Electromagnetic vacuum densities induced by a cosmic string

We investigate the influence of a generalized cosmic string in (D+1) -dimensional spacetime on the local characteristics of the electromagnetic vacuum. Two special cases are considered with flat and locally de Sitter background geometries. The topological contributions in the vacuum expectation values (VEVs) of the squared electric and magnetic fields are explicitly separated. Depending on the number of spatial dimensions and on the planar angle deficit induced by the cosmic string, these contributions can be either negative or positive. In the case of the flat bulk, the VEV of the energy-momentum tensor is evaluated as well. For the locally de Sitter bulk, the influence of the background gravitational field essentially changes the behavior of the vacuum densities at distances from the string larger than the curvature radius of the spacetime.


Introduction
The formation of topological defects is one of the interesting consequences of symmetry breaking phase transitions in the early Universe. Depending on the topology of the vacuum manifold these are domains walls, strings, monopoles and textures. Among them, cosmic strings have been of increasing interest due to the importance that they may have in cosmology [1]. This class of defects are sources of a number of interesting astrophysical effects such as the generation of gravitational waves, high-energy cosmic rays, and gamma ray bursts. Another interesting effect is the influence of cosmic strings on the temperature anisotropies of the cosmic microwave background radiation. More recently, a mechanism for the generation of the cosmic string type objects is proposed within the framework of brane inflation [2,3].
Depending on the underlying microscopic model, the cosmic strings can be either nontrivial field configurations or more fundamental objects in superstring theories. In the simplest theoretical model describing the straight cosmic strings the influence of the latter on the surrounding geometry at large distances from the core is reduced to the generation of a planar angle deficit. In quantum field theory, among the most interesting effects of the corresponding nontrivial spatial topology is the vacuum polarization. This effects have been discussed for scalar, fermion and vector fields (see, for instance, references cited in [4,5]).
In the present paper we present the results of the investigations for the influence of a cosmic string on the vacuum electromagnetic fluctuations. The vacuum expectation value (VEV) of the energymomentum tensor for the electromagnetic field around a cosmic string in D = 3 spatial dimensions has been obtained in [6,7] on the base of the Green function. For superconducting cosmic strings, assuming that the string is surrounded by a superconducting cylindrical surface, in [8] the electromagnetic energy produced in the lowest mode is evaluated. The VEVs of the squared electric and magnetic fields, and of the energy-momentum tensor for the electromagnetic field inside and outside of a conducting cylindrical shell in the cosmic string spacetime have been investigated in [9]. The corresponding VEVs, the Casimir-Polder and the Casimir forces in the geometry of two parallel conducting plates on the background of cosmic string spacetime were discussed in [10,11]. The repulsive Casimir-Polder forces acting on a polarizable microparticle in the geometry of a straight cosmic string are investigated in [12,13]. The Casimir-Polder interaction between an atom and a metallic cylindrical shell in cosmic string spacetime has been studied in [14] (see also [15]). The electromagnetic field correlators and the VEVs of the squared electric and magnetic fields around a cosmic string in background of (D + 1)dimensional locally de Sitter (dS) spacetime were evaluated in [16] (for quantum vacuum effects in the geometry of two straight parallel cosmic strings see [17] and references therein).
The organization of the paper is as follows. In the next section we present the complete set of the electromagnetic field mode functions on the bulk of a (D + 1)-dimensional generalized cosmic string geometry. In Section 3, by using these mode functions, the VEVs of the squared electric and magnetic fields are investigated. The VEV of the energy-momentum tensor is studied in Section 4. In Section 5 we consider the VEVs of the squared electric and magnetic fields, and of the vacuum energy density for a cosmic string in locally dS spacetime. The main results are summarized in Section 6.
2 Electromagnetic field modes around a cosmic string in flat spacetime In the first part of the paper we consider a quantum electromagnetic field with the vector potential A µ (x) in the background of a (D + 1)-dimensional flat spacetime, in the presence of an infinitely long straight cosmic string with the line element where z = z 3 , ..., z D , 0 ≤ φ ≤ φ 0 and the points (r, φ, z) and (r, φ + φ 0 , z) are to be identified. The geometry described by (1) is flat everywhere except the points on the axis r = 0 where one has a deltatype singularity. Though the local characteristics of the cosmic string spacetime in the region r > 0 are the same as those in flat spacetime, for φ 0 = 2π these manifolds differ globally. We are interested in the influence of nontrivial topology induced by a planar angle deficit on local characteristics of the electromagnetic vacuum. In the canonical quantization procedure we need to know a complete orthonormal set {A (β)µ , A * (β)µ } of solutions to the classical field equations ∂ ν |g|F µν = 0, where F µν is the electromagnetic field tensor, F µν = ∂ µ A ν − ∂ ν A µ , and g is the determinant of the metric tensor. Here and below the set (β) of quantum numbers specifies the mode functions. In the Coulomb gauge one has A (β)0 = 0, ∂ l ( |g|A l (β) ) = 0, l = 1, ..., D. In the problem at hand the set of quantum numbers is specified as (β) = (γ, m, k, σ). Here 0 γ < ∞ is the radial quantum number, m = 0, ±1, ±2, . . . is the azimuthal quantum number, k = (k 3 , . . . , k D ) is the momentum in the subspace z 3 , ..., z D , and σ = 1, . . . , D − 1 enumerates the polarization states. The cylindrical modes for the electromagnetic field are given by where l = 1, . . . , D, q = 2π/φ 0 , ω = γ 2 + k 2 , k 2 = D l=3 k 2 l , and J ν (x) is the Bessel function of the first kind. The scalar products are given as k · z = D l=3 k l z l and k · ǫ σ = D l=3 k l ǫ σl . For the polarization vector ǫ σ one has ǫ σ1 = ǫ σ2 = 0, σ = 2, . . . , D − 1, and the relations D l,n=3 The polarization state σ = 1 is the mode of TE type and σ = 2, . . . , D − 1 correspond to D − 2 modes of the TM type. The coefficients C (β) are determined by the normalization condition for vector fields. For a general background with the metric tensor g ik this condition is written as where ∇ µ stands for the covariant derivative and δ ββ ′ is understood as the Kronecker symbol for discrete components of the collective index β and the Dirac delta function for the continuous ones. In the problem under consideration, by using the standard integral for the product of Bessel functions, one finds for all the polarizations σ = 1, . . . , D − 1.
With a given set of mode functions (2), the VEV of any physical quantity F {A µ (x), A ν (x)} bilinear in the field is evaluated by making use of the mode-sum formula where |0 stands for the vacuum state and The expression in the right-hand side of (6) is divergent and requires a regularization with the subsequent renormalization. The regularization can be done by introducing a cutoff function or by the point splitting. A very convenient tool for studying one-loop divergences is the heat kernel expansion (for a general introduction with applications to conical spaces see [18,19]). The heat kernels of Laplacians for higher spin fields and the related asymptotic expansions on manifolds with conical singularities were studied in [20]. In what follows we will use the appoach based on the cutoff function. Compared with the point splitting it essentially simplifies the calculations of the topological contributions in the VEVs of local observables.

VEVs of the squared electric and magnetic fields
First we consider the VEV of the squared electric field. This VEV is obtained by making use of the mode-sum formula Note that the VEV of the electric field squared determines the Casimir-Polder potential between the cosmic string and a polarizable particle with a frequency-independent polarizability. We will regularize the VEV by introducing the cutoff function e −bω 2 with b > 0 (about using this kind of cutoff function in the evaluation of the Casimir energy see, for example, [21]). Substituting the mode functions and using (3), the regularized VEV is presented in the form where the prime on the summation sign means that the term m = 0 should be taken with the coefficient 1/2 and the function is introduced.
For the further transformation of the right-hand side in (9) we use the integral representation After the evaluation of the k-integrals one gets where w = b + y 2 . Next we use the integral [22] ∞ 0 dγγe −wγ 2 J qm (γr)J qm (γr ′ ) = 1 2w with r ′ = r and with I ν (x) being the modified Bessel function. The remaining integral over γ is written as By taking into account that e −wγ 2 = γ 2 ∞ w dt e −tγ 2 and using (13) one finds Substituting this into (14) we obtain with the notation u = r 2 /(2w). By taking into account (13), (16) and passing in (12) from the integration over y to the integration over u one finds For the further transformation we use the formula [10,23] where [q/2] stands for the integer part of q/2 and the prime on the summation sign means that the terms l = 0 and l = q/2 (for even values of q) should be taken with additional coefficient 1/2. In the case q = 1 the l = 0 term remains only. From here it follows that the contribution of the term l = 0 in the VEV (17) corresponds to the VEV in Minkowski spacetime in the absence of cosmic string. We will denote the corresponding regularized VEV by E 2 (0) reg . The latter is obtained from (17) taking the l = 0 term in (18) instead of the series over m: The remaining part in (17) is the contribution induced by the cosmic string (topological part). This part is finite in the limit b → 0 and the cutoff can be removed. We denote the topological part in the VEV of the squared electric field as E 2 t : Substituting (18) into (17), separating the l = 0 term and taking the limit b → 0, after the evaluation of the u-integral, for the topological contribution we find the following result with the notation where the prime means that for even values of q the term l = [q/2] should be taken with coefficient 1/2. Note that the functions (22) also appear in the coefficients of the heat kernel expansion in the background of cosmic string spacetime (see [24,25]).
In figure 1 we have plotted the functions c n (q) for different values of n. These functions are monotonically increasing positive functions of q > 1. For them one has c n (2) = 1/2 and c n (q) > c n+1 (q) for 1 < q < 2. In the region q > 2 we have c n (q) < c n+1 (q).
From (21) we conclude that the topological part in the VEV of the squared electric field is negative for D 3 and for q = 2 one gets For even values of n, the function c n (q) can be further simplified by using the recurrence scheme described in [26]. In particular, one has c 2 (q) = (q 2 − 1)/6 and By using these results one gets [9] for D = 3 and for D = 5. The topological part induced by the string is negative for q > 1. Now we consider the VEV of the squared magnetic field, given by where the summation goes over the spatial indices and F (β)ln = ∂ l A (β)n − ∂ n A (β)l . Note that for D > 3 the magentic field is not a spatial vector. With the mode functions from (2), the VEV, regularized by the cutoff function e −bω 2 , b > 0, is presented as The further evaluation is similar to that for the squared electric field and we will omit the details. The final result for the topological contribution is given by the expression with the function c n (q) from (22). For the regularized VEV in the absence of cosmic string one has B 2 (0) reg = E 2 (0) reg . For the special case q = 2, by taking into account that c n (2) = 1/2, we find Depending on q and D the VEV B 2 t can be either positive or negative. In particular, for q = 2 one has B 2 t < 0 for D = 3 and B 2 t > 0 for D 4. Simple expressions are obtained for odd values of the spatial dimension D. In particular, for D = 3, 5 one gets In D = 3 the VEVs of the squared electric and magnetic fields coincide [9]. In figure 2 we have displayed the topological contributions in the VEVs of the squared electric and magnetic fields, multiplied by r D+1 , as functions of the parameter q for different values of the spatial dimension D (the numbers near the curves). The full and dashed curves correspond to the electric and magnetic fields, respectively, and the dotted curve presents the VEVs for D = 3. Having the VEVs of the squared electric and magnetic fields we can evaluate the VEV of the Lagrangian density The quantity g µρ g νσ F µν F ρσ is the Abelian analog of the gluon condensate in quantum chromodynamics (see, for instance, [27]). Note that in a number of models (for example, string effective gravity [28,29] and models for generation of primordial magnetic fields during inflation [30]) the Lagrangian density contains terms of the form f (Φ)F µν F µν that couple the gauge field to a scalar field Φ (dilaton field in string effective gravity and inflaton in models of magnetic field generation). In these models, the appearance of the nonzero VEV F µν F µν induces a contribution to the effective potential for the field Φ. The stabilization of the dilaton field during the cosmological expansion, based on the nontrivial coupling of dilaton to other fields, has been discussed in [28]. By using (21) and (30), for the topological contribution in the VEV of the Lagrangian density one gets This VEV vanishes for D = 3 and is negative for D 4. The modification of the vacuum fluctuations for the electromagnetic field by a cosmic string gives rise to the Casimir-Polder forces acting on a neutral polarizable microparticle placed close to the string. For the general case of anisotropic polarizability the corresponding potential in the geometry of a D = 3 cosmic string has been derived in [13]. For a special case of isotropic polarizability α P (ω), the corresponding formula takes the form with the function If the dispersion of the polarizability can be neglected, one gets h(r, y) = 2α P , with α P being the static polarizability, and consequently For α P > 0 the corresponding force is repulsive.

Energy-momentum tensor
Another important local characteristic of the vacuum state is the VEV of the energy-momentum tensor. It determines the back-reaction of quantum effects on the background geometry. The VEV is evaluated by using the formula where By taking into account that C 0 0 = − E 2 and using the expression (34) for L , for the topological part in the VEV of the energy density one gets Depending on the parameters q and D, the energy density (40) can be either positive or negative. For the components of (39) corresponding to the axial stresses one gets (no summation over l = 3, . . . , D) The transformation of the second term in the right-hand side is done in a way similar to that for the squared electric field and for the axial stresses we find (no summation over l) T l l t = T 0 0 t , l = 3, . . . , D.
This relation could also be directly obtained from the Lorentz invariance of the problem with respect to the boosts along the directions z l , l = 3, . . . , D.
The off-diagonal components of the vacuum energy-momentum tensor vanish and it remains to consider the VEVs of the radial and azimuthal stresses. For the radial component of the tensor (39) one finds The evaluation of the parts corresponding to the last two terms in the square brackets in (43) is similar to that for the corresponding parts on the squared electric field. For the remaining part, by using (11), we get The integral is evaluated by using the relation and (13). The further steps are similar to that for the VEVs of the squared fields and are based on (18). In this way one finds Finally, for the component C 2 2 one has and the evaluation is similar to the for (43). For the azimuthal stress one gets As seen, one has the relation T 2 2 t = −D T 1 1 t . The VEV of the energy-momentum tensor obeys the covariant conservation equation ∇ ν T ν µ t = 0. For the geometry under consideration the latter is reduced to the single equation ∂ r r T 1 1 t = T 2 2 t . For D = 3 the vacuum energy-momentum tensor is traceless, T µ µ t = 0. For D = 3 the electromagnetic field is not conformally invariant and the trace is not zero.
For D = 3, by taking into account (24) one finds In particular, the energy density is negative for q > 1. This result was obtained in [6,7] by using the corresponding Green function. In the special case D = 5 we have (no summation over l) for l = 0, 3, . . . , D, and The energy density is positive for 1 < q < 2 and negative for q > 2. In the special case q = 2 and for general D one obtains The corresponding energy density vanishes for D = 5.
In figure 3 we have plotted the VEV of the energy density, multiplied by r D+1 , versus the parameter q for different values of the spatial dimension D (the numbers near the curves). For D 5 the energy density is positive for small values of q and is negative for large values of that parameter. For some intermediate value of q there is a maximum with positive energy density.

VEVs for cosmic string on locally dS bulk
In the second part of the paper we will be concerned about the combined effects of a cosmic string and of the background gravitational field, generated by a positive cosmological constant, on the VEVs of the squared electric and magnetic fields and on the vacuum energy density. This investigation has been recently presented in [16] based on the corresponding two-point functions for the electromagnetic field tensor. Here we follow a simpler approach based on the direct evaluation of the mode sums introducing a cutoff function. The vacuum polarization induced by a cosmic string in locally (but not globally) dS spacetime for massive scalar and fermionic fields has been investigated in [31,32,33]. Our choice of the locally dS geometry is motivated by several reasons. First of all the dS spacetime is maximally symmetric and similar to case of the flat background the problem for evaluation of the local characteristics of the electromagnetic field is exactly solvable. In addition, the dS spacetime plays an important role in modern cosmology. In most inflationary models the early expansion of the universe is quasi de Sitterian (for the effects of inflation on the cosmic strings see [34]- [37]). The corresponding accelerated expansion before the radiation dominated era naturally solves a number of problems in the standard cosmological model. The inflation also provides an attractive mechanism of producing long-wavelength electromagnetic fluctuations, originating from subhorizon-sized quantum fluctuations of the electromagnetic field stretched by the dS phase to superhorizon scales. In the post-inflationary era these long-wavelength fluctuations re-enter the horizon and can serve as seeds for cosmological magnetic fields. Related to this mechanism, the cosmological dynamics of the electromagnetic field quantum fluctuations have been discussed in large number of papers ( see [38]- [30] and references therein). More recently, the observational data on high redshift supernovae, galaxy clusters, and cosmic microwave background indicate that at the present epoch the universe is accelerating and the corresponding expansion is driven by a source the properties of which are close to a positive cosmological constant. In this case, the quasi-dS geometry is the future attractor for the universe. Though the cosmic strings produced before or during early stages of the inflationary phase are diluted by the quasi-exponential expansion, the defects can be formed near or at the end of inflation by several mechanisms (see [2] for possible observational consequences from this type of models). It is also possible to have subsequent inflationary stages, with linear defects being formed in between them [41].

Electromagnetic field modes
In terms of the conformal time coordinate τ , −∞ < τ < 0, the line element describing the geometry under consideration is given by the expression where the ranges for the spatial coordinates are the same as in (1). In the absence of cosmic string one has φ 0 = 2π and the geometry coincides with the dS one in inflationary coordinates. For the synchronous time t one has t = −α ln(|τ | /α), −∞ < t < +∞. The parameter α is related to the cosmological constant Λ by Λ = D(D − 1)/(2α 2 ). It has been argued in [42,43] where f (r s ) = 1/ 1 − r 2 s /α 2 . The line element takes the form with 0 ≤ φ ≤ φ 0 . With a new coordinate ϕ = qφ, from (55) we obtain the static line element of dS spacetime with deficit angle previously discussed in [42]. In this paper it is shown that to leading order in the gravitational coupling the effect of the vortex on dS spacetime is to create a deficit angle in the metric (55). For the coordinates corresponding to (53) and for the Bunch-Davies vacuum state the cylindrical electromagnetic modes are presented as where H (1) ν (x) is the Hankel function of the first kind and η = |τ |. Other notations in (56) are the same as in (2). For the normalization constant from (4) one finds For D = 3 the electromagnetic field is conformally invariant and the modes (56) coincide with (2).

Squared electric field
We start with the VEV of the squared electric field obtained from (8). The VEV, regularized by introducing the cutoff function e −bω 2 , is presented as where we have introduced the MacDonald function K ν (x) instead of the Hankel function, ν = D/2 − 2 and the other notations are the same as in (9). For the further transformation we use the integral representation This relation is obtained from the integral representation of the product of MacDonald functions with different arguments given in [44]. Plugging (59) into (58), the integration over k is elementary and the integral over y is expressed in terms of the function K ν (2η 2 /x). In this way one gets where w = x/4 + b. The integrals over γ are evaluated by using the formulas (13), (16) and we find Next we use the formula (18) for the series over m. The l = 0 term gives the regularized VEV in dS spacetime in the absence of the cosmic string, denoted here as E 2 reg dS . The remaining part corresponds to the contribution of the cosmic string. For points r = 0 that part is finite in the limit b → 0 and the cutoff can be removed. In this way, for the topological part E 2 t = E 2 − E 2 dS one gets [16] where E 2 dS is the renormalized VEV in the absence of the cosmic string. In (62) we have introduced the notation s l = sin(πl/q) and g E (x, y) = Note that the regularized VEV for dS bulk in the absence of cosmic string has the form As expected, this VEV diverges in the limit b → 0 and requires a renormalization. From the maximal symmetry of dS spacetime and of the Bunch-Davies vacuum state we expect that the renormalized VEV does not depend on the spacetime point and E 2 dS = const · α −D−1 . In (62), the topological part depends on the coordinates r and η in the form of the ratio r/η. The latter is the proper distance from the string, αr/η, measured in units of the dS curvature scale α.
For odd values of D the function g E (x, y) in (62) is expressed in terms of the elementary functions. In particular, one finds For D = 3 the electromagnetic field is conformally invariant and the topological contribution is related to the one for the flat bulk by standard conformal relation. It is of interest to note that a similar relation takes place for D = 5 as well. For other values of D there is no such a simple relation. For points near the string, assuming that r/η ≪ 1, the contribution of the large u is dominant in (63). By using the corresponding asymptotic expression for the MacDonald function, to the leading order we get is topological contribution in the flat bulk and is given by (21). Near the string the main contribution to the VEVs comes from the fluctuations with wavelengths smaller than the curvature radius and the influence of the background gravitational field on the corresponding modes is weak.
At proper distances from the string larger than the dS curvature radius one has r/η ≫ 1. Now, the contribution from the region near the lower limit of the integration in (63) is dominant. For D 5, to the leading order, the topological part is expressed in terms of c 4 (q) and c 6 (q): In the special case D = 4 from (62) we get E 2 t ≈ − q 2 − 1 ln(r/η) 630π 2 α 5 (r/η) 6 (2q 4 + 23q 2 + 191).
For D = 3 one has the behavior given by (65). At large distances, the total VEV is dominated by the part E 2 dS . As seen, in spatial dimensions D = 4, 6, 7, . . ., at distances larger than the curvature radius, the influence of the gravitational field on the topological part is essential. From (66) and (67) it follows that at large distances E 2 t < 0 for D = 4, 5, 6, and E 2 t > 0 for D 7. By taking into account that near the string one has E 2 t < 0 for D 3 we conclude that in spatial dimensions D 7 the topological contribution E 2 t has a positive maximum for some intermediate value of r/η.

Squared magnetic field
By using the mode functions (56), from the mode-sum formula (27) one gets the following representation for the squared magnetic field Further transformation of this VEV is similar to that for the electric field squared. The final formula for the topological contribution B 2 t = B 2 − B 2 dS is given by [16] with the function We denote by B 2 dS the renormalized VEV of the squared magnetic field in dS spacetime in the absence of the cosmic string. The regularized VEV of the squared magnetic field for the latter geometry is given by For D = 3 this result coincides with that for the squared electric field. Note that for D = 4 and q = 3 the topological part vanishes, B 2 t = 0. For odd values of the spatial dimension D the integral in (70) is expressed in terms of the elementary functions. For D = 3 one has B 2 t = E 2 t and for D = 5 we get Note that, unlike to the case of the electric field, the VEV of the squared magnetic field for D = 5 does not coincide with the corresponding VEV in the flat bulk with the distance r replaced by the proper distance αr/η. For points near the string, r/η ≪ 1, the influence of the gravitational field on the topological contribution is weak and to the leading order one has the relation B 2 t ≈ (η/α) D+1 B 2 (M) t , where the VEV B 2 (M) t is given by the expression (30). The influence of the gravitational field is essential at proper distances from the string larger than the curvature radius of dS spacetime. In the asymptotic region r/η ≫ 1 for the leading terms in the expansions of the topological parts one has Note that for D = 4 at large distances one has E 2 t / B 2 t ∝ ln(r/η), whereas for D 5 one has E 2 t / B 2 t ∝ (r/η) −2 and the topological part in the VEV of the squared magnetic field is much larger than the one for the electric field. For D 5 the topological part B 2 t is positive at large distances.
In figure 4 we have displayed the dependence of the VEVs for squared electric (full curves) and magnetic (dashed curves) fields on the ratio r/η (proper distance from the string in units of the dS curvature scale α) for separate values of the spatial dimension D = 3, 4, 5. For D = 3 the VEVs for the electric and magnetic fields coincide. The graphs are plotted for q = 1.5.

VEV of the energy density
The VEV of the energy density is given by T 0 0 = E 2 + B 2 /8π and is decomposed as T 0 0 = T 0 0 dS + T 0 0 t , where T ν µ dS = const · δ ν µ is the VEV in dS spacetime in the absence of the cosmic string. For the topological contribution one gets the expression with the function Near the string, r/η ≪ 1, to the leading order, one has T 0 0 t ≈ (η/α) D+1 T 0 0 (M) t with the energy density in the flat spacetime from (40). At large distances from the string one has the asymptotic expressions In this asymptotic region the vacuum energy density is dominated by the part T 0 0 dS . The topological contribution is negative for D = 4 and positive for D 5. Figure 5 presents the energy density versus r/η for different values of the spatial dimension D = 3, 4, 5.
One of the interesting effects during the dS expansion, playing an important role in inflationary cosmology, is the so-called classicalization of quantum fluctuations: the evolution of quantum fluctuations into classical fluctuations. In particular, the latter for the inflaton field are expected to be the seeds of large scale structures in the universe. In a similar way, the classicalization of the electromagnetic fluctuations may give rise to large scale magnetic fields (for various types of mechanisms for the generation of cosmological magnetic fields see, for instance, [30,38,39,40]). The discussion we have presented above shows that these fields will be influenced by cosmic strings formed at late stages of the inflationary phase.

Conclusion
We have investigated the influence of a straight cosmic string on the local characteristics of the electromagnetic vacuum. First we have considered a cosmic string on flat spacetime and then the corresponding results are generalized for the locally dS background geometry. A simplified model is used where the effect of the cosmic string on the background geometry is reduced to the generation of a planar angle deficit. In this model, for points outside the core the local geometry is not changed by the cosmic string, but the global properties are different. The corresponding nontrivial topology gives rise to shifts in the VEVs of physical observables. For the investigation of the topological contributions we have employed the direct summation over the complete set of electromagnetic modes. For a cosmic string on (D + 1)-dimensional flat spacetime the complete set of modes for the vector potential is given by (2), where σ enumerates the polarization states. For the regularization of the mode sums in the VEVs of squared electric and magnetic fields the cutoff function e −bω 2 is introduced. The application of the formula (18) for the summation over the azimuthal quantum number allowed us to extract explicitly the parts in the VEVs corresponding to the Minkwoski spacetime in the absence of the cosmic string. For points away from the string core the remaining topological contributions are finite in the limit b → 0 and the cutoff can be safely removed. These contributions for the electric and magnetic fields are given by the expressions (21) and (30), where the function c n (q) depending on the planar angle deficit is defined by (22). In spatial dimensions D 3 the topological part in the VEV of the squared electric field is negative whereas, depending on q and D, the corresponding part for the magnetic field can be either negative or positive. For odd values of D, the functions c n (q) in the expressions for the topological contributions are polynomials in q and the VEVs are further simplified. In the special case D = 3 the electromagnetic field is conformally invariant and the topological contributions for the electric and magnetic fields coincide.
Another important characteristic of the vacuum state that determines the back-reaction of quantum effects on the background geometry is the VEV of the energy-momentum tensor. For a cosmic string on flat bulk this VEV is diagonal. Due to the Lorentz invariance with respect to the boosts along directions z l , l = 3, . . . , D, the topological contributions in the corresponding stresses coincide with the energy density, given by (40). The radial and azimuthal stresses are given by the expressions (46) and (48). They are related by a simple relation T 2 2 t = −D T 1 1 t that is a direct consequence of the covariant conservation equation for the VEV of the energy-momentum tensor. The general expressions are simplified for an odd number od spatial dimension. In particular, for D = 3, 5 one gets the representations (49)-(51). Depending on the planar angle deficit and the spatial dimension, the corresponding energy density can be either negative or positive.
For a string in locally dS spacetime the electromagnetic mode functions, realizing the Bunch-Davies vacuum state, are presented as (56). The topological contributions in the VEVs of the squared electric and magnetic fields are given by the formulas (62) and (69) with the functions (63), (70). The corresponding energy density is obtained by summing the contributions of the electric and magnetic parts. For points near the string the dominant contribution to the VEVs come from the fluctuations with small wavelengths and the influence of the gravitational field is weak. In this region, the leading terms in the VEVs coincide with those for flat spacetime with the distance from the string replaced by the proper distance. The influence of the gravitational field is essential at proper distances larger than the curvature radius of dS spacetime. For D = 4 the topological contributions in the VEVs decay as (r/η) −6 ln(r/η) for the squared electric field and like (r/η) −6 for the squared magnetic field. In this case the corresponding energy density is dominated by the electrical part and is negative. For D > 4 the topological contributions decay as (r/η) −6 in the case of the electric field squared and as (r/η) −4 for the magnetic field squared. The topological term in the vacuum energy density is dominated by the magnetic part and is positive. This behavior is in clear contrast to the problem on flat spacetime where the energy density decays like r −D−1 .