Einstein-Yang-Mills-Lorentz black holes

Different black hole solutions of the coupled Einstein-Yang-Mills equations have been well known for a long time. They have attracted much attention from mathematicians and physicists since their discovery. In this work, we analyze black holes associated with the gauge Lorentz group. In particular, we study solutions which identify the gauge connection with the spin connection. This ansatz allows one to find exact solutions to the complete system of equations. By using this procedure, we show the equivalence between the Yang-Mills-Lorentz model in curved space-time and a particular set of extended gravitational theories.


I. INTRODUCTION
The dynamical interacting system of equations related to non-abelian gauge theories defined on a curved space-time is known as Einstein-Yang-Mills (EYM) theory. Thus, this theory describes the phenomenology of Yang-Mills fields [1] interacting with the gravitational attraction, such as the electro-weak model or the strong nuclear force associated with quantum chromodynamics. EYM model constitutes a paradigmatic example of the non-linear interactions related to gravitational phenomenology. Indeed, the evolution of a spherical symmetric system obeying these equations can be very rich. Its dynamics is opposite to the one predicted by other models, such as the ones provided by the Einstein-Maxwell (EM) equations, whose static behaviour is enforced by a version of the Birkhoff's theorem.
For instance, in the four-dimensional space-time, the EYM equations associated with the gauge group SU(2), support a discrete family of static self-gravitating solitonic solutions, found by Bartnik and McKinnon [2]. There are also hairy black hole (BH) solutions, as it was shown by Bizon [3,4]). They are known as colored black holes and can be labeled by the number of nodes of the exterior Yang-Mills field configuration. Although the Yang-Mills fields do not vanish completely outside the horizon, these solutions are characterized by the absence of a global charge. This feature is opposite to the one predicted by the standard BH uniqueness theorems related to the EM equations, whose solutions can be classified solely with the values of the mass, (electric and/or magnetic) charge and angular momentum evaluated at infinity. In any case, The EYM model also supports the Reissner-Nordström BH as an embedded abelian solution with global magnetic charge [5]. It is also interesting to mention that there are a larger variety of solutions associated with different generalizations of the EYM equations extended with dilaton fields, higher curvature corrections, Higgs fields or cosmological constants (read [6] and references therein for more details).
In this work, we are interested in finding solutions of the EYM equations associated with the Lorentz group as gauge group. The main motivation for considering such a gauge symmetry is offered by the spin connection dynamics. This connection is introduced for a consistent description of spinor fields defined on curved space-times. Although general coordinate transformations do not have spinor representations [7], they can be described by the representations associated with the Lorentz group. In addition, they can be used to define alternative theories of gravity [8].
We shall impose that the spin connection is dynamical and its evolution is determined by the Yang-Mills action related to the SO(1, n − 1) symmetry, where n is the number of dimensions of the space-time. In order to complete the EYM equations, we shall assume that gravitation is described by the metric of a Lorentzian manifold. We shall find vacuum analytic solutions to the EYM system by choosing a particular ansatz, that will relate the spin connection with the gauge connection.
This work is organized in the following way. First, in Section II, we present basic features of the EYM model. In Section III, we show the general results based on the Lorentz group taking as a starting point the spin connection, which yields exact solutions to the EYM equations in vacuum. The expressions of the field for the Schwarzschild-de Sitter metric in a four-dimensional space-time are shown in Section IV, where we also remark some properties of particular the solutions in higher dimensional space-times. Finally, we classify the Yang-Mills field configurations through Carmeli method in Section V, and we present the conclusions obtained from our analysis in Section VI.

II. EYM EQUATIONS ASSOCIATED WITH THE LORENTZ GROUP
The dynamics of a non-abelian gauge theory defined on a four-dimensional Lorentzian manifold is described by the following EYM action: where Unless otherwise specified, we will use Planck units throughout this work (G = c =h = 1), the signature (+, −, −, −) is used for the metric tensor, and Greek letters denote covariant indices, whereas Latin letters stand for Lorentzian indices. The above action is called pure EYM, since it is related to its simplest form, without any additional field or matter content (see [6] for more complex systems).
The EYM equations can be derived from this action by performing variations with respect to the gauge connection: and the metric tensor: where the energy-momentum tensor associated with the Yang-Mills filed configuration is given by: As we have commented, the first non-abelian solution with matter fields was found numerically by Bartnik and McKinnon for the case of a four-dimensional space-time and a SU(2) gauge group [2]. We are interested in solving the above system of equations when the gauge symmetry is associated with the Lorentz group SO(1, 3). In this case, we can write the gauge connection as where the generators of the gauge group J ab , can be written in terms of the Dirac gamma matrixes: J ab = i[γ a , γ b ]/8. In such a case, it is straightforward to deduce the commutative relations of the Lorentz generators:

III. EYM-LORENTZ AN SAT Z
The above set of equations constitutes a complicated system involving a large number of degrees of freedom, which interact not only under the gravitational attraction but also under the non-abelian gauge interaction. It is not simple to find its solutions. We propose the following ansatz, that identifies the gauge connection with the spin connection: with e a λ the tetrad field [9,10], that is defined through the metric tensor g µν = e a µ e b ν η ab ; and Γ λ ρµ is the affine connection of a semi-Riemannian manifold V 4 .
By using the antisymmetric property of the gauge connection with respect to the Lorentz indeces: (A ab ) µ = − (A ba ) µ , we can write the field strength tensor as Then, by taking into account the orthogonal property of the tetrad field e λ a e a ρ = δ λ ρ , the field strength tensor takes the form [11,12]: where R λ ρµν are the components of the Riemann tensor. Thus, F µν = e a λ e ρ b R λ ρµν J b a represents a gauge curvature and we can express the pure EYM Equations (2) and (3) in terms of geometrical quantities. On the one hand, Eq. (2) can be written as: whereas on the other hand, the standard Einstein equations given by Eq. (3) has the following energy-momentum tensor as source: which replaces Eq. (4).

IV. SOLUTIONS OF THE EYM-LORENTZ AN SAT Z
The EYM-Lorentz ansatz described above reduces the problem to a pure gravitational system and simplifies the search for particular solutions. According to the second Bianchi identity for a semi-Riemannian manifold, the components of the Riemann tensor satisfy: By contracting this expression with the metric tensor: By using the symmetries of the Riemann tensor: with R ν λ the components of the Ricci tensor. Then, taking into account (9), we finally obtain: The integrability condition R σ [µν|λ| R ρ]σ = 0 for this expression is known to have as only solutions [13]: where b is a constant.
First, we shall analyze the case of a space-time characterized by four dimensions. In such a case, T µν is trace-free and the solutions are scalar-flat. From the expression of the stress-energy tensor in terms of the Weyl and Ricci tensors, Einstein equations are: where Therefore, by using (15) and the condition C λ µλν = 0, the only solutions are vacuum solutions defined by R µν = 0 [14]. Hence, for empty space, T µν = 0 and all the equations are satisfied for well known solutions [15] such as the Schwarzschild or Kerr metric. Note that these solutions are generally supported for a large variety of different field models and gravitational theories [16]. We can also add a cosmological constant in the Lagrangian and generalize the standard solutions to de Sitter or anti-de Sitter asymptotic space-times, depending on the sign of such a constant.
Once the metric solution is fixed by the particular boundary conditions, the EYM-Lorentz ansatz defined by Eq. (6) determines the solution of the Yang-Mills field configuration. In order to characterize such a configuration, it is interesting to establish the form of the electric E µ = F µν u ν , and magnetic field B µ = * F µν u ν , as measured by an observer moving with four-velocity u ν . In particular, for the Schwarzschild-de Sitter solution, we find the following electric and magnetic projections of the Yang-Mills field strength tensor in the rest frame of reference: It is straightforward to check that the above solution verifies: and tr( E · B) = 0 .
It is also interesting to remark that the family of solutions provided by the EYM-Lorentz ansatz is not restricted to the signature (+, −, −, −). It is also valid for the the Euclidean case (+, +, +, +). For this latter signature, the corresponding gauge group is SO (4) and the associated generators satisfy the following commutation relations: The above solutions can also be generalized to a space-time with an arbitrarily higher number of dimensions. For the n-dimensional case, the assumption of the ansatz (6) in the EYM Equations (2) and (3) is equivalent to work with the following gravitational action in the Palatini formalism: whereñ = n andñ = n − 1 for even and odd n.
In such a case, the Yang-Mills stress-energy tensor takes the form of the one associated with a cosmological constant, in a similar way to certain solutions of modified gravity theories, as the Boulware-Deser solution in Gauss-Bonnet gravity [17]. For instance, for a de Sitter geometry, the Riemann curvature tensor is given by In this case, the energy-momentum tensor associated with the Yang-Mills configuration given by Eq. (10) takes the form Therefore, T µν = 0 is a particular result associated with the four-dimensional space-time.
On the other hand, the equivalence between the Yang-Mills-Lorentz model in curved space-time and a pure gravitational theory is not restricted to Einstein gravity. For example, in the five-dimensional case, we can study the gravitational model defined by the following action in the Palatini formalism: The above expression includes not only the cosmological constant (proportional to α 0 ) and the Einstein-Hilbert term (proportional to α 1 ), but also quadratic contributions of the curvature tensor (proportional to α 2 , α 3 and α 4 ). In this case, the addition of the Yang-Mills action under the restriction of the Lorentz ansatz (6) is equivalent to work with the same gravitational model given by Eq. (29) with the following redefinition of α 4 : It is particularly interesting to consider the model with . In such a case, the higher order contribution in the equivalent gravitational system is proportional to the Gauss-Bonnet term. As it is well known, this latter term reduces to a topological surface contribution for n = 4, but it is dynamical for n ≥ 5. In particular, according to the Boulware-Deser solution, the metric associated with the corresponding equations takes the simple form: where dΩ 2 3 is the metric of a unitary three-sphere, and A 2 (r) is given by: with α 0 /α 1 = −2Λ, α 2 /α 1 = Υ, and σ = 1 or σ = −1. Therefore, from the EYM point of view, the Yang-Mills field contribution modifies the metric solution in a very non-trivial way. We can study the limit Υ → 0 in the Boulware-Deser metric. It is interesting to note that it does not necessarily mean a weak coupling regime of the EYM interaction, since α Y M 4 → 0 does not implies α → 0. It is convenient to distinguish between the branch σ = −1 and σ = 1. The first choice recovers the Schwarzschild-de Sitter solution for Υ = 0: When this metric is deduced from the equations corresponding to a pure gravitational theory, the new contributions from finite values of Υ are usually interpreted as short distance corrections of high-curvature terms in the Einstein-Hilbert action. From the EYM model point of view, these corrections are originated by the Yang-Mills contribution interacting with the gravitational attraction.
On the other hand, the metric solution takes the following form in the EYM weak coupling limit for the value σ = 1: The corresponding geometry does not recover the Schwarzschild-de Sitter limit when Υ → 0, and it presents ghost instabilities.

V. CARMELI CLASSIFICATION OF THE YANG-MILLS FIELD CONFIGURA-TIONS
In the same way that the Petrov classification of the gravitational field describes the possible algebraic symmetries of the Weyl tensor through the problem of finding their eigenvalues and eigenbivectors [18], the Carmeli classification analyze the symmetries of Yang-Mills fields configurations [19].
Let ξ ABCD be the gauge invariant spinor defined by ξ ABCD = 1 4 ǫĖḞ ǫĠḢtr(f AĖBḞ f CĠDḢ ), with f AḂCḊ = τ µ AḂ τ ν CḊ F µν the spinor equivalent to the Yang-Mills strength field tensor written in terms of the generalizations of the unit and Pauli matrices, which establish the correspondence between spinors and tensors. Let φ AB be a symmetrical spinor. Then, by studying the eigenspinor equation ξ CD AB φ CD = λ φ AB , we can classify Yang-Mills field configurations in a systematic way.
This analysis can be applied to any of the EYM-Lorentz solutions but, for simplicity, we will illustrate the computation for the EYM solution related to the Schwarzschild metric in four dimensions. We find the following invariants of the Yang-Mills field: where η ABCD is the totally symmetric spinor ξ (ABCD) , and ξ ABCD satisfies the equalities ξ ABCD = ξ BACD = ξ ABDC = ξ CDAB . Then, the characteristic polynomial p(λ ′ ) = λ ′3 − Gλ ′ /2−H/3 associated with eigenspinor equation of η ABCD provides directly the eigenvalues of the corresponding ξ ABCD . By taking λ = λ ′ + P/3, we obtain the following results: Thus, there are two different eigenvalues: the first one is simple, whereas the the second one is double. There are three distinct eigenspinors and the corresponding Yang-Mills field is of type D P , which is associated with the Yang-Mills configurations of isolated massive objects.

VI. CONCLUSIONS
In this work, we have studied the EYM theory associated with a SO(1, n − 1) guage symmetry, where n is the number of dimensions associated with the space-time. In particular, we have derived analytical expressions for a large variety of black hole solutions. For this analysis, we have used an ansatz that identifies the gauge connection with the spin connection. We have shown that this ansatz allows to interpret different known metric solutions corresponding to pure gravitational systems, in terms of equivalent EYM models. We have demonstrated that this analytical method can also be applied successfully to the study of fundamental black hole configurations.
For the analysis of the corresponding Yang-Mills model with Lorentz gauge symmetry in curved space-time, we have used the appropriate procedure in order to solve the equivalent gravitational equations, which governs the dynamics of pure gravitational systems associated with the proper gravitational theory. In particular, we have derived the solutions for the Schwarzschild-de Sitter geometry in a four-dimensional space-time and for the Boulware-Deser metric in the five-dimensional case. For these solutions, we have specified the corresponding pure gravitational theories. The algebraic symmetries associated with the Yang-Mills configuration related to a given solution can be classified by following the Carmeli method. We have explicitly shown the equivalence with the Petrov classification for the Schwarzschild metric in four-dimensions.
In addition, numerical results obtained for these gravitational systems can be extrapolated to the EYM-Lorentz model by following our prescription. Through the gravitational analogy, one can also deduce the stability properties of the EYM solutions or the gravitational collapse associated with such a system. Here, we have limited the EYM-Lorentz ansatz to the analysis of spherical and static black hole configurations, but it can be used to study other types of solutions. For example, by using the same ansatz, gravitational plane waves in modified theories of gravity may be interpreted as EYM-Lorentz waves. We consider that all these ideas deserve further investigation in future works.