Divergent part of the stress-energy tensor for Maxwell's theory in curved space-time: a systematic derivation

In this paper the Feynman Green function for Maxwell's theory in curved space-time is studied by using the Fock-Schwinger-DeWitt asymptotic expansion; the point-splitting method is then applied, since it is a valuable tool for regularizing divergent observables. Among these, the stress-energy tensor is expressed in terms of second covariant derivatives of the Hadamard Green function, which is also closely linked to the effective action; therefore one obtains a series expansion for the stress-energy tensor. Its divergent part can be isolated, and a concise formula is here obtained: by dimensional analysis and combinatorics, there are two kinds of terms: quadratic in curvature tensors (Riemann, Ricci tensors and scalar curvature) and linear in their second covariant derivatives. This formula holds for every space-time metric; it is made even more explicit in the physically relevant particular cases of Ricci-flat and maximally symmetric spaces, and fully evaluated for some examples of physical interest: Kerr and Schwarzschild metrics and de Sitter space-time.


Introduction
The study of quantum gauge field theories and gravitation is a necessity connected to black hole theory and quantum cosmological models, but beyond that it is also a crucial intellectual achievement. On one hand, electroweak and strong interactions are described by Yang-Mills theories, and are satisfactorily set in a quantum framework; on the other hand, altough General Relativity is in many ways a gauge theory too [1], it stands apart from the other three forces of nature, and a quantum theory of gravity does not yet exist, at least as a coherent discipline. Nevertheless, it is possible to discuss the influence of the gravitational field on quantum phenomena: one can study the regime for quantum aspects of gravity in which the gravitational field is described as a classical background through Einstein's theory while matter fields are quantized; this is reasonable as long as length and time scales of quantum processes of interest are greater than the Planck values (l P lanck ≡ (G /c 3 ) 1/2 ∼ 1.616 × 10 −33 cm, t P lanck ≡ (G /c 5 ) 1/2 ∼ 5.39 × 10 −44 s). Since Planck length is so small (twenty orders of magnitude below the size of an atomic nucleus), one can hope that such a "semiclassical" approach has some predictive power. Therefore one is naturally led to the subject of quantum field theory in a curved background spacetime. Its basic physical prediction is that strong gravitational fields can "polarize" the vacuum and, when timedependent, lead to pair creation; moreover, in a curved space-time, notions of "vacuum" and "particles" need a deeper discussion than in the flat case. These two fundamental results are strongly linked to the most important predictions of the theory, i.e., Hawking and Unruh effects (see Refs. [2], [3], [4]): according to the Hawking effect, a classical, spherically symmetric black hole of mass M has the same emission spectrum of a black body having the temperature T Hawking ≡ 1 8πM ; according to the Unruh effect, from the point of view of an accelerating observer, empty space contains a gas of particles at a temperature proportional to the acceleration. For a detailed treatise on these subjects, see also Refs. [5], [6], [7].
In this context, DeWitt's formalism for gauge field theories is a powerful tool (see Refs. [8], [9], [10], [1]): it provides a framework in which the quantization of fields possessing infinite dimensional invariance groups may be carried out in a manifestly covariant fashion, even in curved space-time; moreover, it makes it possible to classify all gauge theories in a purely geometrical way, i.e., by the algebra which the generators of the gauge group obey; the geometry of such theories is the fundamental reason underlying the emergence of ghost fields in the corresponding quantum theories, too.
For a non-gauge theory, it is well known that the transition amplitude out|in between any two (super)state vectors determined by sone unspecified boundary conditions may be expressed as where N is a normalization factor, while µ[φ] is a suitable measure functional. 1 DeWitt regards the set of all fields as an infinite-dimensional manifold, the space of histories, on which an action functional is defined; then gauge transformations are viewed as flows which leave the action functional unchanged; when the flows Q α satisfy the equations of a closed (altough infinite-dimensional) Lie group (this is the case for Yang-Mills theories and General Relativity), under the group action the space of histories is separated into orbits; one could say that it is in the space of orbits that the real physics of the system takes place; one can then choose on the manifold a new set of coordinates made of two parts: the first one labelling the orbit, I A , and the second one, K α , labelling a particular field configuration belonging to the specified orbit; when one writes down the functional integral and reverts to the original coordinates, one finds out that two new terms appear: where Ω ≡ 1 2 κ αβ K α K β is the gauge-breaking (or gauge-averaging) term, while χ α M α β ψ β is the ghost contribution, which involves two ghost fields; they are fermionic for a bosonic theory and bosonic for a fermionic theory. Therefore one refers tō as the full action functional.
In this paper the Feynman Green function for Maxwell's theory in curved space-time is discussed, following the footsteps of DeWitt and [14] and [15]: both ζ-function regularization method and Fock-Schwinger-DeWitt ansatz are used in order to obtain an asymptotic formula for the Feynman propagator, valid for small values of the geodetic distance; the expansion obtained exhibits the familiar logarithmic singularity which occurs for massive theories in flat space-time and, generally, even for massless theories but in curved space-time. Then the point-splitting method is presented as a valuable tool for regularizing divergent observables such as the stress-energy tensor: one finds out that it can be completely expressed in terms of second derivatives of the Hadamard Green function, which is also closely linked to the effective action. Most of the material in Secs. 2, 3 is quite standard, but nevertheless necessary to obtain a self-contained presentation. In Sec. 4 an original calculation is presented: a short, closed formula for the divergent part of the stress-energy tensor, originating from a careful handling of more than two thousand terms; for this purpose, a program has been written in FORM, which is a symbolic manipulation system whose original author is Jos Vermaseren at NIKHEF (see Refs. [16], [17], [18]). This formula holds for every space-time metric; in Secs. 5 and 6, it is made even more explicit in the physically relevant particular cases of Ricciflat and maximally symmetric spaces, and fully evaluated for some relevant examples: Kerr and Schwarzschild metrics (which are Ricci-flat) and de Sitter metric (which is maximally symmetric); see Refs. [19], [20] for an up-todate review. Concluding remarks are presented in Sec. 7, and relevant details are given in the Appendices.

Quantum Maxwell Theory in Curved Space-Time and Feynman Propagator
In this section, the task will be the evaluation of the photon Green's functions in curved space-time. Following DeWitt's approach and using the minimal coupling, the full action functional for the theory is (our spacetime metric has signature (−, +, +, +)) The first term is the classical action functional for the field A µ , while the second and the third ones are the gauge-averaging and the ghost ones, respectively; moreover, ξ is a real parameter which accounts for the behaviour under rescaling of the gauge-fixing coordinate K α : (2. 2) The full action functional (2.1) can be put in the form

4)
Hence the equation for the photon Green's functions is In order to study these equations, we introduce two non-physical Hilbert spaces spanned by the basis kets |x, µ , |x , respectively; for them, the following orthogonality relations hold: (2.8) Of course, |x is the familiar Dirac notation for the eigenfunctionals of the position operator which has continuous spectrum, while the index of both |x, µ and the associated "bra" x, µ| is viewed as that of a covariant vector density of weight 1/2. The "Hamiltonian" operators H(ξ), H 0 associated with P µν (ξ) and P 0 , respectively, are defined by (2.10) Then the "operator" solution with the Feynman prescription is By taking matrix elements of the previous equation we obtain Thus the "transition amplitude" x, µ; τ |x ′ , ν; 0 (ξ) satisfies the Schrödinger equation associated to H(ξ): with the initial condition For arbitrary values of ξ, the operator P µν (ξ), as well as P λ µ ≡ g ρµ P ρλ (ξ), is non-minimal, i.e. the wavelike-operator part −g µν + R µν is spoiled by (1 − 1/ξ)∇ µ ∇ ν . Nevertheless, if one knows x, µ; τ |x ′ , ν; 0 (ξ) at ξ = 1, one can use this solution, here denoted by x, µ; τ |x ′ , ν; 0 (1) , to evaluate x, µ; τ |x ′ , ν; 0 (ξ) according to the Endo formula (see Ref. [21]) (2.16) The previous equation plays a key role in evaluating the regularized photon Green function, as we shall see in the following. Once the transition amplitude is known, equation (2.12) describes the massless limit of the Feynman propagator (for which one would have to add an infinitesimal negative imaginary mass). At this stage, formula (2.12) needs a suitable regularization. Following Endo, we use ζ-function regularization and introduce a regularization parameter µ A defining (any suffix to denote regularization of the photon Green function is omitted for simplicity of notation): (2.17) It should be stressed that the limit s → 0 should be taken at the very end of all calculations, and cannot be brought within the integral.
The transition amplitude x, µ; τ |x ′ , ν; 0 (1) is known as τ → 0 and as (where the bi-scalar σ(x, x ′ ), which we shall call geodetic interval or world function, is equal to half the square of the distance along the geodesic between x and x ′ ) through its Fock-Schwinger-DeWitt asymptotic expansion (Refs. [8], [1], [22], [23], [14]) x, µ; τ |x ′ , ν; 0 where ∆ is the Van-Vleck Morette determinant ∆ ≡ −|g| −1/2 det(σ µν ′ )|g ′ | −1/2 and the coefficient bivectors b n µν ′ are evaluated by solving a recursion formula obtained upon insertion of (2.18) into eq. (2.14); such a recursion formula reads The equations (2.19) and (2.20) are solved by b 0 µν ′ = g µν ′ , which is known as the geodetic parallel displacement bi-vector; it is characterized by the following fundamental property: by applying it to a local contravariant vector V µ ′ at x ′ one obtains the covariant form of the vector which results from displacing V µ ′ in a parallel fashion along the geodesic from x ′ to x: It can be shown (see Ref. [15] for the detailed calculations) that as x ′ approaches x (which implies σ(x, x ′ ) → 0), eqs. (2.17), (2.18), (2.19) µν ′ (s), (2.22) where, after having defined What is crucial for us is the s → 0 limit of the sum in the previous equation. Indeed, on studying first, for simplicity, the case when the gaugefield operator reduces to a minimal (wavelike) operator, i.e., at ξ = 1, one finds where the first term on the rhs is precisely the first term in the Hadamard asymptotic expansion at small σ(x, x ′ ) (see Ref. [14] ). On the other hand, the Hadamard Green function is, apart from a factor 2, the imaginary part of the Feynman Green function, in agreement with formula (2.22). Eventually, we find therefore, at small σ(x, x ′ ), i.e., the "flat" Feynman propagator, with the iǫ term restored, plus correction resulting from the gauge parameter (ξ = 1 leading to a non-minimal operator) and from the non-vanishing curvature. It can be checked (see Ref. [15]) that this infinite sum (2.25) is also able to recover the familiar log σ(x, x ′ ) singularity, which occurs for massive theories in flat space-time and, more generally, even for massless theories (as in our case) but in curved space-time.

Second Derivatives, Stress-Energy Tensor
In this section it will be shown that, given a field theory (in the present case, quantum Maxwell's theory), there is a close relation between second derivatives of the Hadamard Green's functions, stress-energy tensor and effective action, following the footsteps of Christensen and DeWitt (see Refs. [14], [9]). In a classical field theory, the stress-energy tensor can be obtained as For a free theory, this object is quadratic in the fields; when dealing with the associated quantum theory, the expectation value of this observable is, in general, divergent: this happens because the two field operators are taken at the same space-time point. An useful way to regularize the expectation value of the stress-energy tensor is to insert into the formal expression for T µν not the field operators themselves but operators that have been smeared out by means of a smooth function s of compact support: The resulting operator does exist and the behaviour of its (finite) expectation value may be studied as the size of the support of s(x) tends to zero. A regularization method equivalent to the one of the smearing method but easier to apply in practice is simply to separate the points at which the two fiels in T µν are taken and then to examine the tensor as the points are brought together again.
For the action functional (2.1), the stress-energy tensor is The result is The detailed calculations are provided in Appendix A. In order to exploit the point split method, we write where, in order to avoid any confusion with the Feynman Green function in the minimal case (ξ=1), the Hadamard Green function shall be named G

In a similar manner
and where G (H) (x, x ′ ) is the Hadamard Green's function for the ghost fields.
Hence the point-split method yields

17)
2 It should be pointed out that this is an abuse of notation: given for example two 2-point tensors B, C, whose components are B µν ′ , C µν ′ , respectively, one can only sum the components pertaining to the same point and characterized by the same indices: in fact does not define a 2-point tensor; therefore, throughtout the following, where the DeWitt supermetric has been introduced: We should now specify in which order the various operations we rely upon are performed. Indeed, in the evaluation of the Feynman Green function, we first sum over n and then take the s → 0 limit. Here, we eventually obtain the energy-momentum tensor of the quantum theory according to the point-splitting procedure, with the understanding that the coincidence limit lim x ′ →x is the last operation to be performed. It is clear from (3.15), (3.16), (3.17) that our analysis of the stress-energy tensor is virtually completed if we can provide a closed expression for the coincidence limit of the second derivatives of the Hadamard Green function. It is easy to see that divergences appear; in the minimal case (ξ = 1), on denoting by ε the regulator that we are employing, the divergent part of G with the convention that the coincidence limit lim x ′ →x has to be taken for the quantities in square brackets. In many applications, we are interested in finding the vacuum expectation value of the stress-energy tensor in the vacuum state defined prior to any dynamics in the background gravitational field. This quantity, properly regularized and renormalized, gives us all the information we want about particle production and vacuum polarization. It is the object we choose to use as source in the semiclassical gravitational field equations, when doing a back-reaction problem. So why are T µν matrix , the Green functions and their divergences interesting? The answer is the following: DeWitt showed (see Ref. [9]) that where T µν finite vanishes when there is no particle annihilation, is always finite, and satisfies the conservation equation T µν finite ;ν = 0 (the proof of this beautiful result is described in Appendix B). Hence the divergences appearing in T µν vac and T µν matrix are identical. Regularization of T µν matrix yields the regularized form of T µν vac . Regularizing T µν matrix gives: where T µν div contains the infinite pieces which we will renormalize away by adding infinite counterterms onto the classical action for the gravitational field and T µν matrix,ren is the remaining finite physical part of the matrix element. Renormalizing T µν div away also gives us a renormalized T µν vac to be used as the source in (3.21). Another important fact is the close link between Feynman (and Hadamard) Green's functions and the so-called effective action W : DeWitt showed that Having defined he also found that Thus the renormalized effective Lagrangian is where L div can be evaluated by means of the divergent part of the asymptotic expansion of Feynman and Hadamard Green's functions. Interestingly, the divergent part of the one-loop effective action for the quantum version of Einstein gravity has been recently discussed in Ref. [24] in relation to renormalization group equations for the Newton constant and the cosmological constant; the reader may find there an up-todate discussion of the concepts just introduced in our section.

Divergent part of T µν
In this section we will show the results of the calculation pertaining to the divergent part of the coincidence limit of the Hadamard Green function and their application to the evaluation of the divergent part of T µν ; the divergent part of the Hadamard Green function is (see (3.19)) 2) together with coincidence limits for the coefficient bivectors and for the remaining geometrical quantities which appear in the Fock-Schwinger-DeWitt asymptotic expansion (most of them are carefully derived in Appendices C, D) one obtains In order to obtain the divergent part of T µν , one also needs 1. The so-called quantum Ward identities: they constitute a relation between gauge-field Green's functions and ghost Green's function. In our case, they read Therefore, by taking another covariant derivative, one obtains 2. An expression for the divergent part of the coincidence limit of G ρσ ′ ;µν ′ . They are easily obtained by using the parallel displacement matrix: The final result is therefore Although the expressions for the divergent part of G (H) γβ ′ ;ρτ ′ and T µν div may seem cumbersome, there is a systematic way to deal with them. Indeed, a more careful inspection shows that they result from a very large number of terms: by looking at the coincidence limits in Appendices C, D, it is easy to see that each divergent part of G (H) γβ ′ ;ρτ ′ is obtained from the sum of eighty contractions variously involving the metric tensor, the Ricci and Riemann tensor, and that T µν div is obtained by summing thirty of these objects; therefore expression (4.10) for T µν div results from more than two thousand terms. For this purpose, a program has been written in FORM. In the following two sections, eq. (4.10) will be made more explicit in some physically relevant particular cases.

Ricci-flat space-times
In light of their role in General Relativity, Ricci-flat metric tensors are very relevant, since they solve the Einstein vacuum equations. Whenever one considers a Ricci-flat metric, only four terms are left in the sum eq. (4.10), i.e., the ones which only involve the Riemann tensor and its derivatives: An important example of vacuum solution is the Kerr metric, which describes the exterior of a rotating, stationary, axially symmetric star; it depends on two parameters: the Schwarzschild radius r s ≡ 2GM c 2 and the angular momentum J, through a ≡ J M c ; in a spherical coordinate system (t, r, θ, φ), the metric components g µν form the matrix where g 00 = rr s r 2 + a 2 cos 2 (θ) − 1, g 11 = r 2 + a 2 cos 2 (θ) a 2 + r 2 − rr s , g 22 = r 2 + a 2 cos 2 (θ), g 33 = sin 2 (θ) rr s sin 2 (θ)a 2 r 2 + a 2 cos 2 (θ) + a 2 + r 2 , g 03 = g 30 = arr s sin 2 (θ) r 2 + a 2 cos 2 (θ) .
Of course, if J = 0, then a = 0, and the Kerr metric reduces to the Schwarzschild metric; in this case, the same calculations yield

Maximally symmetric spaces
Modern cosmology is based on the hypothesis that on a large enough scale the universe is spatially homogeneous and isotropic. Together, these two assumptions are known as the cosmological principle. As is well known, spaces which are both spatially homogenous and isotropic are maximally symmetric, i.e., they possess the largest possible number of Killing vector fields which in a n-dimensional manifold equals n(n + 1)/2. It can be shown that the following holds for a maximally symmetric space: 1. The scalar curvature R is a constant; 2. The Ricci tensor is proportional to the metric tensor, i.e., 3. The Riemann curvature tensor is given by As a consequence, all terms which involve derivatives in eq. (4.10) vanish; therefore only nine terms are left in the sum, and eq. (4.10) takes the simplified form A crucial example is de Sitter space, which is the maximally symmetric vacuum solution of Einstein's field equations with a positive cosmological constant Λ (corresponding to a positive vacuum energy density and negative pressure), actually; the cosmological constant is linked to the Hubble constant by It is often useful to coordinatize the space-time in two different ways, depending upon whether one wishes to think of it as an expanding Friedmann-Lemaître-Robertson-Walker or a static universe with an event horizon. In the former case (s, χ, θ, φ) are used, while (t, r, θ, φ) coordinates are employed in the latter; the metric components thus become where C 00 = 5H 4 2 − 2H 2 r 2 , C 11 = 5 2 H 4 (−1 + H 2 r 2 ), (6.7)

Concluding remarks
In this paper the Feynman propagator for Maxwell's theory in curved spacetime has been described by means of the Fock-Schwinger-DeWitt asymptotic expansion; its crucial role has been emphasized, together with the pointsplitting method, in the evaluation and regularization of quadratic (in the dynamical field) observables. Among these, there is the stress-energy tensor: its matrix element has been derived in terms of second covariant derivatives of the Hadamard Green function of the electromagnetic field. Remarkably, the divergences occurring in T µν vac and T µν matrix are identical, therefore regularizing T µν matrix is equivalent to regularizing T µν vac . An original computation has been then presented: a concise, explicit formula for the divergent part of the stress-energy tensor. This has been obtained from a careful handling of more than two thousand terms, and in order to perform such a calculation, a program has been written in FORM (see Refs. [16], [17], [18]). Such a formula holds for every space-time, and is fully evaluated for some relevant examples: Kerr and Schwarzschild metrics (which are Ricciflat) and de Sitter metric (which is maximally symmetric); see Refs. [19], [20] for an up-todate review. As far as we know, our original results in Eqs. [25], [26]). In any theory of interacting fields the set of currents that describe the interaction is of fundamental importance; in General Relativity, these currents are the components of the stress-energy tensor, therefore the main problem in developing a quantum field theory in curved space-time is precisely to understand the stress-energy tensor (see Ref. [9]). Compared to the flat space-time case, in a curved background the resulting renormalized stress-energy tensor is covariantly conserved, of course, but it possesses a state-independent anomalous trace (see Refs. [27], [28], [29], [30]).
The results obtained are interesting also in the context of effective action theory in curved space-time, whose divergent part is essential to discuss renormalization group equations for the Newton constant and the cosmological constant [24]. Moreover, they can be used to obtain a proper source in the semiclassical gravitational field equations, when doing a back reaction problem, for every background gravitational field.

A T µν Calculations
In this appendix the calculations regarding the derivation of (3.3) from (3.7), (3.8), (3.9) are explicitly shown: Maxwell calculations: T µν gauge calculations: Integrating by parts on the last line, one obtains T µν ghost calculations: Upon integrating by parts on the last line, one obtains = − 1 2 |g(x)| 1/2 χ ψg µν δg µν +|g(x)| 1/2 χg να g µβ δg αβ ψ ;νµ −|g(x)| 1/2 χg νµ g ρη δg νη ψ ;ρµ − |g(x)| 1/2 χ ;µ g νµ g ρη δg νη ψ ;ρ + 1 2 |g(x)| 1/2 χ ;η g νµ g ρη δg µν ψ ;ρ + 1 2 |g(x)| 1/2 χg νµ g ρη δg µν ψ ;ρη = − 1 2 |g(x)| 1/2 χψ α ;α g µν δg µν +|g(x)| 1/2 χψ ;αβ δg αβ −|g(x)| 1/2 χψ ;ην δg νη − |g(x)| 1/2 χ ;µ ψ ;η δg µη Therefore T µν ghost = χ ;α ψ ;α g µν − (χ ;µ ψ ;ν + χ ;ν ψ ;µ ) . In this appendix the proof of the following fundamental result will be outlined: where T µν finite vanishes when there is no particle annihilation, is always finite, and satisfies the conservation equation T µν finite ;ν = 0. Let us assume that space-time has two causally connected stationary regions, an "in" region and an "out" region, each possessing complete Cauchy hypersurfaces and a timelike Killing vector, which makes it possible to define positive and negative frequencies. Let us consider a free theory, i.e., a theory whose action fuctional S is quadratic in the (real) dynamical field; then the equation of motion is given in terms of a linear, self-adjoint, differential operator F , to which a conserved inner product on the space of solutions is associated. Hence, given a complete set {u i } of normalised basis solutions which contain only positive frequencies, the field solution can be expanded in the form By using the canonical (anti)commutation relations, or, in a more elegant and manifestly covariant way, by using the Peierls [31] definition of (anti-)commutator, it is easy to see that the operator coefficients in the expansion satisfy the (anti-)commutation relations This operator algebra serves in the traditional fashion to define a Fock space and a "vacuum" state: In our case, there are two sets {u i in }, {u i out } of normalised basis solutions which contain only positive frequencies, associated with the "in" and "out" regions, respectively; they will be connected by a Bogoliubov transformation The annihilation operators in the "in" and "out" regions are related by

B.2 Creation and Annihilation Amplitudes, Vacuumto-Vacuum Amplitude, Relations of its divergencies with those of T µν
Of particular importance in quantum cosmology are the many-particle production and annihilation amplitudes: It can be easily proven that the production amplitudes V i 1 ...in and the annihilation amplitudes Λ i 1 ...in obey where p denotes a summation over the n! 2 n/2 (n/2)! distinct pairings of the labels i 1 , ..., i n . The previous equations reveal that particle production and annihilation processes as composed of individual pair creation and annihilation events.
Consider now an infinitesimal change δg µν in the metric tensor; it yields a change δS in the action functional for the field φ; if the support of δg µν is confined to the space-time region between the "in" and "out" regions then, by Schwinger variational principle, it follows that: Introduce now the following notation, in which integration over space-time coordinates is suppressed: Then a more precise notation for the stress energy tensor can be introduced: Using the field expansion and the creation/annihilation amplitudes, one obtains The first term is (B.29) while the second term is zero when there is no particle annihilation (because of the presence of Λ ij ) and is always finite; let us show that it satisfies the conservation equation; it suffices to note that and that i.e., the conservation equation. Hence it is proven that where T µν finite is zero when there is no particle annihilation, is always finite, and satisfies the conservation equation T µν finite ;ν = 0; it can be expressed as C World Function: Coincidence Limits C.1 General equations satisfied by the covariant derivatives of the world function Following Synge in Ref. [32], we will show a method to calculate the coincidence limits of the covariant derivatives of the world function, up to order six; these quantities are crucial in the evaluation of the divergent part of the stress-energy tensor. First, one needs to recall the fundamental equations satisfied by the world function: Differentiating the first equation, and indicating with a subscript that a certain index is free, one obtains while differentiating the second one, one obtains (C.7) σ ;α 1 α 2 α 3 α 4 α 5 α 6 − σ ;α 1 α 3 α 2 α 4 α 5 α 6 = −R α 1 λα 2 α 3 ;α 4 α 5 α 6 σ ;λ − R α 1 λα 3 α 2 ;α 4 α 5 σ ;λ α 6 −R α 1 λα 2 α 3 ;α 4 α 6 σ ;λ α 5 − R α 1 λα 3 α 2 ;α 4 σ ;λ For the sake of readability, the following notation will be introduced: when an index is not a summation index, it will be indicated with a number, e.g.

D Coefficient Bivectors: Coincidence Limits
We will derive the coincidence limits of the following coefficient bivectors: ; these quantities, together with the fundamental formula for the derivatives of the coincidence limit of bitensors ..;γ (x, x ′ )] make it possible to evaluate explicitly the right-hand side in (3.19).