Lattice Universe: examples and problems

We consider lattice Universes with spatial topologies \documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$T\times T\times T$$\end{document}T×T×T, \documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$ T\times T\times R $$\end{document}T×T×R, and \documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$ T\times R\times R$$\end{document}T×R×R. In the Newtonian limit of General Relativity, we solve the Poisson equation for the gravitational potential in the enumerated models. In the case of point-like massive sources in the \documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$T\times T\times T$$\end{document}T×T×T model, we demonstrate that the gravitational potential has no definite values on the straight lines joining identical masses in neighboring cells, i.e. at points where masses are absent. Clearly, this is a nonphysical result, since the dynamics of cosmic bodies is not determined in such a case. The only way to avoid this problem and get a regular solution at any point of the cell is the smearing of these masses over some region. Therefore, the smearing of gravitating bodies in \documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$N$$\end{document}N-body simulations is not only a technical method but also a physically substantiated procedure. In the cases of \documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$ T\times T\times R $$\end{document}T×T×R and \documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$ T\times R\times R$$\end{document}T×R×R topologies, there is no way to get any physically reasonable and nontrivial solution. The only solutions we can get here are the ones which reduce these topologies to the \documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$T\times T\times T$$\end{document}T×T×T one.


Introduction
Papers devoted to the lattice Universe can be divided into two groups. The first group includes articles (see, e.g., [1][2][3][4][5][6][7][8][9][10][11]) offering alternative cosmological models. Despite the great success of the standard CDM model, it has some problematic aspects. The main one is the presence of dark energy and dark matter which constitute about 96 % of the total energy density in the Universe. However, the nature of these components is still unknown. Another subtle point is that the conventional model is based on the Friedmann-Lemaitrea e-mail: maxim.brilenkov@gmail.com b e-mail: maxim.eingorn@gmail.com c e-mail: ai.zhuk2@gmail.com Robertson-Walker (FLRW) geometry with the homogeneous and isotropic distribution of matter in the form of a perfect fluid. Observations show that such an approximation works well on rather large scales. According to simple estimates made on the basis of statistical physics, these scales correspond to 190 Mpc [12], which is in good agreement with observations. This is the cell of uniformity size. Deep inside this cell, our Universe is highly inhomogeneous. Here, we clearly see galaxies, dwarf galaxies, groups, and clusters of galaxies. Therefore, it makes sense to consider matter on such scales in the form of discrete gravitational sources. In this case, we arrive at the question how this discrete distribution influences global properties and dynamics of the Universe. This problem was investigated in the above mentioned papers (see also [13]). Here, gravitating masses are usually distributed in a very simplified and artificial way. They form either periodic structures of identical masses with proper boundary conditions or correspond to Einstein equation solutions (e.g., Schwarzschild or Schwarzschild-de Sitter solutions) matching with each other with the help of the Israel boundary conditions. Usually, such models do not rely on the CDM background solution and do not include observable parameters (e.g., the average rest-mass densityρ of matter in the Universe). As a result, these models have nothing in common with the observable Universe. Their main task is to find new phenomena following from discretization and nontrivial topology.
Papers from the second class are devoted to numerical Nbody simulations of the observable Universe. Here, the lattice is constructed as follows. In the spatially flat Universe, we choose a three-dimensional cell with N arbitrarily distributed gravitating masses m i and suppose periodic boundary conditions for them on the boundary of the cell. Such models rely on a background FLRW geometry with a scale factor a. It is supposed that the background solution is the CDM model with the perfect fluid in the form of dust with the average rest-mass density ρ. Discrete inhomogeneities with the real rest-mass density ρ = N i=1 m i δ(r − r i ) perturb this background. The gravitational potential inside the cell is determined in the Newtonian limit by the following Poisson equation [14][15][16]: (1.1) where G N is the Newtonian gravitational constant, and r, r i belong to the cell, e.g., Here, the Laplace operator = ∂ 2 /∂ x 2 + ∂ 2 /∂ y 2 + ∂ 2 /∂z 2 , and the coordinates x, y, and z, the gravitational potential ϕ, and the restmass densities ρ and ρ correspond to the comoving frame. All these quantities are connected with the corresponding physical ones as follows: R phys = ar, phys = ϕ/a, and ρ phys = ρ/a 3 . Equation (1.1) is the basic equation for the N -body simulation of the large scale structure formation in the Universe [16]. The same equation can also be obtained in the Newtonian limit of General Relativity [12,17,18]. If we know the gravitational potential, then we can investigate the dynamics of the inhomogeneities/galaxies taking into account both gravitational attraction between them and the cosmological expansion of the Universe [17,19,20].
It can easily be seen that in the case of a finite volume (e.g., the volume of the cell) Eq. (1.1) satisfies the superposition principle. Here, for each gravitating mass m i we can determine its contribution to the average rest-mass density: Therefore, we can solve Eq. (1.1) for each mass m i separately.
If we do not assume periodic boundary conditions, at least for one of the directions, there is no lattice in these directions and space along them is not compact (in the sense of the lack of a finite period of the lattice). Obviously, in infinite space the number of inhomogeneities must also be infinite: N → ∞. This case has a number of potentially dangerous points. First, the superposition principle does not work here because we cannot determine ρ i for each of the masses m i . Second, it is known that the sum of an infinite number of Newtonian potentials diverges (the Neumann-Seeliger paradox [21]). Therefore, in general, the considered model can also suffer from this problem if we do not distribute masses in some specific way. Third, we can easily see from Eq. (1.1) that the presence of ρ will result in quadratic (with respect to the noncompact distance) divergence. Hence, to avoid it, we should cut off gravitational potentials in these directions. This also may require a very specific distribution of the gravitating masses.
In the present paper, we investigate Eq. (1.1) for different topologies of space which imply different kinds of lattice structures. First, in Sect. 2, we consider the T × T × T topology with periodic boundary conditions in all three spatial dimensions. For point-like sources, we obtain a solution in the form of an infinite series. This series has the well-known Newtonian type divergence in the positions of the masses. However, we show that the sum of the series does not exist on the straight lines joining identical particles in neighboring cells. Therefore, there is no solution in points where masses are absent. This is a new result. To avoid this nonphysical property, in Sect. 3, we smear point-like sources. We present them in the form of uniformly filled parallelepipeds. In this case, the infinite series has definite limits on the considered straight lines. Therefore, smearing of the gravitating masses in N -body simulations plays a dual role: first, this is the absence of the Newtonian divergence in the positions of the masses, second, this is the regular behavior of the gravitational potential in all other points. Thus, in the present paper we provide a physical justification for such a smearing.
In Sects. 4 and 5 we consider a possibility to get reasonable solutions of Eq. (1.1) in the case of absence of periodicity in one or two spatial directions. In Sect. 4, we investigate a model with the spatial topology T × T × R, i.e. with one noncompact dimension, let it be z. As we mentioned above, due to noncompactness, the gravitational potential may suffer from the Neumann-Seeliger paradox and additionally has a divergence of the form ρz 2 → +∞ for |z| → +∞. In this section we try to resolve these problems with the help of a special arrangement of gravitating masses in the direction of z. A similar procedure in the flat Universe with topology R 3 was performed in [17]. Unfortunately, in the case of the topology T × T × R, there is no possibility to arrange the masses in such a way that the gravitational potential is a smooth function in any point z. We have the same result for the Universe with topology T × R × R, which is considered in Sect. 5. Here we also demonstrate the impossibility of constructing a smooth potential. The main results are briefly summarized in Sect. 6.

Topology T × T × T : point-like masses
Obviously, for topology T × T × T the space is covered by identical cells, and, instead of an infinite number of these cells, we may consider just one cell with periodic boundary conditions. As we mentioned in Introduction, due to the finite volume of the cell, we can apply the superposition principle. It means that we can solve Eq. (1.1) for one arbitrary gravitating mass, and the total gravitational potential in a point inside the cell is equal to a sum of gravitational potentials (in this point) of all N masses. Without loss of generality, we can put a gravitating mass m at the origin of coordinates. Then the Poisson equation (1.1) for this mass reads Taking into account that delta functions can be expressed as 1 Therefore, it makes sense to look for a solution of this equation in the form where the unknown coefficients C k 1 k 2 k 3 can easily be found from Eq. (2.3): (2.5) Hence, the desired gravitational potential is where k 2 1 + k 2 2 + k 2 3 = 0. If x, y, z simultaneously tend to zero, then the gravitational potential (2.6) has the Newtonian limit 1 This is the standard Dirac delta-function representation for the considered geometry of the model (see, e.g., [10]). 2 In the expression below, instead of the product cos(2π k 1 x/l 1 ) cos(2π k 2 y/l 2 ) cos(2π k 3 z/l 3 ) we can write cos(2π k 1 x/l 1 + 2π k 2 y/l 2 + 2π k 3 z/l 3 ), and with the help of the wellknown formulas for the cosine of the sum this expression will give only the contribution of the above mentioned form, cos(2π k 1 x/l 1 ) cos(2π k 2 y/l 2 ) cos(2π k 3 z/l 3 ). In fact, all terms containing, e.g., sin(2π k 1 x/l 1 ) (being an odd function of k 1 ), will disappear from the sum with symmetric limits (i.e. k 1 varying from −∞ to +∞).
where r = (x 2 + y 2 + z 2 ) 1/2 , as it should. A good feature of the potential (2.6) is that its average value (integral) over the cell is equal to zero: ϕ = 0. 3 This is a physically reasonable result, because ρ − ρ = 0. Clearly, in the case of a point-like gravitating source, we have the usual divergence at the point of its location. Now, we want to demonstrate that there is also a problem at the points where gravitating masses are absent. More precisely, we will show that the sum (2.6) is absent on straight lines which connect identical masses in neighboring cells. In our particular example, they are lines of intersection (pairwise) of the planes x = 0, y = 0, and z = 0. Let us consider the potential (2.6) on the straight line y = 0, z = 0. The numerical calculation of the potential on this straight line at the point x = l 1 /2 for different values of the limiting number n (being the maximum absolute value of the summation indices: |k 1,2,3 | ≤ n) is presented in the following table for the cubic cell case l 1 = l 2 = l 3 ≡ l. This table clearly demonstrates that the potential does not tend (with the growth of n) to any particular finite number. To understand the reason for this, let us analyze the structure of the expression (2.6) in more detail. For z = 0 the gravitational potential reads It is worth noting that in [12,17,22] the concrete mass distribution in the Universe with topology R 3 is cited as an example of the case of nonzero average value ϕ = 0. From a purely mathematical point of view this case is inadmissible in the framework of the first-order perturbation theory.
where we used the tabulated formulas for sums of series (see, e.g., [23], 5.1.25). All sums in this expression are potentially dangerous. To show it, we can drop the hyperbolic cotangents because coth k → 1 for k → +∞. The two last sums are divergent, depending on which straight line we consider: x = 0 or y = 0, respectively. For example, on the straight line y = 0, the sum +∞ The rough estimate of the double sum also leads to a divergent result. To be more precise, we investigate now finite sums 4 of the "suspect" terms on the straight line y = 0: It is worth noting that in the case l 1 = l 2 and x/l 1 = 1/2 the logarithmically divergent terms exactly cancel each other. In fact, it follows directly from the following estimates: Therefore, both of these logarithmically divergent terms cancel each other. Nevertheless, the expression (2.9) does not have a definite limit for n → +∞. To demonstrate it, along with (2.9) let us introduce the function 4 Obviously, the inclusion of the hyperbolic cotangents does not effect the main results but makes calculations more complicated.
Evidently, if the expression (2.9) is convergent for n → +∞, then in this limit the difference f n+1 (x) − f n (x) → 0. After some simple algebra we get (for l 1 Here, the last term in the third line vanishes for n → +∞. Therefore, the problem of the convergence of (2.9) is reduced now to the analysis of f n (x). In Fig. 1, we show the graph of f n (x) (for x/l 1 = 1/2) as a function of n. Each point gives the value of f n (x) for the corresponding number n. This picture clearly demonstrates that the difference f n+1 (x) − f n (x) does not tend to zero for growing n. Even more, it does not go to any definite value.
It can also be verified that a similar result takes place for any other point on any of the straight lines and holds also for l 1 = l 2 . Therefore, we have proven that in the case of pointlike gravitating masses in the considered lattice Universe the gravitational potential has no definite values on the straight lines joining identical masses in neighboring cells. Clearly, this is a nonphysical result, since the dynamics of cosmic bodies is not determined in such a case. Can the smearing of gravitating masses resolve the problem found in the previous section? To answer this question, we present gravitating masses as uniformly filled parallelepipeds. This representation of the masses looks a bit artificial. However, such a form is the most appropriate for the considered cells, and the most important point is that the form of smearing does not matter for us at the moment. We just want to get a principal answer to the question of the possibility to avoid the problem with the help of smearing. So, let the mass m be uniformly smeared over a parallelepiped (with the lengths of the edges a, b, and c) which we put, without loss of generality, in the middle of the cell. It is convenient to introduce a function f 1 (x) equal to 1 for x ∈ [−a/2, a/2] and 0 elsewhere inside [−l 1 /2, l 1 /2]. We can write this function Similarly, and Therefore, the rest-mass density of the mass under consideration is Then Eq. (1.1) for this mass reads 2 π n sin aπ n l 1 cos 2π n l 1 x sin bπ j l 2 cos 2π j l 2 y × sin cπ k l 3 cos 2π k l 3 z This equation implies that it makes sense to look for a solution in the following form: Let us choose the same straight line as in the previous section, that is, y = 0, z = 0, and the same point x = l 1 /2. The numerical calculation of the gravitational potential in this point for different values of the limiting number n is presented in the following table for the cubic cell case under the additional condition a = b = c = (3/7)l. In contrast to the previous case of a point-like source, here the potential apparently tends to a particular finite value. Therefore, in the case of smeared gravitating masses the gravitational potential has a regular behavior at any point inside the cell (including, e.g., the point x = y = z = 0).

Topology T × T × R
The T ×T × R topology implies one noncompact dimension; say z. Therefore, there is a lattice structure in the directions x and y and an irregular structure in the direction z. In a column x ∈ [−l 1 /2, l 1 /2], y ∈ [−l 2 /2, l 2 /2], z ∈ (−∞, +∞) there is an infinite number of gravitating masses. To obtain a "nice" regular solution, we will try to arrange the masses in the z direction in such a way that in each point z the gravitational potential is determined by one mass only. There are two possibilities to do that. Let this mass be at z = 0. In the first scenario, the potential and its first derivative (with respect to z) should vanish at some distance z 0 (which we determine below). Then the next mass should be at a distance (in the z direction) equal to or greater than z 0 + z 1 , where z 1 is a distance at which the gravitational potential and its first derivative vanish for the second mass. Similarly, we should shift in the direction of z the third mass with respect to the second one and so on. In this scenario, we can arrange strips z between masses where the potential is absent. It occurs, e.g., between the first and second masses if the second mass is situated at distances greater that z 0 + z 1 . In the strip, we place a uniform medium with the rest-mass density ρ. The coordinates x ∈ [−l 1 /2, l 1 /2] and y ∈ [−l 2 /2, l 2 /2] of masses are arbitrary. In the second scenario, we should determine distances z 0 , z 1 , z 2 , . . . where potentials of neighboring (in the z direction) particles are smoothly matched to each other. This means that at these distances the potentials are generally nonzero. Moreover, we suppose that their first derivatives are zero at the points of matching, i.e. the potentials have extrema in these points. In this scenario, the neighboring (in the z direction) masses should have the same coordinates x and y. Now let us consider these scenarios in detail. For both of them, we need to look for a solution just for one particle. Let this particle be in the point x = y = z = 0. Then Eq.
Keeping in mind the regular structure in the x and y directions, we can represent the delta functions δ(x) and δ(y) in the form (2.2). So, Eq. (4.1) is reduced to Evidently, we can look for a solution of this equation in the form and from the Poisson equation (4.2) we get (4.4) In this section, the prime denotes the derivative with respect to z. Now, we should determine the unknown functions C k 1 k 2 (z). First, we find the zero mode C 00 (z), which satisfies the equation

This equation has the solution
where B is a constant of integration. This solution is a function growing with z. Therefore, we must cut it off at some distance z 0 . Let us consider the first scenario. From the condition C 00 (z 0 ) = 0 we obtain The second condition C 00 (z 0 ) = 0 provides the value of B: (4.8) Now, we want to determine the form of C k 1 k 2 (z) when k 2 1 + k 2 2 = 0. In this case Eq. (4.4) is consistent only if the following condition holds true: We look for a solution of this equation in the form where A and B are constants. The substitution of this function into Eq. (4.9) gives Therefore, From the boundary condition C k 1 k 2 (z 0 ) = 0 we get It can easily be verified that the function (4.12) (with B from (4.13)) does not satisfy the boundary condition C k 1 k 2 (z 0 ) = 0. Hence, we cannot determine the gravitational potential in accordance with the first scenario. Now, we intend to demonstrate that there is a possibility to find the potential in the framework of the second scenario in the case of identical masses. However, this construction has a drawback inherent in the T × T × T model with the point-like source.
In the second scenario with identical masses m, all of them have the same coordinates x, y and are separated by the same distance 2z 0 ≡ l 3 in the direction of z. Here, the function C 00 (z) still has the form (4.6). Since we require C 00 (z 0 ) = 0, the boundary z 0 is determined by (4.7). However, the constant B is not given now by (4.8), because the condition C 00 (z 0 ) = 0 is absent. This constant can by found from the condition ϕ = 0 over the period l 3 = 2z 0 . That is, (4.14) The functions C k 1 k 2 (z) for k 2 1 + k 2 2 = 0 are given by Eq. (4.12), where the constant B follows from the boundary condition C k 1 k 2 (z 0 ) = 0: It can easily be verified that C k 1 k 2 (z) can be rewritten in the form (4.16) Therefore, in the second scenario the gravitational potential is sinh(2π k 1 z 0 /l 1 ) cos (2π k 1 x/l 1 ) cos (2π k 2 y/l 2 ) When z = 0 and x, y simultaneously go to zero, the potential ϕ → −G N m/ x 2 + y 2 , as it should. From the physical point of view, it is clear that this scenario should coincide with the T × T × T case. In fact, the triple sum (2.6) can be rewritten in the form (4.17) with the help of [23] (see 5.4.5). It can also easily be seen that on the plane z = 0 the expression (4.17) exactly coincides with Eq. (2.8). Therefore, in the second scenario we again arrive at the nonphysical result that the gravitational potential has no definite values on straight lines y = 0 and x = 0.

Topology T × R × R
In this section we consider a model with a periodic boundary condition in one direction only. Two other spatial dimensions are noncompact. Here, in analogy with the previous section, we also suppose that the gravitational potential in the vicinity of a particle is determined by its mass only.
The shape of such a domain is dictated by the symmetry of the model and will be described below. On the boundary (in the direction of noncompact dimensions) of this domain the potential and its first derivative are equal to zero, and between such domains the potential is absent: ϕ = 0. Therefore, this model is similar to the first scenario in the previous section. Let the mass be at the point x = y = z = 0 and the periodic boundary condition (with the period l 1 ) be along the x coordinate. Then the Poisson equation (4.1) for this topology can be written as follows: We look for a solution of this equation in the form Then from the Poisson equation (5.1) we get For the zero mode k 1 = 0 this equation gives Following the geometry of the model, it makes sense to turn to polar coordinates: Then the two-dimensional Laplace operator is It is clear that due to the symmetry of the problem the functions C k 1 do not depend on the azimuthal angle φ. Therefore, Eq. (5.5) reads

This equation has the solution
where we took into account that ξ ln ξ = 2πδ (ξ ). Similar to the previous model with one noncompact dimension, here the solution is also divergent in some directions. In the present case, it grows with the polar radius ξ . So, we must cut off this solution at some distance ξ 0 . Clearly, this boundary represents the cylindrical surface ξ = ξ 0 . The domain in which we put the mass m 0 = m is a cylinder with the radius ξ 0 and the generator is parallel to the x-axis. The length of the cylinder along the x-axis is l 1 . The mass m is in the center of the cylinder (with the coordinate x = 0 for the considered case). The next particle of the mass m 1 is inside its own cylinder with the generator along the x-axis and the radius ξ 1 . This particle may have a coordinate x different from the first particle. All these cylinders have the periodic (with the period l 1 ) boundary conditions along the x-axis. On the other hand, they should not overlap each other in the transverse (with respect to the x-axis) direction. Moreover, it is impossible to match them smoothly via cylindrical surfaces. Therefore, we demand that the gravitational potential outside the cylinders is equal to zero. Hence, on the boundaries of the cylinders (ξ = ξ 0 for the first mass) the gravitational potential and its first derivative (with respect to ξ ) are equal to zero. These boundary conditions enable us to determine the radius ξ 0 and the constantB in Eq. (5.9). For example, from the condition dC 0 (ξ 0 )/dξ = 0 we get where s 0 = πξ 2 0 is the cross-sectional area of the cylinder. From the second boundary condition C 0 (ξ 0 ) = 0 we get the value ofB: Obviously, in the case k 1 = 0, Eq. (5.3) is consistent only if the following condition holds true: which for ξ > 0 can be rewritten in the form The solutions of this equation are the modified Bessel functions: where C 1 is a constant of integration. We took into account that the function K 0 (ξ ) → − ln ξ for ξ → 0, so the twodimensional Laplacian acting on this function provides the necessary delta function in Eq. (5.12). The function (5.14) should satisfy the same boundary conditions at ξ = ξ 0 as the function C 0 (ξ ). It can easily be verified that we cannot simultaneously reach both equalities C k 1 (ξ 0 ) = 0 and dC k 1 (ξ 0 )/dξ = 0. Hence, we cannot determine the gravitational potential in accordance with the proposed scenario.
To conclude this section, it is worth noting that we can construct the potential in the scenario similar to the second one from the previous section. This is the case of identical masses distributed regularly in all directions. Obviously, this case is reduced to the T × T × T model from Sect. 2 with the drawback inherent in it.
Therefore, similar to the previous section, we also failed in determining a physically reasonable gravitational potential in the model with the topology T × R × R.

Conclusion
Our paper was devoted to cosmological models with different spatial topologies. According to the recent observations, our Universe is spatially flat with rather high accuracy. So, we restricted ourselves to this case. However, such a spatially flat geometry may have different topologies depending on the number of directions/dimensions with toroidal discrete symmetry. These topologies result in different kinds of lattice Universes. There are a lot of articles exploring the lattice Universes (see, e.g., [1][2][3][4][5][6][7][8][9][10][11] and references therein). One of their main motivations is to provide an alternative (compared to the standard CDM model) explanation of the late-time accelerated expansion of the Universe. Another important point is that our Universe is highly inhomogeneous inside the cell of uniformity with the size of the order of 190 Mpc [12]. Hence, it is quite natural to consider the Universe on such scales filled with discrete sources rather than a homogeneous isotropic perfect fluid.
On the other hand, N -body simulations of the evolution of structures in the Universe are based on the dynamics of discrete sources in chosen cells. To perform such simulations, we should know the gravitational potentials generated by these sources. Therefore, the main purpose of our paper was the determination of the gravitational potentials in the cases of three different spatial topologies: T × T × T , T × T × R, and T × R × R. The potential satisfies the corresponding Poisson equations of the form (1.1). These equations can be obtained as a Newtonian limit of General Relativity [12,17]. So, to determine the potential, we should solve them. One of the main features of the analyzed Poisson equations is that they contain the average rest-mass density, which represents a constant in the comoving frame. This results in two problems. First, we cannot, in general, apply the superposition principle. Second, the presence of such a term leads to divergences in the directions of the noncompact dimensions. We tried to avoid these problems arranging masses in special ways. Our investigation has shown that the T × T × T model is the most physical one. Here, due to the discrete symmetry in all three directions, we can represent the infinite Universe as one finite cell with periodic boundary conditions in all dimensions. The finite volume of the cell enabled us to use the superposition principle and solve the Poisson equation for a single mass. The total potential in an arbitrary point of the cell is equal to the sum of potentials of all particles in the cell. Unfortunately, in the case of point-like gravitating sources the obtained solution has a very important drawback. Usually, it is expected that potentials diverge at the positions of the masses. However, in the model under consideration the gravitational potential has no definite values on the straight lines joining identical masses in neighboring cells, i.e. at the points where masses are absent. Clearly, this is a nonphysical result, since the dynamics of cosmic bodies is not determined in such a case. Then, looking for a more physical solution, we smeared the gravitating masses over some regions and showed that in this case the gravitational potential shows a regular behavior at any point inside the cell. Therefore, smearing represents the necessary condition of getting a regular gravitational potential in the lattice Universe. Usually in N -body simulations some sort of smearing is used to avoid divergences at the positions of the masses. Now, we have demonstrated that this procedure helps to avoid problems on the above mentioned straight lines as well. Therefore, the smearing of gravitating bodies in numerical simulations is not only a technical method but also a physically substantiated procedure, and in the present paper we provide a physical justification for such a smearing.
In the T × T × T model, particles in the cell may have different masses and may be distributed arbitrarily. In the cases of the topologies T × T × R and T × R × R, we cannot do this. We have shown that the only way to get a solution here is to suppose the periodic (in all dimensions) distribution of identical masses. However, such a solution is reduced to the one obtained in the case of the T × T × T topology. Therefore, first, this solution has a drawback inherent in this model, and, second, the distribution of the masses looks very artificial.