# Torsion Wave Solutions in Yang-Mielke Theory of Gravity

Authors: Vedad Pasic; Elvis Barakovic
Journal: Advances in High Energy Physics
 (2015)

---

## Abstract

The approach of metric-affine gravity initially distinguishes it from Einstein’s general relativity. Using an
independent affine connection produces a theory with 10 + 64 unknowns. We write down the Yang-Mills action
for the affine connection and produce the Yang-Mills equation and the so-called complementary Yang-Mills
equation by independently varying with respect to the connection and the metric, respectively. We call this
theory the Yang-Mielke theory of gravity. We construct explicit spacetimes with pp-metric and purely axial
torsion and show that they represent a solution of Yang-Mills theory. Finally we compare these spacetimes to
existing solutions of metric-affine gravity and present future research possibilities.


---

## Body

## 1. Introduction

Einstein’s geometric theory of gravity can be summarised, paraphrasing Wheeler [1], as follows: spacetime tells matter how to move; matter tells spacetime how to curve. In order to understand this, we have to understand the following:(i)
The motion of particles which are so small that their effect on the gravitational field they move in is negligible.(ii)
The nature of matter as a source for gravity.(iii)
Einstein’s equation, which shows how this matter source is related to the curvature of spacetime.Einstein’s equation is at the centre of general relativity. It gives us a formulation of the relationship between spacetime geometry and the properties of matter. This equation is formulated usingRiemannian geometry, in which the geometric properties of spacetime are described by the metric. The vacuum Einstein’s equation Ricαβ-(1/2)Rgαβ=0 is obtained by varying the Einstein-Hilbert action (1)c416πG∫R,with respect to the metric g. Here R is the scalar curvature (A.9), Ric is the Ricci curvature (A.8), g is the metric, c is the speed of light, and G is the gravitational constant, the recommended numerical value of which is 6.67384(80)×10-11m3kg-1s-2, with relative standard uncertainty 1.2×10-4 (see [2]). The full field equation is then obtained by adding the matter Lagrangian to the Einstein-Hilbert action, which gives us Einstein’s equation in tensor form (2)Ricμν-12Rgμν=8πGc4Tμν,where T is the stress energy tensor that arises from the matter Lagrangian (see, e.g., [3]). The simplest solution of this equation is the Minkowski spacetime from special relativity.Two problems with general relativity arose quite quickly after its initial introduction in 1915. Einstein considered that what are recognised locally as inertial properties of matter must be determined by the properties of the rest of the universe. Einstein’s efforts to discover to what extent general relativity manages to do this founded the modern study of cosmology. The second problem of general relativity was that electromagnetism is not included in the theory. As Einstein said in [4], “A theory in which the gravitational field and the electromagnetic field do not enter as logically distinct structures would be much preferable.” He expected much more from general relativity than the merging of gravitation and electromagnetism at the macroscopic level and he thought that the theory should explain the existence of elementary particles and should provide a treatment for nuclear forces (see [4]). Einstein spent most of the second part of his life trying to achieve this, unfortunately with no real success, and only after his death did the subject again become “fashionable.”A number of recent developments in physics have evoked the possibility that the treatment of spacetime might involve more than just using the Riemannian spacetime of Einstein’s general relativity, like our failure to quantize gravity, the description of hadron or nuclear matter in terms of extended structures, the accelerating universe, the study of the early universe, and so forth (see Hehl et al. [5]).The smallest departure from a Riemannian spacetime of Einstein’s general relativity consists of admittingtorsion (A.3), arriving at a Riemann-Cartan spacetime, and furthermore, possiblenonmetricity (A.1), resulting in ametric-affine spacetime. Metric-affine gravity is a natural generalisation of Einstein’s general relativity and it was propagated by Einstein himself for some time. In metric-affine gravity we consider spacetime to be a connected real 4-manifold M equipped with a Lorentzian metric g and an affine connection Γ and the characterisation of spacetime by anindependent linear connection Γ immediately distinguishes metric-affine gravity from general relativity. The connection incorporates the inertial properties of spacetime and it can be viewed, according to Weyl [6], as the guidance field of spacetime, while the metric describes the structure of spacetime with respect to its spaciotemporal distance relations.As stated by Hehl et al. in [5], in general relativity the linear connection of its Riemannian spacetime is metric compatible and symmetric and the symmetry of the Levi-Civita connection translates into the closure of infinitesimally small parallelograms and the transition from the flat gravity-free Minkowski spacetime to the Riemannian spacetime in Einstein’s theory can locally be understood as a deformation process. The lifting of the constraints of metric-compatibility and symmetry yields nonmetricity and torsion, respectively. The continuum under consideration is thereby assumed to have a nontrivial microstructure. The geometrical concepts of nonmetricity and torsion arise in the three-dimensional continuum theory of lattice defects; however, see [7, 8]. For a comprehensive review of metric-affine gravity, see [5] as well as [9].This paper has the following structure. In Section2 we introduce the Yang-Mielke theory or gravity. In Section 3 we define our new spacetimes, where in Section 3.1 we recall the known properties classical pp-waves and in Section 3.2 we generalise the notion of a pp-wave to spacetimes with purely axial torsion. Finally, in Section 5 we compare our solutions with existing results and consider future research possibilities. Appendix provides the notation we use throughout the paper.


## 2. Yang-Mielke Theory of Gravity

We consider spacetime to be a connected real 4-manifoldM equipped with a Lorentzian metric g and an affine connection Γ. The unknowns of our theory are the 10 independent components of the metric tensor gμν and the 64 connection coefficients Γλμν. Inquadratic metric-affine gravity we define the action as (3)S≔∫qR,where q is an O(1,3)-invariant quadratic form on curvature R. Independent variation of (3) with respect to the metric g and the connection Γ produces Euler-Lagrange equations which we will write symbolically as (4)∂S∂g=0,(5)∂S∂Γ=0.The Yang-Mills action for the affine connection is a special case of (3) with (6)qR≔RκλμνRλκμν.The objective of this paper is to study the system of (4), (5) in the special case (6). The origins of this theory lie in the works of Élie Cartan, Arthur Eddington, Albert Einstein, Erwin Schrödinger, Tullio Levi-Civita, and Hermann Weyl. The motivation for choosing a model of gravity which is purely quadratic in curvature is explained in detail in Section 1 of [10] and Section 1 of [11]. The results in this paper strongly rely on the work of Yang [12] and Mielke [13] who, respectively, showed that Einstein spaces satisfy (5) and (4). We therefore refer to the special case (6) of the field equations (5) and (4) as theYang-Mielke theory of gravity. There are many works devoted to the study of system (4), (5) in the special case (6) and one can get an idea of the historical development of the Yang-Mielke theory of gravity from the references stated in [11]. Further aspects of the history of this theory are also given in [14]. Detailed descriptions of the irreducible pieces of curvature and quadratic forms on curvature can be found in [10, 15] and our previous work in this theory can be found in [11, 16–18], where much more information and references on the history and development of metric-affine gravity and known solutions of this theory can be found.


## 3. pp-Waves with Purely Axial Torsion

We use pp-waves, which are well known spacetimes in general relativity, in order to construct our solutions. In Section3.1 we first provide a brief reminder on classical pp-waves, following the exposition from [11, 18] and then in Section 3.2 we generalise them to spacetimes with purely axial torsion. See [11, 18] for extensive references therein for much more information on pp-waves and pp-wave type solutions of metric-affine gravity in general.


### 3.1. Properties of Classical pp-Waves

We define app-wave as a Riemannian spacetime which admits a nonvanishing parallel spinor field. It is now a well known fact that pp-waves are solutions of the system of (4), (5), as first shown in [10]. We denote the nonvanishing parallel spinor field appearing in the definition of pp-waves by χ=χa and we assume this spinor field to befixed. Put (7)lα≔σαab˙χaχ-b˙,where σα are Pauli matrices, where we use the spinor formalism introduced in [11, 18]. Then l is a nonvanishing parallel real null vector field. We define the real scalar function, which we call thephase, as(8)φ:M⟶R,φx≔∫l·dx.Put Fαβ≔σαβabχaχb where the σαβ are “second-order Pauli matrices” and σαβac≔1/2(σαab˙ϵb˙d˙σβcd˙-σβab˙ϵb˙d˙σαcd˙) (see [11, 18]). F can be expressed as F=l∧m, where m is a complex vector field satisfying (9)mαmα=lαmα=lαm¯α=0,mαm¯α=-2.Note that it is known that pp-waves can also be defined as a Riemannian spacetime whose metric can be written locally in the form(10)ds2=2dx0dx3-dx12-dx22+fx1,x2,x3dx32in some local coordinates (x0,x1,x2,x3). The corresponding curvature tensor R is linear in f; that is, (11)Rαβγδ=-12l∧∂αβl∧∂γδf,where (l∧∂)αβ≔lα∂β-∂αlβ. The choice of local coordinates in which the pp-metric assumes the form (10) is not unique. We will restrict our choice to those coordinates in which (12)χa=1,0,lμ=1,0,0,0,mμ=0,1,∓i,0.With this choice of local coordinates (10), (12), the phase function becomes φ(x)=x3+const. Formula for the curvature of a pp-wave (11) can now be rewritten in invariant form; that is, (13)R=-12l∧∇⊗l∧∇f,where l∧∇≔l⊗∇-∇⊗l. pp-waves curvature only has two irreducible pieces, that is, (symmetric) trace-free Ricci and Weyl; see [17] for their explicit formulae.


### 3.2. Generalising pp-Waves to Spacetimes with Purely Axial Torsion

Definition 1.
A generalised pp-wave with purely axial torsion is a metric compatible spacetime with pp-metric and torsion(14)T≔∗A,where A is a real vector field defined by A=k(φ)l, where k:R↦R is an arbitrary real function of the phase.Remark 2.
The real vector fieldA is a plane wave solution of the polarized Maxwell equation ∗dA=±idA; see (16) of [18]. This is not surprising as in our special local coordinates the vector field A is the gradient of a scalar function.We list below the main properties of these generalised pp-waves. Note that here and further on we denote by{∇} the covariant derivative with respect to the Levi-Civita connection which should not be confused with the full covariant derivative ∇ incorporating torsion. Using our special local coordinates (10), (12), we can express torsion as (15)T=∓i2kx3l∧m∧m¯.Note that the ∓ sign is chosen to correspond to the sign in (12). Torsion (14) is clearly purely axial, as Tκμν=k(φ)lαεακμν, which is just the totally antisymmetric part of torsion.Remark 3.
Our torsion completely corresponds to Singh’s axial torsion from [19, 20]. Put m=-1/2k(x3) in formula (16) of [19] or put n=0, m=-1/2k(x3) in formula (20) of [20].Remark 4.
The connection of a generalised pp-wave with purely axial torsion is clearly metric compatible. SinceΓκμν=λμν+Kκμν=λμν+1/2Tκμν, we get that (16)∇μgαβ=∇μgαβ-Kημαgηβ-Kημβgαηand {∇}μgαβ=0 as classical pp-waves are metric compatible. However, since our torsion is purely axial, we get that ∇μgαβ=Kαμβ-Kαμβ=0; that is, we have metric-compatibility.The curvature of a generalised pp-wave is(17)R=-12l∧∇⊗l∧∇f+14k2Rel∧m⊗l∧m¯∓12k′Im⁡l∧m⊗l∧m¯.This can be equivalently written down as(18)Rαβγδ=-12l∧∂αβl∧∂γδf+∑i,j=12rijl∧miαβl∧mjγδ,where r11=r22=1/4k2, r12=-r21=±1/2k′. It is a highly nontrivial fact that the torsion generated curvature, that is, RTκλμν=∂μKκνλ-∂νKκμλ+KκμηKηνλ-KκνηKημλ, which is equal to (19)RT=k24Rel∧m⊗l∧m¯∓k′2Im⁡l∧m⊗l∧m¯and the Riemannian curvature simply add up to produce formula (17). We know that the Riemannian part of curvature has two irreducible pieces of curvature, namely, Weyl and (symmetric) trace-free Ricci. It turns out that the torsion also generates Ricci curvature and it reads (20)Ric=12f11+f22-k2l⊗l,where fαβ≔∂α∂βf. Scalar curvature is then clearly zero by the properties of l.Remark 5.
The Ricci curvature is zero if Poisson’s equationf11+f22=k2 is satisfied.Remark 6.
Ricci is parallel iff11+f22=k2+C, in which case Ric=Λl⊗l, for some constant Λ.


## 3.1. Properties of Classical pp-Waves

We define app-wave as a Riemannian spacetime which admits a nonvanishing parallel spinor field. It is now a well known fact that pp-waves are solutions of the system of (4), (5), as first shown in [10]. We denote the nonvanishing parallel spinor field appearing in the definition of pp-waves by χ=χa and we assume this spinor field to befixed. Put (7)lα≔σαab˙χaχ-b˙,where σα are Pauli matrices, where we use the spinor formalism introduced in [11, 18]. Then l is a nonvanishing parallel real null vector field. We define the real scalar function, which we call thephase, as(8)φ:M⟶R,φx≔∫l·dx.Put Fαβ≔σαβabχaχb where the σαβ are “second-order Pauli matrices” and σαβac≔1/2(σαab˙ϵb˙d˙σβcd˙-σβab˙ϵb˙d˙σαcd˙) (see [11, 18]). F can be expressed as F=l∧m, where m is a complex vector field satisfying (9)mαmα=lαmα=lαm¯α=0,mαm¯α=-2.Note that it is known that pp-waves can also be defined as a Riemannian spacetime whose metric can be written locally in the form(10)ds2=2dx0dx3-dx12-dx22+fx1,x2,x3dx32in some local coordinates (x0,x1,x2,x3). The corresponding curvature tensor R is linear in f; that is, (11)Rαβγδ=-12l∧∂αβl∧∂γδf,where (l∧∂)αβ≔lα∂β-∂αlβ. The choice of local coordinates in which the pp-metric assumes the form (10) is not unique. We will restrict our choice to those coordinates in which (12)χa=1,0,lμ=1,0,0,0,mμ=0,1,∓i,0.With this choice of local coordinates (10), (12), the phase function becomes φ(x)=x3+const. Formula for the curvature of a pp-wave (11) can now be rewritten in invariant form; that is, (13)R=-12l∧∇⊗l∧∇f,where l∧∇≔l⊗∇-∇⊗l. pp-waves curvature only has two irreducible pieces, that is, (symmetric) trace-free Ricci and Weyl; see [17] for their explicit formulae.


## 3.2. Generalising pp-Waves to Spacetimes with Purely Axial Torsion

Definition 1.
A generalised pp-wave with purely axial torsion is a metric compatible spacetime with pp-metric and torsion(14)T≔∗A,where A is a real vector field defined by A=k(φ)l, where k:R↦R is an arbitrary real function of the phase.Remark 2.
The real vector fieldA is a plane wave solution of the polarized Maxwell equation ∗dA=±idA; see (16) of [18]. This is not surprising as in our special local coordinates the vector field A is the gradient of a scalar function.We list below the main properties of these generalised pp-waves. Note that here and further on we denote by{∇} the covariant derivative with respect to the Levi-Civita connection which should not be confused with the full covariant derivative ∇ incorporating torsion. Using our special local coordinates (10), (12), we can express torsion as (15)T=∓i2kx3l∧m∧m¯.Note that the ∓ sign is chosen to correspond to the sign in (12). Torsion (14) is clearly purely axial, as Tκμν=k(φ)lαεακμν, which is just the totally antisymmetric part of torsion.Remark 3.
Our torsion completely corresponds to Singh’s axial torsion from [19, 20]. Put m=-1/2k(x3) in formula (16) of [19] or put n=0, m=-1/2k(x3) in formula (20) of [20].Remark 4.
The connection of a generalised pp-wave with purely axial torsion is clearly metric compatible. SinceΓκμν=λμν+Kκμν=λμν+1/2Tκμν, we get that (16)∇μgαβ=∇μgαβ-Kημαgηβ-Kημβgαηand {∇}μgαβ=0 as classical pp-waves are metric compatible. However, since our torsion is purely axial, we get that ∇μgαβ=Kαμβ-Kαμβ=0; that is, we have metric-compatibility.The curvature of a generalised pp-wave is(17)R=-12l∧∇⊗l∧∇f+14k2Rel∧m⊗l∧m¯∓12k′Im⁡l∧m⊗l∧m¯.This can be equivalently written down as(18)Rαβγδ=-12l∧∂αβl∧∂γδf+∑i,j=12rijl∧miαβl∧mjγδ,where r11=r22=1/4k2, r12=-r21=±1/2k′. It is a highly nontrivial fact that the torsion generated curvature, that is, RTκλμν=∂μKκνλ-∂νKκμλ+KκμηKηνλ-KκνηKημλ, which is equal to (19)RT=k24Rel∧m⊗l∧m¯∓k′2Im⁡l∧m⊗l∧m¯and the Riemannian curvature simply add up to produce formula (17). We know that the Riemannian part of curvature has two irreducible pieces of curvature, namely, Weyl and (symmetric) trace-free Ricci. It turns out that the torsion also generates Ricci curvature and it reads (20)Ric=12f11+f22-k2l⊗l,where fαβ≔∂α∂βf. Scalar curvature is then clearly zero by the properties of l.Remark 5.
The Ricci curvature is zero if Poisson’s equationf11+f22=k2 is satisfied.Remark 6.
Ricci is parallel iff11+f22=k2+C, in which case Ric=Λl⊗l, for some constant Λ.


## 4. New Solutions of Yang-Mielke Theory of Gravity

In this section we aim to use the spacetimes introduced in Section3 in order to construct new solutions of the Yang-Mielke theory of gravity. The main result of this paper is the following.Theorem 7.
Generalised pp-waves with purely axial torsion with parallel{Ric} are solutions of (4), (5) in the special case (6).Remark 8.
Note that by{Ric} we denote the Ricci curvature generated by the Levi-Civita connection only. The condition {∇}{Ric}=0 implies that f11+f22=C. Note that the result also holds if Ric is assumed to be parallel.Remark 9.
In the special case (6), we call (5) the Yang-Mills equation for the affine connection; that is,(21)∂νRμν+Γν,Rμν=0,where [Γν,Rμν]κλ=ΓκνηRηλμν-ΓηνλRκημν. We call (4) in the special case (6), thecomplementary Yang-Mills equation; that is, (22)H-14trHg=0,where H=Hνρ≔RκλμνRλκμρ. Equivalently, (22) can be written down as (23)RκλναRλκνβ-14gαβRκλμνRλκμν=0.See [21] for the explicit derivations of (21) and (22).Proof of Theorem7.
Since we know (see, e.g., [11, 18, 22]) that classical pp-waves of parallel Ricci curvature are solutions of (4), (5) in the special case (6), it is enough to show the result for the torsion generated part of curvature (19). In proving that generalised pp-waves solve (21) and (22), we will use (9), special local coordinates (10), (12), and the formulae for curvature (17), (18), torsion (15), and torsion generated curvature (19). To show that (21) is satisfied, we only need to show that (24)∂νRTμν+Kν,RTμν=0,since the curvature is the sum of the Riemannian curvature (13) and the torsion generated curvature (19), the connection of the sum of the Christoffel symbol and contortion, and since classical pp-waves solve the Yang-Mills equation. Now, since F=l∧m, in special local coordinates (10), (12), F takes the form (25)Fαβ=01∓i0-1000±i0000000and since the function k(φ) is the function of x3 in special local coordinates, using the formula for curvature (19) we directly get that ∂νRTμν=0.
Using the explicit formula for torsion (15), the fact that it is purely axial, which implies that T=2K, the explicit formula for torsion generated curvature (19), and special local coordinates (10), (12), we get that the only nonzero term of ΓκνηRηλμν is for κ=0, λ=3, and μ=0; that is, -1/2k·k′. However, the only nonzero term of ΓηνλRκημν is also when κ=0, λ=3, and  μ=0; that is, -1/2k·k′, so these two terms cancel out. Hence, (21) is satisfied.
Checking that all the terms in (22) are zero is a straightforward exercise, using the formulae for curvature (17), (18), special local coordinates (10), (12), and (9).


## 5. Discussion and Comparison with Existing Solutions

Vassiliev [10] proved the uniqueness of Riemannian solutions of the system of (4), (5), so we are left with searching for non-Riemannian solutions, that is, those incorporating torsion and possible nonmetricity. Vassiliev [10] presented one non-Riemannian solution of system (4), (5) in the most general case of the purely quadratic action (3), which was atorsion wave solution with explicitly given torsion. This result was previously presented in [23] for the Yang-Mills case (6) and was first independently obtained by Singh and Griffiths [24]. Vassiliev went on to conclude that this torsion wave was a non-Riemannian analogue of a pp-wave and whence came the motivation for generalising the notion of a classical Riemannian pp-wave to spacetimes with torsion in such a way as to incorporate the non-Riemannian torsion wave solution into the construction.Constructing vacuum solutions of quadratic metric-affine gravity in terms of pp-waves is a recent development. Classical pp-waves of parallel Ricci curvature were first shown to be solutions of (4), (5) in [10, 22, 25]. There are a number of other publications in which authors suggested various generalisations of the concept of a classical pp-wave; see [26] and extensive references therein. These generalisations were performed within the Riemannian setting and usually involved the incorporation of a constant nonzero scalar curvature. Our construction in [11, 16–18] generalised the concept of a classical pp-wave in a different direction; we added torsion while retaining zero scalar curvature. We preserved this approach in the current paper.An interesting generalisation of the concept of a pp-wave was presented by Obukhov in [27]. Obukhov was motivated by his previous result [26] which deals with the Riemannian case. The ansatz for the metric and the coframe of [27] is exactly the same as in the Riemannian case. However, the connection extends the Christoffel connection so that torsion andnonmetricity (A.1) are present and are determined by this extension of the connection. Obukhov’s gravitational wave solutions provide a minimal generalisation of the pseudoinstanton (see [15]), in the sense that nonmetricity does not vanish and that curvature has two irreducible pieces. We chose not to take this approach, as our connection remains metric compatible.In our previous work [11, 16–18], we presented results which were new explicit vacuum solutions of the system of our field equations (4), (5) and called these generalised pp-waves with torsion. However, it is important to note that the torsion there waspurely tensor, while the torsion considered in the current paper ispurely axial. The previous generalisation was done similarly to the approach of this paper, by using the pp-metric and giving an explicit torsion, identical to the torsion wave obtained by Vassiliev in [10]. We further explored the properties and characteristics of these generalised pp-waves, showing that they are indeed solutions of the system of our field equations (4), (5) in the most general case. Generalised pp-spaces with purely tensor torsion of parallel Ricci curvature appear to admit a sensible physical interpretation, which we explored in detail in [11], where we gave a comparison with a classical model (namely, Einstein-Weyl theory), constructed pp-wave type solutions of this theory, and pointed out that generalised pp-waves of parallel Ricci curvature are very similar to pp-wave type solutions of the Einstein-Weyl model. The main difference in using the metric-affine model lies in the fact that Einstein-Maxwell and Einstein-Weyl theories contain the gravitational constant, whereas our model is conformally invariant and the amplitudes of the two curvatures, namely, the torsion generated curvature (19) and the metric generated curvature (13) are totally independent.We aim to be able to do a similar feat using generalised pp-waves with purely axial torsion, that is, first showing that they are solutions of the field equations (4), (5) in the most general case, by writing down the field equations explicitly under the assumption of purely axial torsion. We also hope to be able to similarly compare these solutions to the solutions of Einstein-Weyl theory in order to provide a more detailed physical interpretation of these spacetimes.In [28] Mielke and Romero considered axial torsion in the Einstein-Cartan context. We are particularly interested in the section in which the authors recapitulate the minimal coupling of gravity to Dirac fields and where they state that the coupling of axial torsion to the axial current is the only additional term in a prolongation to Riemann-Cartan spacetimes. This will make a significant influence on our reasoning once we attempt to provide a sensible physical interpretation of our solutions.It is interesting to note that in [29] Guilfoyle and Nolan discuss the initial value problem for the Yang-Mills equations and argue that while the long term existence has been established, it is not expected that Yang’s equations have a long term well-posed initial value problem. Of course, the inclusion of torsion can be very problematic in this context. As stated in the proof of the main result in [29], Yang’s equations constitute a third-order quasi-linear system of partial differential equations and fall outside of the wave equations framework used for the initial value problem of general relativity and gauge theory. The authors separate the metric and the connection and propagate them separately by wave equations and state that if the connection and metric are initially compatible, they remain so throughout. It is important to note that Yang was looking for Riemannian (i.e., torsion-free) solutions, so he specialised (5) to the Levi-Civita connection,after the variation was carried out. In this case, (5) reduces to ∇λRicκμ-∇κRicλμ=0. However, according to [22], for a generic 16-parameter action, (5) restricted to the Levi-Civita connection becomes ∇Ric=0. Since our connection is metric compatible as well (see Remark 4) and Ricci is assumed to be parallel, we expect this to also be the case for our solutions and this is a matter which we will look at and hopefully answer in the near future.The two papers of Singh [19, 20] were of special interest to us in our task of finding new vacuum solutions of quadratic metric-affine gravity. Singh [20] presents solutions of the field equations (4), (5) for the Yang-Mills case (6) for a purelytrace torsion. We are not sure whether these torsion waves can also be used to create new generalised pp-wave solutions of this theory at this time. In [19] Singh presents solutions of the field equations (4), (5) for the Yang-Mills case (6) for a purelyaxial torsion and constructed a class of solutions that cannot be obtained using the double duality ansatz; see, for example, [15]. Singh used the “spin coefficient technique” from his previous work with Griffiths [30]. Following the reasoning behind the generalised pp-waves of [18] that were shown to be solutions of the field equations (4), (5), where we “combined” the pp-metric and the purely tensor torsion waves to obtain a new class of solutions for quadratic metric-affine gravity, we wanted to be able to do the same with purely axial torsion waves. This paper has managed to do just that in the special case (6), and we hope to be able to obtain the general result. The next obvious step would be to provide a physical interpretation of these new solutions by comparing them to existing classical solutions, like it was done in [11] for purely tensor torsion generalised pp-waves.



---

*Source: 239076-2015-08-12.xml*