Unruh effect universality: emergent conical geometry from density operator

The Unruh effect has been investigated from the point of view of the quantum statistical Zubarev density operator in space with the Minkowski metric. Quantum corrections of the fourth order in acceleration to the energy-momentum tensor of real and complex scalar fields, and Dirac field are calculated. Both massless and massive fields are considered. The method for regularization of discovered infrared divergences for scalar fields is proposed. The calculated corrections make it possible to substantiate the Unruh effect from the point of view of the statistical approach, and to explicitly show its universality for various quantum field theories of massless and massive fields. The obtained results exactly coincide with the ones obtained earlier by calculation of the vacuum average of energy-momentum tensor in a space with a conical singularity. Thus, the duality of two methods for describing an accelerated medium is substantiated. One may also speak about the emergence of geometry with conical singularity from thermodynamics. In particular, the polynomiality of the energy-momentum tensor and the absence of higher-order corrections in acceleration can be explicitly demonstrated.

A remarkable observation is that these effects allow to show the duality of various theoretical approaches. An example is the CVE, which can be obtained in the framework of different statistical approaches [17][18][19][20][21], using the hydrodynamic approach with the quantum axial anomaly [2], in the framework of an effective field theory [4], on the basis of the gravitational anomaly [5]. Another example is the chiral magnetic effect [4,22].
In this paper, we focus on another well-known effect related to the motion of a medium such as the Unruh effect [6]. According to this effect, the accelerated observer perceives the Minkowski vacuum as a medium with a temperature T U , proportional to the acceleration modulus |a| This temperature is known as Unruh temperature.
In recent years, a fundamental theoretical approach has been developed that allows one to study the effects associated with acceleration. It is based on the Zubarev quantum statistical density operator [17,18,[23][24][25][26]. Acceleration-related effects can be obtained by calculating quantum corrections to the mean values of the observed quantities in the inertial system described by the Minkowski metric. Thus, in particular, corrections up to the fourth order in acceleration to the energy-momentum tensor of Dirac field [16,27], as up to the second order for scalar field [17,18,26] were calculated.
The mean values calculated in this way correspond to the normalization at which the contribution corresponding to the Minkowski vacuum is subtracted. Thus, it becomes possible to verify the Unruh effect from the point of view of quantum statistical mechanics. Indeed, this effect should lead to a situation where the mean values vanish at the proper temperature equal to the Unruh temperature: so the Minkowski vacuum corresponds to an accelerated medium with Unruh temperature [28][29][30][31].
Some results in this direction have already been obtained: in particular, the Unruh effect in this way was shown for the massless Dirac field [16,27], for which it was necessary to calculate fourth-order corrections in acceleration. In addition, a new effect was discovered related to the instability at Unruh temperature [16,28].
In this paper, we test the statement about the Unruh effect in a statistical approach for a wider class of theories and show that it is general. We calculated the corrections to the energy-momentum tensor of the real and complex free massless scalar fields, as well as the quadratic mass corrections for scalar and Dirac fields. We show that in all investigated cases the calculated coefficients exactly satisfy the condition of vanishing at Unruh temperature. Thus, we conclude that the effect previously shown in [27] is universal.
Despite the fact that the final conclusion about the Unruh effect is the same for fermions and scalar fields, the quantum corrections themselves have a different structure. If for fermions the fourth-order terms turned out to be finite, then for scalar fields these terms contain infrared divergences. We show that the appearance of infrared divergences in higher orders of perturbation theory follows from the general structure of the correlator, related to the coefficient of the n-th order. We discuss the connection of infrared divergences with Matsubara zero modes and substantiate the procedure for their regularization.
An amazing observation that we make is the emergence of conical geometry in the Zubarev statistical approach. This conclusion is based on the fact that the calculated quantum corrections exactly correspond to the results obtained in the framework of quantum field theory in a space with a conical singularity [29,30,[32][33][34][35]. The emergence of conical geometry in the statistical approach was first noted by us and discussed in the case of massless fermions in [16]. In this paper, we show that this is a general phenomenon, which is also true for massless scalar fields and for massive scalar and Dirac fields.
In particular, this duality of two approaches to describing the thermodynamics of an accelerated medium -statistical one, with the Zubarev operator, and geometrical approach with a conical singularity -allows one to obtain effects for an accelerated medium from the point of view of an inertial observer, using the available results for cosmic strings and vice versa [30].
The revealed duality also allows us to make a number of valuable statements regarding the statistical approach. First, in the conical singularity approach, the polynomiality of the energy-momentum tensor and the absence of higher-order corrections in acceleration can be explicitly demonstrated. Accordingly, we predict, on the basis of the duality, the absence of such corrections in the statistical approach. We have verified this statement directly in a particular case when calculating acceleration corrections for massive fields.
In addition, we get additional confirmation of the possibility of using the method of regularization of infrared divergences.
The paper has the following structure. In Section II, we discuss the possibility of describing an accelerated medium from the point of view of two different approaches, statistical and geometrical, based on field theory in conical space, and also discuss some aspects related to the discovered duality between them. Section III provides calculation of quantum corrections of the fourth-order in acceleration to energy-momentum tensor of real scalar field in the massless case and in the quadratic order in mass. It is shown that when calculating acceleration corrections, infrared divergences arise and the procedure for their regularization is described. In the Section IV we give similar results for complex scalar field. Section V contains earlier results for massless fermions, as well as the calculation of quadratic mass corrections for massive Dirac field. Section VI discusses the emergence of conical geometry in the Zubarev statistical approach. In the Section VII we establish the need for perturbative consideration of the effects of mass. Section VIII is devoted to various aspects of infrared divergences: their relationship with Matsubara zero modes, the need for summation in the massive case and the possibility of subtraction in the massless one. In the Section IX generalizing remarks about the observed universality of the Unruh effect in the statistical approach are made, and the consequences from the duality are discussed. In the Section X conclusions are given.

II. OVERVIEW OF THE DUALITY BETWEEN QUANTUM-STATISTICAL AND FIELD-THEORETICAL APPROACHES
There exist two different approaches to evaluate various matrix elements, in equilibrium as functions of temperature T , chemical potential µ, vorticity ω µ , acceleration a µ . In the first approach the central role is played by Zubarev density operatorρ [17,23,24] where β µ = u µ /T and u µ is the 4-velocity of an element of the medium,P µ is the operator of the 4-momentum,Ĵ µν x are the generators of the Lorentz transformations, shifted by vector x µ ,Q is the charge operator conjugated with the chemical potantial µ. Moreover denotes the thermal vorticity. In the hydrodynamic setup, the operatorĴ µν and tensor ̟ µν in Eq. (2.1) can be decomposed aŝ whereK µ is the boost operator andĴ µ is the angular momentum, and vectors w µ and α µ are related to the usual vorticity and acceleration by the relations w µ = ω µ /T and α µ = a µ /T in the state of global equilibrium. Note that in many cases, see, e.g., textbook [36] the term containing the boost operator is not included into the density operatorρ. The main advantage and motivation to still use Eq. (2.1) is that it is explicitly Lorentz-covariant, see, in particular [28]. Note that inclusion of the boost operator makes explicit calculations of the statistical averages much more involved since the boost operator does not commute with the Hamiltonian.
Statistically averaged matrix elements can be calculated perturbatively, by expanding the density operator in a µ , ω µ and are expressed through the integrals over the momentum d 3 p with the weight function representing the Bose or Fermi distribution, depending on the spin of the fields. In this way one evaluates one-loop effects perturbatively within the statistical approach. It is worth emphasizing that the expansion in acceleration of the equilibrium matrix elements is a novel technique elaborated only recently [28]. The most advanced explicit example of such calculations at the moment is provided by the evaluation of terms of fourth order in acceleration in expansion of the energy-momentum tensor [37].
The other approach can be called geometrical, or field theoretical. It has been elaborated not in all the generality but only in some particular cases. The most interesting case is µ, ω = 0, a = 0. It is well known that for an accelerated observer there exists a horizon. In other words, the relevant space-time has a boundary. In the Euclidean version, the temperature also acquires a geometrical meaning. Namely, the Euclidean time coordinate is compact and the length of the corresponding circle is the inverse temperature. Qualitatively, these simple observations alone allow for a geometrical treatment of the effects of acceleration, Quantitatively, to accommodate temperature and acceleration as independent parameters one considers the Rindler space with a conical singularity. Introduce first Rindler space with Minkowskian signature where η = γλ, x = r cosh η, t = r sinh η, dx 2 ⊥ = dy 2 + dz 2 and γ = const. The proper acceleration |a| = √ −a µ a µ and the proper time of accelerated observer can be expressed in terms of the variables λ and r |a| = r −1 , τ = γrλ . (2.5) At finite temperature, the proper time τ is to be made imaginary and periodic in the inverse proper temperature T −1 . Thus, the metric (2.5) takes the form The space (2.6) describes a flat two-dimensional cone with angular deficit 2π − |a|/T (plus a factorized transverse 2d Euclidean space). Further details (and a picture) can be found in [16]. Now, by expanding in modes one can evaluate energy density ρ ≡< T 0 0 > associated with various quantum fields living on the space (2.6) . For massless particles of spin 1/2 the result is [30] where ν = 2πT r. Since r = 1/|a|, Eq. (2.7) allows to unambiguously fix the energy density, associated with quantum massless field of spin 1/2 as function of temperature and acceleration. Thus, knowing the Eq. (2.7) one could have predicted in advance the corresponding statistical one-loop average of the operatorT 0 0 evaluated along the lines discussed above. There is a word of caution, however. There are two different field theories behind derivation of Eq (2.7) and the statistical perturbation theory. Any field-theoretic calculation might suffer uncertainties due to divergences. Moreover, Eq. (2.7) is derived within so to say fundamental field theory (on a nontrivial manifold) which is valid in ultraviolet. The statistical perturbation theory deals with effective interaction introduced within thermodynamical approach rather on a macroscopical scale, or in the infrared. Thus, the structure of divergences (if any) could be very different. Moreover, there are specific features of the two theories which might make the comparison of the results difficult. In particular, the first term in the r.h.s. of Eq. (2.7) represents the pure thermal energy, and is fixed by the Stephan-Boltzmann law. However, the last term in the r.h.s. of Eq. (2.7) represents the pure quantum Casimir effect due to existence of the boundary, or horizon on the Rindler space. The statistical approach weighs all the types of energy with the 1/T factor and, in this sense, deals with various types of thermal contributions.
Within the statistical approach ρ s=1/2 (a, T ) has been evaluated perturbatively, see [16] and references therein, up to the fourth order in acceleration. The result coincides with (2.7) exactly. Since the statistical approach is formulated in Minkowski space and reproduces the Casimir energy due to the Rindler horizon, one could even talk about the horizon as an emergent notion.
In any case, duality in description of ρ s=1/2 (a, T ) has been established without any adjustment of parameters, or else. Within the statistical approach the equilibrium energy is understood as energy of real particles in the state with maximal entropy. While within the field-theoretic approach the energy is a sum of the lowest energy levels of quantum oscillators, (1/2)ω n , and is associated with virtual particles living on a non-trivial manifold.
Although the coincidence of the results is impressive by itself, there are a few subtle points to be mentioned. First, turn to the structure of divergences. The original expression for the Rindler vacuum energy (2.7) is ultraviolet divergent and it is rendered finite by subtracting the Minkowski expression, see [30]. Since the Minkowski vacuum is characterized by T U = |a|/2π one can say that the vanishing of the r.h.s. of Eq (2.7) at the Unruh temperature is imposed through a subtraction. There is no need for such a subtraction in case of the statistical approach, see [37].
It is worth also emphasizing that the Eq. (2.7) is valid only at T ≥ T U . This is obvious in the geometric language, since the angular deficit cannot be negative. On the other hand, if one concentrates on the statistical perturbation theory in Minkowski space there is no such a limitation. Moreover, we are confronted with another question. Namely, Eq. (2.7) makes it explicit that there are only three terms, of order |a| 0 , |a| 2 , |a| 4 in the expression for the Rindler vacuum energy. Explicit evaluation of such terms within the statistical perturbation theory does reproduce Eq. (2.7), for details see [37] and references therein. It remains unclear, however, why higher terms in the ratio |a| 2 /T 2 are not in fact present.
Both problems have been resolved through working out a non-perturbative expression for ρ s=1/2 within the statistical approach. Namely, the following integral representation was proposed for ρ s=1/2 in the massless case [27] Eq. (2.8) is motivated on theoretical grounds and goes through a number of non-trivial checks, for details see [27] and references therein. In particular, expansion of (2.8) in the acceleration |a| is exhausted by the first three terms and coincides with (2.7), once the latter equation is rewritten in terms of |a| and T . Also, the representation (2.8) reveals nonanalyticity at the Unruh temperature, T U = |a|/2π which cannot be detected perturbatively. Moreover, Eg (2.8) suggests an analytical continuation to T < T U and, in this respect, is more informative than Eq. (2.7), for details see [16].
To summarize, the statistical perturbation theory and field theory on non-trivial manifolds provide in case of massless fermions dual descriptions which are rather complementary to each other and allow for novel applications. In this paper we explore the possibility of extending these results to scalar fields and massive Dirac fields.

A. Massless real scalar field
In the case of a medium with acceleration, the density operator (2.1) contains a term with acceleration and a boost operator Using (3.1), corrections related to acceleration to the energy-momentum tensor can be calculated. From symmetry considerations it follows that in the fourth order of the perturbation theory the energy-momentum tensor has the form The purpose of this section is to calculate quantum corrections in acceleration to the mean value of energy-momentum tensor of free scalar field. The energy-momentum tensor of a free real scalar field has the well-known operator form In this subsection, we will consider the case of massless fields m = 0. The coefficients ρ 0 and p 0 correspond to standard formulas for the energy density and pressure of gas of massless bosons (they can also be found directly using (3.1)) Coefficients A n are to be found on the basis of (3.1). In [17,26], the second-order coefficients in acceleration A 1 , A 3 , A 5 were calculated where the index 0 means that we are considering the case of m = 0. However, in the second order, the condition necessary to justify the Unruh effect was not fulfilled. One can easily check using (3.4) and (3.5), that T µν (T = T U ) = 0. Therefore, higher order corrections must be calculated. We proceed to calculate the coefficients A 2 , A 4 , A 6 . The general algorithm of calculation of the hydrodynamic coefficients on the basis of (3.1) is described in [17,21,26], and in the case of fourth-order corrections, in [27,37]. To find the coefficients A 2 , A 4 , A 6 , it is necessary to expand Eq. (3.1) in the series of the perturbation theory in the acceleration and calculate quantum correlators with boost operators and operator of the quantity under study. Rewriting the boost operator through the energy-momentum tensor, we will need to calculate five-point quantum correlators of the form The index β(x), c means that mean value is to be defined using the operator (3.1) with α µ = 0 and that only connected correlators are taken into account, T τ means ordering by inverse temperature, and |β| = 1 T . The coefficients in (3.2) are expressed in terms of (3.6) as follows We present the result of calculation for the coefficient A 2 in integral form where n (k) B (p) = d k dp k 1 e p/t −1 is the derivative of the Bose-Einstein distribution. An essential property of (3.8) is the appearance of infrared divergence in the limit |p| → 0. The appearance of this infrared divergence is a direct consequence of the Bose distribution pole for p → 0 in (3.8). It turns out that if we extract this divergence as a term of the Laurent series with negative power of the momentum, then the infinite integral (3.8) can be represented as the sum of the finite contribution and the divergent integral of the form d|p|/|p| 2 .
A similar situation will be for the other coefficients in (3.2). We write out the final expressions for the coefficients, representing them as the sum of the finite and diverging contributions (3.9) A standard technique in quantum theory of massless fields is to equate separately appearing divergent integrals of the form d|p|/|p| 2 to zero, which is associated with the absence of a dimensional parameter in the integral [38][39][40]. This statement is known as Veltman's formula. Now we will follow this rule, while in the Section VIII we give a more detailed and rigorous justification.
Subtracting the divergences in (3.9) and taking into account the coefficients (3.4) and (3.5), we obtain the next expression for the energy-momentum tensor One can easily check that T µν 0 real vanishes at the Unruh temperature The fulfilment of condition (3.11) is a direct indication of the Unruh effect: the Minkowski vacuum corresponds to the proper temperature equal to the Unruh temperature.

B. Massive real scalar field
Mass corrections can be calculated using the same algorithm used in massless theory. Mass effects are contained in the energy-momentum tensor itself (3.3), as well as in propagators [17]. The terms of the order m 2 T 2 can be obtained from the standard formulas for ρ 0 and p 0 , which describe the energy density and pressure of static gas of massive bosons. The corresponding standard formulas can also easily be calculated using the Zubarev density operator, and in this case it will be necessary to subtract the standard ultraviolet-diverging vacuum contribution. The finite parts will have the form where E p = m 2 + |p| 2 . In the order m 2 we obtain, in particular, for ρ 0 The integral in (3.13) converges and we obtain (similarly for p 0 ) (3.14) Corrections of the order m 2 |a| 2 can be obtained on the basis of the formulas [26] or [17]. In general case of m = 0 coefficients A 1 , A 3 , A 5 are We note, however, that we did not find these formulas for real scalar fields in the form (3.15) in the literature. Exactly the same formulas, but with a factor 2, are given in [17] for complex scalar fields. Despite the fact that it is obvious in advance that the result for a real scalar field will be two times smaller, we derived (3.15) directly from the density operator with a scalar field, following the algorithm [17].
Corrections of the order m 2 can be obtained in the same way as above, by expanding the integrands in (3.15) in a series in mass. In particular, for the coefficient A 1 we get As in the previous section, when calculating the terms |a| 4 , the integral (3.16) contains the infrared divergence of the form 1/|p| 2 . We isolate this divergence as a separate term. Then the coefficient A m2 1 will be presented as a combination of a finite term and a divergent integral. A similar situation is realized for the remaining coefficients in (3.15). As a result, we obtain (3.17) The terms of the order m 2 |a| 4 /T 2 can be calculated on the basis of the formulas (3.7) and (3.6), where it is necessary to keep the mass in the propagators and the energy-momentum tensor. Moreover, we find that these terms contain only infrared divergences, and the finite contribution in all coefficients is zero.
Accordingly, in the order m 2 we obtain (we keep the divergences that appeared earlier) Acting in the same way as in the case of infrared divergences in (3.9) and (3.17), we cancel the divergences d|p|/|p| 2 and d|p|/|p| 4 in (3.18). However, as will be shown in the Section VIII, the situation in the massive case becomes more non-trivial compared to the massless one. In contrast to the massless case, it is now necessary to sum up the complete series of divergences d|p|/|p| 2n in all orders in mass. However, the result of such a summation does not contribute to the corrections of the order of m 0 and m 2 , and therefore, effectively these divergences can be subtracted from the terms considered by us now. As a result, taking into account (3.14), (3.17) and (3.18) we obtain the following expression for the corrections of the order m 2 to the energy-momentum tensor 20) and thus, the condition necessary for the Unruh effect is also satisfied in the order m 2 .

IV. COMPLEX SCALAR FIELD
A. Massless complex scalar field We will consider complex scalar fields with zero chemical potential µ = 0. The results obtained in this case are predictably the same as for the real scalar field, and differ only by a factor of 2, which is associated with a double number of degrees of freedom. However, at the technical level, the two cases are a bit different, which, in particular, is due to the fact that in the case of complex scalar field there is an additional conjugate field. This simplifies the application of Wick theorem and from a technical point of view, calculations in the case of complex scalar fields turn out to be less complicated.
We start with the following standard expression for the energy-momentum tensor of complex scalar fieldŝ Calculating the corrections according to the algorithm described in the previous section, we find that all the coefficients for complex scalar fields are described exactly by the formulas (3.4), (3.5) and (3.9), but with an additional coefficient of 2. And as a result, we get a 2 times larger value for the mean value of energy-momentum tensor Thus, the Unruh effect is also observed statistically for massless complex scalar fields.

B. Massive complex scalar field
In the case of massive complex scalar fields, acceleration corrections can be calculated based on the formulas (3.6) and (3.7) and the formulas from [17], in exactly the same way as it was done in the previous section for real scalar fields. As a result, the mass corrections are described by the same formulas as for the real scalar fields (3.14), (3.17) and (3.18), but with an additional coefficient of 2. The final result for the corrections of the order m 2 to the mean value of the energy-momentum tensor is the doubled real scalar one Thus, massive complex scalar field also satisfies the condition associated with the Unruh effect.

A. Massless Dirac field
In this section, for completeness, we present the results for massless fermions obtained in [27]. The calculation of the coefficients (3.2) for fermions can be done on the basis of the formulas (3.6) and (3.7), where it is necessary to use the energy-momentum tensor of fermions. As a result, we obtain the following coefficients where the second-order coefficients A 1 , A 3 , A 5 were calculated in [17]. The energy-momentum tensor takes the form Unlike scalar fields (3.9), the energy-momentum tensor of fermions is free from infrared divergences. This situation corresponds to the fact that in the Fermi-Dirac distribution, in contrast to the Bose distribution, there is no singularity at zero energy.
It is easy to see that the Unruh effect is statistically fulfilled

B. Massive Dirac field
Coefficients of the order m 2 can be calculated in the same way as previously. As a result, we obtain where the coefficients ρ m2 0 , p m2 0 are calculated by expanding the standard formulas for the energy and pressure of the static gas of massive fermions. The coefficients A m2 1 , A m2 3 , A m2 5 are calculated by expanding in mass the formulas from [17], while the coefficients A m2 2 , A m2 4 , A m2 6 can be obtained based on the formulas (3.6) and (3.7), by holding the mass in the propagators and the energy-momentum tensor (complete formulas are not given because of their too large size). Taking into account (5.4), we obtain the next expression for the mean value of the energy-momentum tensor of Dirac field in the order m 2 where T µν 0 fermi corresponds to massless case (5.2). It is easy to see that the energymomentum tensor (5.5) satisfies the condition resulting from the Unruh effect According to (5.4), when calculating corrections with acceleration in the hydrodynamic coefficients of massive fermions, there are no divergences and all terms are finite. The same situation was in the case of massless fermions. It is also important to note that the terms of higher order m 2 |a| 4 /T 2 , as can be seen from the formulas for A m2 2 , A m2 4 , A m2 6 , are equal to zero.

VI. THE EMERGENCE OF CONICAL GEOMETRY IN THE ZUBAREV STA-TISTICAL APPROACH
It turns out that all the formulas (3.10), (3.20), (4.2), (4.3), (5.2), (5.5), calculated in the framework of the perturbation theory following from the Zubarev density operator (3.1) in an ordinary flat Minkowski space, can be obtained in another approach based on the consideration of a space with a conical singularity [29,30,[32][33][34][35]. This allows us to talk about the emergent conical geometry in the statistical approach of Zubarev or about the duality of the two approaches. The first indications of such duality were noted by us in [16], and now we will show it at a more general level. Now, to consider the medium with acceleration, we move into space-time with an event horizon described by the Rindler metric (2.4), which at finite temperature takes the form (2.6). As noticed in the Section II, the space, described by (2.6) contains a flat twodimensional cone with an angular deficit 2π − |a|/T . One of the important properties of the space (2.6) is the presence of a conical singularity at r = 0. We note in this case that despite the fact that the acceleration depends on the coordinate as |a| = 1/r, the angular deficit is constant, since T ∼ 1/r, and |a|/T = const, which is a consequence of global thermodynamic equilibrium [17].
In the papers [29,30,[32][33][34][35] a quantum field theory in space-time of a cosmic string was considered. This space-time is equivalent to the Euclidean Rindler space-time (2.6) up to change of the numbering of coordinates [30]. In particular, the energy density in space-time (2.6) turns out to be equal to the vacuum average of the component T 2 2 of the energymomentum tensor in space-time of the cosmic string: ρ Rindler = T 2 2 string . In [29,30,[32][33][34][35] the expressions for the T 2 2 of massless real scalar field (s = 0) and fermion field (s = 1/2) are given where ν defines the period 2π/ν of the angular coordinate for the space-time of the cosmic string. For ν = 1, the conical singularity disappears. In order to move to space (2.6), it is necessary to replace ν = 2πT r and take into account the relation ρ Rindler = T 2 2 string . As a result, we get Taking into account (2.5) we get exactly the energy density from (3.10) and (5.2) In [33,34] the results of calculation of quantum corrections with quadratic mass corrections for real scalar fields are given which, taking into account the comments made earlier, leads to energy density in space (2.6) This formula exactly coincides with the expression for energy density, following from (5.5).
In [35] the case of massive fermions in a space of cosmic string is considered. However, we did not find a derivation of corrections of the order m 2 from the general formula given in [35]. Further we present such a calculation. According to [35] and taking into account the correspondence between the Rindler metric and the metric with a cosmic string, the energy density of fermions with mass m is described by the formula where T 0 and T 1 are of the form where K 1 and K 2 are the modified Bessel functions of the second kind. We expand the functions in (6.7) in a series in mass up to the order of m 2 . Then the energy density will take the form ρ m2 s=1/2 = I 0 + m 2 I 1 , (6.8) where the integrals I 0 and I 1 are of the form The integrals (6.9), can be found and, thus, the energy density for fermions in the order m 2 takes the following form The formula (6.11) exactly matches the result from the Zubarev operator (5.5). Summarizing, despite the difference between the two methods, statistical (with Zubarev operator) and geometrical (either in Euclidean Rindler space-time or space-time of cosmic string), both at the ideological and technical levels, it is striking that both methods lead to exactly the same results: formulas (3.10), (3.20), (5.2), (5.5) exactly coincide to (6.3), (6.5) and (6.11).
Thus, we should talk about the emergent conical geometry in the statistical approach of Zubarev or about the duality of the two methods. The first method is statistical; all calculations are carried out in a flat space described by the Minkowski metric. This method "knows nothing" about curvilinear coordinates, but nevertheless leads to relations directly following from the Unruh effect: the coefficients turn out to be precisely such that the Minkowski vacuum corresponds to a proper temperature equal to Unruh temperature. The second method considers space with a boundary, an event horizon, which then transforms into space with a conical singularity. In this method, it is obvious in advance that all observables vanish at the Unruh temperature, since even at the level of the Green function, subtraction was performed at the Unruh temperature. In this sense, the first approach is an independent verification of the Unruh effect, while the second considers it as the initial premise.

VII. BEYOND EXPANSION IN MASS: THE NEED FOR PERTURBATIVE CON-SIDERATION
After reading Sections III B, IV B and V B, the question may arise -is it possible to evaluate the Unruh effect without using mass expansion? Indeed, the coefficients of |a| 2 and |a| 4 terms can be found outside the expansion in mass, by accounting mass in propagators. We confine ourselves to considering the energy density of massive fermions 1 .
In the zero order in acceleration, the energy density of Dirac fields is well known Coefficient A 1 (m, T ) of |a| 2 term is described by the formula (5.30) in [17]. Coefficient A 2 (m, T ) was found in [37] and has the form F (E p ) 2) (formula (7.2) is equivalent to that given in [37]). As a result, we can check what the energy density is at Unruh temperature for an arbitrary mass, without using mass expansion 3) The graph of (7.3) is shown in Fig.1. As might be expected, for small masses ρ(m, T U ) ≈ 0, however, for larger masses this condition is violated. This fact should not be surprising -in fact, in formula (7.3) we have taken into account only terms up to the order |a| 4 . Section IX gives arguments in favor of the absence of corrections to (7.3), but only in the case of a mass equal to zero or in the corrections m 2 . In general case, such a correction arises and should be taken into account when considering the Unruh effect. There is no doubt that in the general case the energy density should turn to zero at the Unruh temperature, since the Unruh effect is a universal phenomenon (look, in particular, (6.9)). Given the comments made, the mass expansion used in the previous sections is seen as a suitable way of analyzing the Unruh effect in massive theories.

VIII. INFRARED DIVERGENCES: SUMMATION, ZERO MODES, NONPER-TURBATIVE TERMS
In this section, we discuss in more detail the infrared divergences that appeared in the Sections III, IV. The infrared divergences arose for both massless (3.9) and massive scalar fields (3.17), (3.18). We first consider the case with massless fields and restrict ourselves to the consideration of divergences in the energy density (the conclusions made below are to be valid for other divergences in the energy-momentum tensor).
First, it can be shown from the general structure of the perturbation theory that in 2n-th order in acceleration, a leading infrared divergence of the form d|p|/|p| 2n−2 arises, unless the coefficient at it turns out to be zero. Indeed, the contribution to the energy density of a massless real scalar fields in the 2n-th order in acceleration can be schematically represented in the form [17,37] ρ ∼ A n |a| 2n ∼ |a| 2n where ∆(P ) = 1/(P 2 + m 2 ) is the scalar thermal Green function, px denotes a linear combination of scalar products of the form p i x j , τ ω denotes a linear combination of products of the form τ i ω j , and D 00 i denotes D 00 (±iP i ′ , ±iP i ′′ ) -the operator that occurs when the energy-momentum tensor is presented in a split form [17,37]. Summing over the Matsubara frequencies and leaving in the expression (8.1) only the terms contributing to the leading divergence, we obtain where ∂ 2n (∂p i ) 2n denotes a linear combination of derivatives of the 2n-th order of the form (without proof, we assume that the explicit dependence on the coordinates in any order can be rewritten through the derivatives and the integration of the exponential factor e px leads to the replacement of all the momenta of the form p i → ±p as it was in all orders of perturbation theory considered so far). Given that D 00 i is quadratic in momenta, the first term of the Laurent series, which gives the leading infrared divergence, in (8.2) has the form A n |a| 2n ∼ |a| 2n T d|p|/|p| 2n−2 , which was to be proved. On the other hand, it can be shown that the diverging contribution in the massless case (3.9) exactly corresponds to the Matsubara zero modes. Indeed, expression (3.8) is formed from a set of correlators of the same type, the number of which is determined by Wick theorem (24 for Dirac fields and complex scalar fields and 24 × 16 for real scalar fields). In particular, for real scalar fields, the coefficient A 2 equals [37] where ellipsis includes similar 24 × 16 − 1 terms from other correlators in Wick theorem. Keeping in (8.4) the contribution of only p n = q n = k n = r n = l n = 0 and making the necessary integrations, we find that this contribution entirely enters the infrared divergence A direct calculation of the remaining correlators shows that their contributions are equal and, as a result, we obtain which exactly corresponds to the divergence (3.9). Thus, indeed, the divergences arising in the massless theory are entirely determined by the zero Matsubara modes. The regularization proposed in the Section III, in fact, has serious physical grounds. We consider integrals independent of the dimensional parameter, which, by definition, satisfy the relation [40] I(αp) = α l I(p) , (8.7) in particular, d(α|p|)/(α|p|) 2n = α 1−2n d|p|/|p| 2n . It turns out that in dimensional regularization, such integrals are always zero which is connected with the axioms and definitions of dimensional regularization [38,40] and is sometimes called Veltman's formula in the literature [39]. Property (8.8) is often used in quantum field theory, including quantum field theory at finite temperatures (see, in particular, Chapter 2 of [41]). It would seem that in this way, we immediately get confirmation of the recipe for dealing with these divergences by subtracting them. However, as noted, for example, in [41], the situation becomes nontrivial, if higher orders of perturbation theory lead to an infinite series of similar divergences. And then, despite the fact that each of the diverging integrals separately is axiomatically zero, their sum can give a finite contribution.
To test the possibility of such a situation, it is necessary to consider higher orders of perturbation theory in acceleration, which is a difficult task from a technical point of view. However, a partial answer to the question about the divergences in higher orders can be obtained if we consider only the contribution of zero modes.
In particular, the sixth-order term in perturbation theory is described by the formula ×D 00 (iP 6 , −iP 7 )D 00 (iP 7 , −iP 1 ) + .... , (8.9) where the ellipsis corresponds to the contribution of the other terms coming from the Wick theorem. Using the equation and considering the contribution of the zero modes ω 1 = ... = ω 7 = 0 we get that the contribution of the correlator under consideration is equal to zero. Assuming that, as in the case of fourth-order coefficients, the contributions of zero modes from different correlators arising from Wick theorem are equal, we obtain In the same way we also obtain A ω=0 Thus, at least, the leading divergences in the first two higher orders of the perturbation theory apparently do not arise. If this situation is general (no leading divergences in higher orders and no subleading divergences), we can remove the divergences from the expressions (3.9) based on (8.8).
We now consider the divergences for the finite mass (3.17) and (3.18). For a finite mass, all divergences arising, both d|p|/|p| 2 and d|p|/|p| 4 , are fictitious in the sense that the integral formulas themselves, in particular (3.15), as functions of mass, do not contain divergences, which can be verified directly numerically.
On the other hand, if we sum up all the divergences in all orders in mass, then, as we will now show, we eliminate the fictitious divergences and get the correct expression for the perturbative series. A similar procedure of summation of infrared divergences was realized, in particular, in [41].
We first consider the divergences in the order a 2 . By directly decomposing the integrand in (3.15) and isolating the divergences as negative-power terms of the Laurent series, we can show that a series of divergences arises where the ellipsis includes both terms of higher orders and integrals from the nondivergent parts of the orders m 4 , m 6 . In this case, there are no subleading infrared divergences. We can also assume that the infrared divergences form a geometric progression. To sum up these divergences mathematically rigorously, we consider the integrand A 1 (m) = ∞ 0 d|p|a 1 (m 2 , |p| 2 ) in (3.15). It is easy to prove that by expanding it in a series of m 2 , the leading divergence in the order m 2n has the form m 2n /|p| 2n . Then the expansion of a 1 (m 2 , |p| 2 ) in a series has the form n m 2n |p| 2n−1 + ... . (8.14) We will replace |p| → λ|p|, m → λm, after which we find the limit λ → 0. This will allow us to sum up the leading infrared divergences The left-hand side in (8.15) can be easily found, we get 16) and, thus, the assumption made in (8.13), that the leading infrared divergences form a geometric progression, is confirmed. In particular, expanding the left-hand side of (8.16) in a series, we would obtain the terms (8.13).
Integrating (8.16), we obtain a contribution to the energy density The contribution (8.17) can be called nonperturbative in mass, since it has the form √ m 2 and does not directly follow from the perturbative expansion in m 2 . Thus, in the order m 2 , taking into account the contribution of infrared divergences, we obtain + ... , (8.18) where the ellipsis denotes the potential contribution of subleading divergences and finite terms in orders m 2n , n > 1.
Note that the correctness of the result obtained (8.18) can be checked numerically by finding the numerical value of the derivatives of the integral ∂ ∂m A 1 (m) and ∂ 2 ∂m 2 A 1 (m), which, in particular, are finite.
We can also rigorously prove that there are no subleading divergences. In particular, this follows from the equality The absence of subleading divergences corresponds to equality of (8.19) to a finite polynomial with positive powers. This has been verified for a number of values k (k = 1, 2, 3, 4).
A similar situation will be with the divergences in the order a 4 . In particular, the divergence d|p|/|p| 2 , which, as previously described, can be excluded in the massless case, since it is equal to zero, should now be summed with all terms of higher orders m 2n . There is no contradiction with what we talked about previously in the massless case, since each of the divergences is equal to zero separately, but their sum can be finite.
First, we need an expression for the coefficient in energy density for an arbitrary mass, without expansion in mass. This can be done by holding the mass in the energy-momentum tensor and propagators, as a result of which we obtain an expression similar to (3.8) B (E p ) + 3m 2 |p| 2 10 + |p| 4 n (5) B (E p ) + m 2 |p| 4 70 + |p| 6 25 n B (E p ) Expanding (8.20) in a series in mass, we obtain a series of divergences As in the previous case, we see that there are no subleading divergences. It can be shown that the leading divergences are of the order m 2n−2 /|p| 2n . Accordingly, expanding the integrand in (8.21), we obtain Replacing |p| → λ|p|, m → λm and taking the limit λ → 0, we get ∞ n=1 g n m 2n−2 |p| 2n = lim λ→0 λ 2 a 2 (λ 2 m 2 , λ 2 |p| 2 ) = T |p| 2 (15m 4 + 40m 2 |p| 2 + 16|p| 4 ) 60π 2 (m 2 + |p| 2 ) 4 . (8.23) Thus, we have found the sum of the leading divergences. After integration we obtain , (8.24) and the contribution to the coefficient A 2 which is also confirmed numerically. Thus, the infrared divergences found in the Section III can indeed be excluded both in the massless case and for the massive theory. In the case of a massive theory, these divergences can be summed up and give a finite nonperturbative and odd-in-mass contribution, and in this sense they can be excluded from terms of the zeroth and m 2 order. The study of these terms from the point of view of the Unruh effect requires additional consideration of nonperturbative in acceleration terms, which is beyond the scope of this paper.
We also note that there is another way to cancel the infrared divergences, if we require the execution of T µν (T = T U ) = 0 from the very beginning. This approach is similar to [29,32,35] and also leads to the exclusion of terms with divergences. However, nonperturbative terms m|a| 2 , |a| 4 /m may be lost.
In conclusion, we discuss a possible connection with Bose condensation. Indeed, according to, for example, [41], the appearance of infrared divergences is a possible indication of Bose condensation. The question of the possibility of Bose condensation due to acceleration is a non-trivial problem requiring a separate consideration. The main argument in favor of the absence of such a phenomenon is the lack of such condensate in the dual approach with a conical singularity. In this approach, condensation does not occur, at least in the temperature range T > T U .
In the statement of the problem, we consider a gas of free particles. At zero chemical potential, Bose condensate does not occur in such a gas. When the system acquires acceleration, we would not expect the appearance of condensate, since acceleration leads to heating of the medium, and temperature, as a rule, plays the role of a factor that destroys the condensate.
The conclusion is that the appearance of infrared divergences is typical consequence of the Bose distribution, but is not necessarily associated with Bose condensation (in particular, in the simplest example, expanding the energy density of the Bose gas in a series in mass, we would also get a similar series of infrared divergences).

IX. DISCUSSION
In the Sections III, IV, V we calculated quantum corrections related to acceleration to the energy-momentum tensor. We have shown that both in the case of massless fields and in the case of massive fields in the first order in mass, the calculated corrections satisfy the condition following from the Unruh effect. It is clear, since the calculated mean value of the energy-momentum tensor is normalized to the Minkowski vacuum, which corresponds to taking all the products of the operators using normal ordering [26]. Then, according to the Unruh effect, the Minkowski vacuum is perceived by the accelerated observer as a heat bath with Unruh temperature. Therefore, at the proper temperature equal to the Unruh temperature, the mean value of the energy-momentum tensor should be zero. This is what we have shown for a wide class of theories. Thus, we can talk about confirming the universality of the Unruh effect in the framework of the Zubarev approach, which is a general quantum-field phenomenon that does not depend on the type of fields under consideration.
We have also shown the emergence of conical geometry [29,30,[32][33][34][35] in the statistical Zubarev approach [17,23,24]. The expressions obtained in the framework of statistical approach exactly coincide with the mean values calculated in the space-time with a conical singularity both in the case of massless fields and in the quadratic order in mass.
In particular, this allows one to obtain expressions for an accelerated medium from known results for cosmic strings and vice versa.
An important consequence about the non-renormalization of the obtained expressions follows from this duality. When considering the formulas (3.10), (3.20), (4.2), (4.3), (5.2), (5.5) the question arises as to whether the calculated acceleration orders are maximal. Now we have received a positive answer to this question. Indeed, in formulas (6.3), (6.5) and (6.11), obtained using the geometrical approach, the calculated orders are maximal as the acceleration effects are taken into account in a nonperturbative way.
Thus, we can make a prediction that the calculation of subsequent acceleration corrections, in which negative degrees of temperature could formally appear, within the framework of the statistical approach with the operator (3.1) will give zero. We have also verified this statement directly in a particular case of corrections of the order m 2 |a| 4 /T 2 in the coefficients A m2 2 , A m2 4 and A m2 6 in (3.18) and (5.4). These corrections turned out to be zero (in the case of scalar fields, after subtracting the divergences).
We also note that absence of higher orders or polynomiality is associated with the properties of Sommerfeld integrals when integrated in the complex plane [16] as was also discussed in Section II. Moreover, according to [16], it is necessary to make a substantial remark that formulas of the form (3.10), (3.20), (4.2), (4.3), (5.2), (5.5) are exact nonperturbative expressions only in the region T > T U . When considering the domain T < T U , perturbative formulas of the form (5.2) may stop to be applicable and additional nonperturbative contributions can appear. Moreover, we can talk about the existence of instability at the boundary of two regions at T = T U at least for Dirac field.

X. CONCLUSIONS
We have calculated quantum corrections related to the acceleration to free-field energymomentum tensors using the statistical Zubarev density operator. A wide class of theories is considered: massless real and complex scalar fields, Dirac field, and also massive fields in the quadratic order in mass. All calculated corrections satisfy the Unruh effect: the energymomentum tensor, taking into account the obtained corrections, turns out to be zero at the proper temperature equal to the Unruh temperature. Thus, the universality of the Unruh effect in the statistical approach is demonstrated.
In the case of Dirac field, the studied corrections lead to finite momentum integrals, both in the massless case and for the corrections of the order of m 2 . However, for scalar fields, infrared divergences appear in the corrections of the order O(|a| 4 ) and O(m 2 |a| 2 ). In the case of massless theory, these divergences correspond to the Matsubara zero modes and can be excluded based on Veltman's formula. In the case of massive fields, a summation of an infinite series of infrared divergences can be made, as a result of which it was shown that they contribute to the odd terms in mass, a detailed study of which is beyond the scope of this paper. To summarize, effectively these divergences can be regularized by subtracting the corresponding negative power terms of the Laurent series of the form 1/|p| 2 and 1/|p| 4 . As a result, we obtain the expressions for the energy-momentum tensor satisfying the Unruh effect.
It is shown that in the used statistical approach of Zubarev, conical geometry emerges. In particular, the calculated quantum corrections exactly correspond to the corrections calculated in the framework of field theory in a space with a conical singularity [29,30,[32][33][34][35] in all cases considered. We can also talk about the duality of statistical and geometrical approaches. This duality was first noted in [16], and in this paper we show that it is a general phenomenon.
We began to study the consequences of the discovered duality. In particular, since all the expressions calculated in a space with a conical singularity were exact and nonperturbative, it should be expected that in the statistical approach all the higher order terms will be also equal to zero. We have verified this directly in particular cases by calculating quantum corrections of the order of m 2 |a| 4 /T 2 for all considered field theories. All corrections of this type turned out to be equal to zero.
The statistical approach inherently describes an effective interaction, introduced on a macroscopic scale or in the infrared. At the same time, the dual quantum field approach in a space with a conical singularity, as expected, on the contrary should be valid on a microscopic scale in the ultraviolet region. The existence of the duality of these two approaches makes it possible to smoothly join two regions of scales.
In addition, duality allows us to discuss the issue of Bose condensation in an accelerated medium. From the point of view of the statistical approach, Bose condensation associated with acceleration should be investigated as a separate non-trivial case. On the other hand, field theory with a conical singularity indicates the absence of such a phenomenon, which is confirmed by general arguments about the relationship between acceleration and temperature resulting from the Unruh effect.