ξ ) . From the previous expressions, we will establish those of the energy density per unit invariant volume T ( ξ ) and the total energy of the nonlinear induction interaction fields E f defined by the relations:</p><p>T ( ξ ) = T 0 0 ( ξ ) − 3 g (27)</p><p>E f = ∫ 0 ξ c     T 0 0 − 3 g d ξ . (28)</p><p>In generally from (11) one gets [<xref ref-type="bibr" rid="scirp.114441-ref18">18</xref>]:</p><p>j ν = − φ , i φ , i ψ I ( I ) A ν . (29)</p><p>It allows to express the non-zero components of the 4-vector current density j ν opposite:</p><p>j 0 = − e − 2 ( γ + α )   C 2 P I ( I ) A , (30)</p><p>j 1 = j 2 = j 3 = 0. (31)</p><p>The charge density ρ e ( ξ ) , the charge density per unit invariant volume ρ ( ξ ) and the total charge of elementary particles Q verify the relations:</p><p>ρ e ( ξ ) = − C 2 e − ( 2 α + γ )   P I ( I ) A , (32)</p><p>ρ ( ξ ) = − C 2 e − 2 γ A P I ( I ) sin θ , (33)</p><p>and</p><p>Q = − C 2 ∫ 0 ξ c     e − 2 γ A d P ( I ) d I   sin θ d ξ . (34)</p><p>In Section 3, we will determine the exact static spherical symmetric solutions to the Einstein equation, the electromagnetic and scalar nonlinear induction field equations using the calibrated invariance function:</p><p>P ( I ) = P 0 ( N − λ I ) 2 , (35)</p><p>where P 0 , N are dimensionless constants satisfying the conditions N &gt; λ I and P ( I ) = 1 in the spatial infinity.</p></sec><sec id="s3"><title>3. Exact Static Spherical Symmetric Solutions of the Einstein Equation, the Electromagnetic and Scalar Nonlinear Induction Field Equations</title><p>Putting (35) into (26), the electric scalar potential is:</p><p>A ( ξ ) = N λ ( 1 − σ 2 ) tanh ( b ξ ) , (36)</p><p>where b = C N P 0 λ ( 1 − σ 2 ) , σ 2 = χ N 2 λ .</p><p>From (3), (19), (25) and (36), we establish the solutions of Einstein’s equation:</p><p>g 00 ( ξ ) = cosh 2 ( b ξ ) − σ 2 ( 1 − σ 2 ) cosh 2 ( b ξ ) , (37)</p><p>g 11 ( ξ ) = − 1 − σ 2 S 4 cosh 2 ( b ξ ) cosh 2 ( b ξ ) − σ 2 , (38)</p><p>g 22 ( ξ ) = g 33 ( ξ ) sin 2 θ = − 1 − σ 2 S 2 cosh 2 ( b ξ ) cosh 2 ( b ξ ) − σ 2 (39)</p><p>where S = S ( k , ξ ) .</p><p>From (13), (19), (27), (28), (36), (37), (38) and (39), the chronometric invariant I ( ξ ) , the energy density T 0 0 ( ξ ) , the energy density per unit invariant volume T ( ξ ) and the total energy of nonlinear induction fields E f verify:</p><p>I ( ξ ) = N sinh 2 ( b ξ ) λ [ cosh 2 ( b ξ ) − σ 2 ] , (40)</p><p>T 0 0 ( ξ ) = S 4 N 2 P 0 C 2 2 cosh 2 ( b ξ ) [ 1 − σ 2 cosh 2 ( b ξ ) − σ 2 + 1 cosh 2 ( b ξ ) − 4 sinh 2 ( b ξ ) cosh 2 ( b ξ ) − σ 2 ] , (41)</p><p>T ( ξ ) = R 1 [ ( 1 − σ 2 ) cosh ( b ξ ) [ cosh 2 ( b ξ ) − σ 2 ] 5 / 2 + cosh − 1 ( b ξ ) [ cosh 2 ( b ξ ) − σ 2 ] 5 / 2   − 4 sinh 2 ( b ξ ) cosh ( b ξ ) [ cosh 2 ( b ξ ) − σ 2 ] 5 / 2 ] , (42)</p><p>E f = R 1 [ ( 1 − σ 2 ) E f 1 + E f 2 − 4 E f 3 ] ,</p><p>where</p><p>R 1 = N 2 P 0 C 2 2 ( 1 − σ 2 ) 3 / 2 sin θ ,</p><p>E f 1 = ∫ 0 ξ c cosh ( b ξ ) [ cosh 2 ( b ξ ) − σ 2 ] 5 / 2 d ξ ,</p><p>E f 2 = ∫ 0 ξ c 1 cosh ( b ξ ) [ cosh 2 ( b ξ ) − σ 2 ] 3 / 2 d ξ ,</p><p>E f 3 = ∫ 0 ξ c sinh 2 ( b ξ ) cosh ( b ξ ) [ cosh 2 ( b ξ ) − σ 2 ] 5 / 2 d ξ</p><p>After a series of mathematical transformations, we obtain E f 1 and E f 2 :</p><p>E f 1 = R 2 sinh ( b ξ c ) [ cosh 2 ( b ξ c ) − σ 2 ] 3 / 2 + 2 R 3 sinh ( b ξ c ) cosh 2 ( b ξ c ) − σ 2 ;</p><p>E f 2 = R 4 [ 2 σ σ 2 − 1 sinh ( b ξ c ) cosh 2 ( b ξ c ) − σ 2 + ln | σ sinh ( b ξ c ) − cosh 2 ( b ξ c ) − σ 2 σ sinh ( b ξ c ) + cosh 2 ( b ξ c ) − σ 2 | ] ,</p><p>where</p><p>R 2 = 1 3 b ( 1 − σ 2 ) ,</p><p>R 3 = 1 3 b ( 1 − σ 2 ) 2 ,</p><p>R 4 = − 1 2 b σ 3 .</p><p>The relation E f 3 being difficult to integrate, we will deduce its location on [ 0, ξ c ] after its extension on [ 0, + ∞ ] . To do this, we will use the formula of the standard table of integrals [<xref ref-type="bibr" rid="scirp.114441-ref26">26</xref>]:</p><p>∫ 0 ∞ sinh μ − 1 x cosh ν − 1 x ( cosh 2 x − β ) ρ d x = 2 B ( μ 2 ,1 + ρ − μ + ν 2 ) &#215; F ( ρ ,1 + ρ − μ + ν 2 ; 1 + ρ − ν 2 , β ) ;</p><p>β ∉ ( 1, ∞ ) , R e ( μ ) &gt; 0 , 2 R e ( 1 + ρ ) &gt; R e ( ν + μ ) . In this expression, B ( a , b ) is the B&#234;ta function and F ( a , b ; c , m ) is the Gauss hyper-geometric function. So, we obtain:</p><p>E f 3 &lt; ∫ 0 ∞ sinh 2 ( b ξ ) cosh ( b ξ ) [ cosh 2 ( b ξ ) − σ 2 ] 5 / 2 d ξ ,</p><p>E f 3 &lt; F ( 5 2 ; 1 ; 5 2 ; σ 2 ) &#215; 2 B ( 3 2 , 1 ) ,</p><p>E f 3 &lt; 4 3 ( 1 − σ 2 ) .</p><p>Thus,</p><p>E f &lt; ∞ . (43)</p><p>Also, the expressions (32), (33) and (34) are transformed into:</p><p>ρ e ( ξ ) = 2 P 0 C 2 S 4 N 3 / 2 λ sinh ( b ξ ) cosh 2 ( b ξ ) cosh 2 ( b ξ ) − σ 2 , (44)</p><p>ρ ( ξ ) = 2 C 2 P 0 λ [ N ( 1 − σ 2 ) ] 3 / 2 cosh ( b ξ ) sinh ( b ξ ) [ cosh 2 ( b ξ ) − σ 2 ] 2 sin θ , (45)</p><p>Q = − C N P 0 1 / 2 ( 1 − σ 2 ) [ 1 cosh 2 ( b ξ c ) − σ 2 − 1 1 − σ 2 ] sin θ . (46)</p><p>In Section 4, we will discuss the influence of the function S ( k , ξ ) on the obtained solutions.</p></sec><sec id="s4"><title>4. Discussion</title><p>The electric scalar potential A ( ξ ) , the component g 00 ( ξ ) of the metric tensor, the energy and the charge densities per unit invariant volume ( T ( ξ ) , ρ ( ξ ) ) are regular functions, independent of the concrete form of the function S ( k , ξ ) . <xref ref-type="fig" rid="fig1">Figure 1</xref> below gives a graphical illustration:</p><p>In <xref ref-type="fig" rid="fig1">Figure 1</xref>(a), the solution of the equation to the electromagnetic and scalar fields of nonlinear induction and taking into account the own gravitational field of elementary particles describes a massless system contrary to the massive system obtained by [<xref ref-type="bibr" rid="scirp.114441-ref19">19</xref>].</p><p>In <xref ref-type="fig" rid="fig1">Figure 1</xref>(c), the energy density per unit invariant volume is an asymptotic and localized function. Its depth and width of localization depend on the value of the integration constants.</p><p>In <xref ref-type="fig" rid="fig1">Figure 1</xref>(d), the charge density per unit invariant volume is also an asymptotic and localized function, with depth and width of localization varying with the values of the constants integration.</p><p>Let us point out from (43) and (46) that, the total charge of elementary particles is a finite quantity and the total energy of fields is limited.</p><p>On the other hand, the components g 11 ( ξ ) , g 22 ( ξ ) , g 33 ( ξ ) of the metric tensor, the energy and charge densities ( T 0 0 ( ξ ) , ρ e ( ξ ) ) depend on the concrete form of the function S ( k , ξ ) .</p><p>In order to respect the regularity conditions [<xref ref-type="bibr" rid="scirp.114441-ref19">19</xref>] and [<xref ref-type="bibr" rid="scirp.114441-ref25">25</xref>], the obvious and trivial form S ( k , ξ ) = ξ is often used. Let us analyze the solutions of the field and Einstein equations of Sect 0, using all concrete forms of the function S ( k , ξ ) because it also respects the boundary conditions.</p><sec id="s4_1"><title>4.1. Case 1: k &gt; 0</title><p>The concrete form of S ( k , ξ ) is:</p><p>S ( k , ξ ) = sinh ( k ξ ) k . (47)</p><p>The relations (47) (38), (39), (41) and (44) lead respectively to:</p><p>g 11 ( ξ ) = − k 4 1 − σ 2 sinh 4 ( k ξ ) cosh 2 ( b ξ ) cosh 2 ( b ξ ) − σ 2 , (48)</p><p>g 22 ( ξ ) = g 33 ( ξ ) sin 2 θ = − k 2 1 − σ 2 sinh 2 ( k ξ ) cosh 2 ( b ξ ) cosh 2 ( b ξ ) − σ 2 , (49)</p><p>T 0 0 ( ξ ) = N 2 P 0 C 2 sinh 4 ( k ξ ) 2 k 4 cosh 2 ( b ξ ) [ 1 − σ 2 cosh 2 ( b ξ ) − σ 2 + 1 cosh 2 ( b ξ )   − 4 sinh 2 ( b ξ ) cosh 2 ( b ξ ) − σ 2 ] , (50)</p><p>ρ e ( ξ ) = 2 P 0 C 2 N 3 / 2 λ sinh 4 ( k ξ ) k 4 cosh 2 ( b ξ ) sinh ( b ξ ) cosh 2 ( b ξ ) − σ 2 . (51)</p></sec><sec id="s4_2"><title>4.2. Case 2: k &lt; 0</title><p>S ( k , ξ ) = sin ( k ξ ) k . (52)</p><p>The relation (52) in those (38), (39), (41) and (44) verify the equalities:</p><p>g 11 ( ξ ) = − k 4 1 − σ 2 sin 4 ( k ξ ) cosh 2 ( b ξ ) cosh 2 ( b ξ ) − σ 2 , (53)</p><p>g 22 ( ξ ) = g 33 ( ξ ) sin 2 θ = − k 2 1 − σ 2 sin 2 ( k ξ ) cosh 2 ( b ξ ) cosh 2 ( b ξ ) − σ 2 , (54)</p><p>T 0 0 ( ξ ) = N 2 P 0 C 2 sin 2 ( k ξ ) 2 k 4 cosh 2 ( b ξ ) [ 1 − σ 2 cosh 2 ( b ξ ) − σ 2 + 1 cosh 2 ( b ξ )   − 4 sinh 2 ( b ξ ) cosh 2 ( b ξ ) − σ 2 ] , (55)</p><p>ρ e ( ξ ) = 2 P 0 C 2 N 3 / 2 λ sin 4 ( k ξ ) k 4 cosh 2 ( b ξ ) sinh ( b ξ ) cosh 2 ( b ξ ) − σ 2 . (56)</p></sec><sec id="s4_3"><title>4.3. Case 3: k = 0</title><p>S ( k , ξ ) = ξ .</p><p>The relations (38), (39), (41), (44) give:</p><p>g 11 ( ξ ) = − 1 − σ 2 ξ 4 cosh 2 ( b ξ ) cosh 2 ( b ξ ) − σ 2 , (57)</p><p>g 22 ( ξ ) = g 33 ( ξ ) sin 2 θ = − 1 − σ 2 ξ 2 cosh 2 ( b ξ ) cosh 2 ( b ξ ) − σ 2 , (58)</p><p>T 0 0 ( ξ ) = N 2 P 0 C 2 ξ 4 2 cosh 2 ( b ξ ) [ 1 − σ 2 cosh 2 ( b ξ ) − σ 2 + 1 cosh 2 ( b ξ ) − 4 sinh 2 ( b ξ ) cosh 2 ( b ξ ) − σ 2 ] , (59)</p><p>ρ e ( ξ ) = 2 P 0 C 2 N 3 / 2 λ ξ 4 cosh 2 ( b ξ ) sinh ( b ξ ) cosh 2 ( b ξ ) − σ 2 . (60)</p><p>Figures 2-4 give a summary illustration of the properties of all solutions obtained in each of the Sections 4.1, 4.2 and 4.3.</p><p>In <xref ref-type="fig" rid="fig2">Figure 2</xref>(a), <xref ref-type="fig" rid="fig2">Figure 2</xref>(b), <xref ref-type="fig" rid="fig3">Figure 3</xref>(a), <xref ref-type="fig" rid="fig3">Figure 3</xref>(b), <xref ref-type="fig" rid="fig4">Figure 4</xref>(a) and <xref ref-type="fig" rid="fig4">Figure 4</xref>(b), all components of the metric tensor g 11 ( ξ ) , g 22 ( ξ ) and g 33 ( ξ ) , exhibit</p><p>a gravitational singularity ( e β = ∞ ) that is uncontrollable by change of variable in infinite space whatever the form of the function S ( k , ξ ) as stated in [<xref ref-type="bibr" rid="scirp.114441-ref27">27</xref>].</p><p>In <xref ref-type="fig" rid="fig2">Figure 2</xref>(c), <xref ref-type="fig" rid="fig3">Figure 3</xref>(c) and <xref ref-type="fig" rid="fig4">Figure 4</xref>(c), the energy densities T 0 0 ( ξ ) are asymptotic, localized functions, all canceling in infinite space. The width of the localization and the depth vary with the values of the integration constants, in particular that of k.</p><p>In <xref ref-type="fig" rid="fig2">Figure 2</xref>(d), <xref ref-type="fig" rid="fig3">Figure 3</xref>(d) and <xref ref-type="fig" rid="fig4">Figure 4</xref>(d), the charge densities ρ e ( ξ ) have the same properties as the energy densities of Figures 2(c)-4(c) but are positive definite.</p><p>We will focus in Section 5 on the role of the own gravitational field of elementary particles on the soliton-like solutions.</p></sec></sec><sec id="s5"><title>5. Solution in Flat Space-Time</title><p>In the absence of the own gravitational field of elementary particles, the metric (2) becomes:</p><p>d s 2 = d t 2 − d ξ 2 − [ d θ 2 + sin 2 ( θ ) d φ 2 ] . (61)</p><p>The electromagnetic field Equation (17) takes the form:</p><p>A ″ − C 2 P I ( I ) A = 0, (62)</p><p>which has the solution:</p><p>&#177; C ξ = ∫ d A P ( I ) . (63)</p><p>Using (35), the relation (63) gives the expression of electric scalar potential:</p><p>A ( ξ ) = N λ tanh ( u ξ ) , (64)</p><p>where u = C N P 0 λ .</p><p>The energy and charge densities per unit invariant volume ( T ( ξ ) , ρ ( ξ ) ) verify the following expressions:</p><p>T 0 0 ( ξ ) = T ( ξ ) sin θ = P 0 N 2 C 2 cosh 4 ( u ξ ) [ 1 − 2 sinh 2 ( u ξ ) ] , (65)</p><p>ρ ( ξ ) = ρ e ( ξ ) − 3 g = 2 C 2 P 0 N 3 / 2 λ sinh ( u ξ ) cosh 3 ( u ξ ) sin θ . (66)</p><p><xref ref-type="fig" rid="fig5">Figure 5</xref> below, shows the role of the own gravitational field of elementary particles on the solutions established in Section 4.</p><p>In <xref ref-type="fig" rid="fig5">Figure 5</xref>(a), we see that in the absence of the own gravitational field of the elementary particles, the electric scalar potential (64) remains a regular but of smaller amplitude than the one obtained in <xref ref-type="fig" rid="fig1">Figure 1</xref>(a).</p><p>In <xref ref-type="fig" rid="fig5">Figure 5</xref>(b), the energy density per unit invariant volume has the same properties as those obtained by taking into account the own gravitational field of the elementary particles but with almost equal depth.</p><p>In <xref ref-type="fig" rid="fig5">Figure 5</xref>(c), the charge density per unit invariant volume has a more extensive depth in the absence of the elementary particle gravitational field, is asymptotic and localized in an interval whose width depends on the integration constants.</p><p>The total energy of fields E f and the total charge Q of elementary particles are given by the expressions:</p><p>E f = C N 3 / 2 P 0 1 / 2 λ 1 / 2 [ tanh ( u ξ c ) − tanh 3 ( u ξ c ) ] sin θ , (67)</p><p>Q = − 2 C N P 0 1 / 2 3 [ 1 cosh 3 ( u ξ c ) − 1 ] sin θ . (68)</p></sec><sec id="s6"><title>6. Conclusion</title><p>It has been proved that with all forms of the function S ( k , ξ ) , the electromagnetic and scalar nonlinear induction field equations, taking into account the own gravitational field of the elementary particles, are solvable. The obtained results show that, the component g 00 ( ξ ) of the metric tensor is a regular function. However, the other metric functions present a gravitational singularity in infinite space. All energy densities are localized and have a localization depth and width whose interval varies according to the values of the integration constants. The total energy of the nonlinear induction fields and the total charge of elementary particles are finite. These solutions are soliton-like and constitute a model able to describe the complex internal configuration of the elementary particles. In the near future, we will discuss the stability as well as the observability of the localized configurations obtained.</p></sec><sec id="s7"><title>Conflicts of Interest</title><p>The authors declare no conflicts of interest regarding the publication of this paper.</p></sec><sec id="s8"><title>Cite this paper</title><p>Yamadjako, A.E., Adomou, A., Kpomahou, Y.J.F., Edou, J. and Massou, S. (2022) Soliton-Like Spherical Symmetric Solutions to the Electromagnetic and Scalar Nonlinear Induction Field Equations in the General Relativity Theory. Journal of High Energy Physics, Gravitation and Cosmology, 8, 147-163. https://doi.org/10.4236/jhepgc.2022.81011</p></sec></body><back><ref-list><title>References</title><ref id="scirp.114441-ref1"><label>1</label><mixed-citation publication-type="other" xlink:type="simple">Bay, A. (n.d.) 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