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Monthly Notices of the Royal Astronomical Society
, Volume 476 (1) – May 1, 2018

6 pages

/lp/ou_press/a-modified-friedmann-equation-for-a-system-with-varying-gravitational-tjeX3yYWsM

- Publisher
- The Royal Astronomical Society
- Copyright
- © 2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society
- ISSN
- 0035-8711
- eISSN
- 1365-2966
- D.O.I.
- 10.1093/mnras/sty335
- Publisher site
- See Article on Publisher Site

Abstract The Laser Interferometer Gravitational-Wave Observatory (LIGO) detection of gravitational waves that take away 5 per cent of the total mass of two merging black holes points out on the importance of considering varying gravitational mass of a system. Using an assumption that the energy-momentum pseudo-tensor of gravitational waves is not considered as a source of gravitational field, we analyse a perturbation of the Friedmann–Robertson–Walker metric caused by the varying gravitational mass of a system. This perturbation leads to a modified Friedmann equation that contains a term similar to the ‘cosmological constant’. Theoretical estimates of the effective cosmological constant quantitatively corresponds to observed cosmological acceleration. dark energy, cosmology: theory 1 INTRODUCTION An idea of a bouncing universe, where the Big Bang happens after the collapse of a previous universe, is actively investigated for last years (see, for example, Novello and Bergliaffa 2008; Cai et al. 2012; Brandenberger and Peter 2017). The bouncing cosmological models are free from a singularity, but have two other major problems: A physical cause of the Big Bang is unclear so far, as a cause for current acceleration of the Universe. Dynamics of matter and radiation in the bouncing cosmological models has been studied for long time (see e.g. Alpher and Herman 1949). High temperature ∼1010 K in the collapsed universe results in the complete destruction of nuclei of all chemical elements created in stars. Dicke et al. (1965) stated that ‘the ashes of the previous cycle would have been reprocessed back to the hydrogen required for the stars in the next cycle’. Temperature of 1010 K means that the Universe was compressed by approximately 1010 times, i.e a size of the Universe was about 1–10 light-years. The high temperature of 1010 K of the collapsed Universe could produce a high level of isotropy observed in the Universe at the present time (Misner 1968; Hawking and Ellis 1973). Recently, the Laser Interferometer Gravitational-Wave Observatory (LIGO) Scientific Collaboration announced a detection of gravitational waves caused by the merger of two black holes with masses of about 36 and 29 times the mass of the sun (Abbot et al. 2016). About three times the mass of the sun, i.e. about 5 per cent of the initial total mass of the black holes, was converted into gravitational waves. Recently, an idea of the existence of numerous black holes with masses of 20–100 times the mass of the sun was suggested (Bird et al. 2016). Those massive black holes can serve as ‘the dark matter’ (Bird et al. 2016). Therefore, the black holes become an important component of cosmological models, particularly, of the bouncing cosmology because the black holes are the only macro object that can survive the Big Crunch and the Big Bang and appear in the next cycle of the Universe (Clifton, Carr & Coley 2017). Studies of the cosmological dynamics with black holes, which have sizes up to the Hubble radius, were carried out in Quintin and Brandenberger (2016), Poplawski (2016), Chen et al. (2017), and Clifton et al. (2017). It is logical to hypothesize that the supermassive black holes of the centres of galaxies will be merged at final stages of the collapsing universe. For example, a simple estimate shows that 1011 supermassive black holes cannot be packed into a sphere with the radius being less than ∼0.1 light-year. Thus, numerous mergers of black holes will occur in the collapsed Universe having a size of 1–10 light-years. This merging process will likely form a single black hole (Penrose 2011), or the biggest black hole (the big black hole or BBH) and a number of smaller black holes, which will not have sufficient time to merge and which will exist in the expanding universe after the Big Bang (Clifton et al. 2017). In the framework of this hypothesis, it is interesting to consider a generalization of the Friedmann–Robertson–Walker (FRW) metric for a perturbation caused by a gravitational field of the BBH. Whereas the homogeneous universe is characterized by a scalefactor, a(t), which depends on time only, a universe perturbed by a variable gravitational mass is described by an inhomogeneous metric. Thus, the scalefactor can depend on space coordinates. Such inhomogeneous metrics were considered by Tolman (1934) and others (see e.g. Zel'dovich and Grishchuk 1984 and review of inhomogeneous cosmologies in Bolejko, Celerier, & Krasinski 2011). During the Big Crunch, the total mass of black holes will reduce because they will lose a few percent of their mass at each act of the merging process. Black holes that survive the Big Crunch will increase their mass after the Big Bang due to absorption of matter and radiation including the background gravitational radiation. The BBH will increase its mass with the highest rate because it has the largest cross-section of absorption. In 1998, the accelerated expansion of the Universe was discovered using observations of the distant supernovae (Riess et al. 1998; Perlmutter et al. 1999). An accelerating universe can be described by the Einstein equations with a phenomenological cosmological constant, Λ, which characterizes a repulsive force (Einstein 1952): \begin{equation} G_{\mu \nu }-g_{\mu \nu }\Lambda =-\frac{8 \pi G}{c^{4}}T_{\mu \nu }, \end{equation} (1)where Gμν is the Einstein tensor; gμν is the metric tensor; Tμν is the energy-momentum tensor; and G is the gravitational constant. Data collected by the Planck satellite instrument allow us to get the following estimate of the cosmological constant (Ade et al. 2016a): \begin{equation} \Lambda \approx 1.1 \times 10^{-56} \, \mathrm{cm^{-2}}. \end{equation} (2) At present, cosmological models containing the cosmological constant are widely used to describe main observations: the cosmic microwave background, spectra of the baryonic oscillations, and the chemical composition of the early Universe (Misner et al. 1973; Fixsen et al. 1997; Mather and Boslough 2008; Ade et al. 2016a). A physical nature of the cosmological constant is unclear so far. It is supposed that the repulsive force is caused by vacuum dark energy. A density of the dark energy, ρvac, is related to the cosmological constant by the following equation: Λ = 8πGρvac (see e.g. Carrol 2008). However, all attempts to calculate ρvac from the quantum theory bring to estimates, which exceed the observational data by 40–120 orders of the magnitude (Weinberg 1989; Carrol 2008). The LIGO detection of the gravitational waves attracts the attention to consideration of a varying gravitational mass in the general theory of relativity. It is well known that the energy of the gravitational field cannot be described by the energy-momentum tensor in contrast to the energy of ordinary matter and electromagnetic field. The energy of the gravitational field also cannot be localized. Before 1917, Einstein supposed that the energy of gravitational field is equivalent to the energy of matter as a source of gravitational field and included the energy-momentum pseudo-tensor of gravitational field in the right-hand part of his equations. After famous discussion with Schrodinger, Bauer and other scientists, Einstein changed his opinion. Since 1917, he never included pseudo-tensor of gravitational field in his equations. Due to these circumstances, any contributions of purely gravitational origin or combinations from metric tensor may be excluded from the right-hand part of Einstein’ equations or from a list of sources of a gravitational field by opinion, e.g. Einstein (1953), Eddington (1975), Chandrasekhar (1983), and Tourrenc (1997). This is kind of a non-standard approach accounting for energy of gravitational waves, but we follow Einstein's opinion: ‘Tik represents the energy that generates the gravitational field, but is itself of non-gravitational character (Einstein 1953). That means that the total gravitational mass of the Universe changes when a significant fraction of the mass of the black holes is converted into gravitational waves. An opposite process of increasing gravitational mass of the Universe is related to absorption of the background gravitational radiation by the BBH. In this paper, we consider cosmological effects of the variability of the gravitational mass caused by both conversion of the mass of merging black holes into gravitational waves and absorption of the background gravitational radiation by black holes. Other ways for changing of the gravitational mass are possible (e.g. Kutschera 2003), but in this paper we will consider a variability of the gravitational mass in general form, without discussion of specific physical causes of such variability. Kutschera (2003) and Gorkavyi and Vasilkov (2016) got solutions of the Einstein equations for the varying gravitational mass of a quasi-spherical system. The solution found by Kutschera (2003) and Gorkavyi and Vasilkov (2016) is a modified Schwarzschild metric for the varying gravitational mass. Using a relativistic gravitational potential in the fixed coordinate system, Gorkavyi and Vasilkov (2016) derived an equation for a repulsive force (for a probe particle with a unit mass): \begin{equation} F=\frac{\mathrm{\partial} }{\mathrm{\partial} {r}}\left[\frac{GM_0}{r}{\rm e}^{-\alpha (t-r/c)}\right]=-{\frac{GM}{r^2}}+{\frac{\alpha }{c}}{\frac{GM}{r}}. \end{equation} (3)The second term in equation (3) originates from the variability of a gravitational mass with a characteristic time 1/α and the finite velocity of spreading of gravitational field disturbances: \begin{equation} M(t,r)={M_0}{\rm e}^{-\alpha (t-r/c)}. \end{equation} (4) We will call this term α-force. The α-force is essentially relativistic because it depends on the light speed. Using a non-Einsteinian scalar–tensor theory, Galiautdinov and Kopeikin (2016) investigated gravitational forces caused by the variable gravitational constant. They also revealed a new force that is additional to the Newtonian attraction force. Reduction of the gravitational mass of the collapsing Universe due to merging of the black holes causes the repulsive α-force, which may be responsible for the Big Bang and accelerated expansion of the Universe at the initial stage (the analogy of the inflation period; Gorkavyi and Vasilkov 2016). It follows from equation (3) that the α-force can be larger than the Newtonian term in case of the strong change of a gravitational mass, i.e. α ≫ c/r. The model of the bouncing universe, which completely renews its chemical composition at the final contractive stage and explodes because of merging black holes, is based on the well-known physical concepts and does not involve new essences. But this model should provide an explanation of the current acceleration of the expanding Universe. This motivates a derivation of modified Friedmann equations that account for a perturbation of the Schwarzschild metric with a varying gravitational mass. A main question to this model can be formulated as follows: What rate of mass variability would it take to produce the currently measured acceleration attributed to the cosmological constant or dark energy? A focus of this paper is answering to this question. The paper is structured as follows. In Section 2, we briefly describe how the classical Friedmann equations are derived from the Einstein equations. The modified FRW metric is discussed in Section 3. In Section 4, we consider the modified Friedmann equations for the case of a variable gravitational mass and make an estimate of the cosmological constant. We also interpret the result in terms of cosmological acceleration. The discussion is provided in Section 5. Conclusions are given in Section 6. 2 THE CLASSICAL FRIEDMANN EQUATIONS To describe an expanding universe, the FRW metric is used. The classical Friedmann equation is derived from the Einstein equations assuming the FRW metric. According to this metric for a flat space, the time–space interval is expressed in the Cartesian coordinates as follows: \begin{equation} {\rm d}{s}^2={c^2}{\rm d}{t}^{2}-a^2(t)\left({\rm d}x^2_{\ast }+{\rm d}y^2_{\ast }+{\rm d}z^2_{\ast }\right), \end{equation} (5)where $${\rm d}r_{\ast }^2={\rm d}x^2_{\ast }+{\rm d}y^2_{\ast }+{\rm d}z^2_{\ast }$$ is the distance in the comoving coordinate system. The physical distance is related to the distance in the comoving coordinate system by the scalefactor a: r = a(t)r*. The FRW metric describes an isotropic and uniform universe in the comoving coordinate system. At the present time, the scalefactor is equal to unity: a(t) = 1. Assuming that the matter has no pressure, i.e. T00 = ρc2, we get the first Friedmann equation from equations (1) and (5): \begin{equation} \left(\frac{\dot{a}}{a}\right)^{2}=\frac{{\Lambda }c^{2}}{3}+\frac{8{\pi }G{\rho }}{3}. \end{equation} (6)To get the second Friedmann equation, let us differentiate equation (6) over time (Friedmann 1922; Liddle 2003): \begin{equation} \frac{\ddot{a}}{a}=\frac{{\Lambda }c^{2}}{3}+\frac{8{\pi }G{\rho }}{3}+\frac{4{\pi }G{\dot{\rho }}}{3}\frac{a}{\dot{a}}. \end{equation} (7) 3 A MODIFIED FRW METRIC The Schwarzschild metric in the Cartesian coordinates for a weak gravitational field is written as \begin{eqnarray} {\rm d}{s}^2=(1-b_{0}){c^2}{\rm d}{t}^{2}-(1+b_{0})\left({\rm d}x^{2}+{\rm d}y^{2}+{\rm d}z^{2}\right), \end{eqnarray} (8)where b0 = 2GM0/(rc2) (e.g. Landau and Lifshitz 1975; Weinberg 1972, see equation 8.3.7 with the first-order terms in this reference). Here, we use the physical distance, r, in a fixed coordinate system. In the modified Schwarzschild metric derived in Kutschera (2003); Gorkavyi and Vasilkov (2016), the constant mass, M0, is replaced with a variable mass M(t, r). The equation (8) in the comoving coordinates transforms to \begin{eqnarray} {\rm d}{s}^2\!=\![1-b(t,r)]{c^2}{\rm d}{t}^{2}\!-\!a^2(t,r)[1+b(t,r)]\left({\rm d}x^2_{\ast }\!+\!{\rm d}y^2_{\ast }\!+\!{\rm d}z^2_{\ast }\right),\nonumber \\ \end{eqnarray} (9)where b(t, r) = 2GM(t, r)/(rc2) is the known function and a(t, r) is the unknown scalefactor. Such a perturbed metric was first derived in McVittie (1933). It was also used in Dodelson (2003, see equation 4.9). In equation (9), b(t, r) can be considered as an analogy to the scalar potentials 2Φ = −2Ψ in equation (4.9) in Dodelson (2003). This type of a metric was studied in detail in Kopeikin (2012). According to Stephani et al. (2003), the metric (9) belongs to the type of spherically symmetric non-stationary metrics (see section 16.2 of the book by Stephani et al. 2003). Such a metric allows introduction of an isotropic comoving system of coordinates (equation 16.22 of section 16.2). Our modified Friedmann equations are derived for this system of coordinates. The metric of equation (9) can be considered as a combination of two metrics: the Schwarzschild metric and the FRW metric. In an essence, it is a modified FRW metric with a scalar perturbation function. In this section, we will write the Einstein equation for a general type of the b(t, r) function. In the specific case of b(t, r) = 2GM(t, r)/(rc2), we can hypothesize that the perturbation of the FRW metric is caused by a varying mass of a BBH, which is a final result of merging of many black holes and is located on the edge of the observed Universe. The centre of the coordinate system is located in the centre of the BBH, and we get a spherically symmetric physical system. But we prefer to explore this system in Cartesian coordinates. After we obtain the Friedmann equations for such a system, we can arbitrarily shift the initial point of coordinates. We will assume an approximation of weak fields, i.e. b(t, r) ≪ 1. That is why we will neglect non-linear combinations of this function. It should be noted that the time is not uniform in the Schwarzschild metric as it is the case in the FRW metric. We will neglect such non-uniformity of time because the non-uniformity of time is determined by the function 1 − b(t, r), which usually can be considered to be equal to unity. However, its derivatives should be accounted for in the derivation of the modified Friedmann equations. For the metric (9), we use the Einstein equations (1) without the term containing the cosmological constant. 4 THE MODIFIED FRIEDMANN EQUATIONS AND COSMOLOGICAL ACCELERATION Let us derive modified Friedmann equations for the metric (9). We assume that the dependence of a(t, r) on space coordinates is significantly weaker than that of b(t, r). This assumption allows us to neglect all derivatives of a(t, r) over the space coordinates as compared with those of b(t, r). We validate this assumption a posteriori in the discussion section. Details of the derivation are provided in Appendix A, here we give just the final equations. The presence of the function b(t, r) in the metric (9) results in a number of additional terms in the zero component of the Einstein equations. These terms contain second derivatives of the metric components over space coordinates. These additional terms can be considered as an effective ‘cosmological constant’, which can be called the ‘cosmological function’, Λ(t, r), because it depends on time and space. For the case of weak gravitational fields, b(t, r) ≪ 1, we get the first modified Friedmann equation in the form of \begin{equation} \left(\frac{\dot{a}}{a}\right)^{2}+\left(\frac{\dot{a}}{a}\right){\dot{b}}=\frac{{\Lambda (t,r)}c^{2}}{3}+\frac{8{\pi }G{\rho }}{3}, \end{equation} (10)where the cosmological function Λ(t, r) is given by the following expression: \begin{eqnarray} \Lambda (t,r)=\frac{1}{a^2}\left(\frac{\mathrm{\partial} ^2 b}{\mathrm{\partial} x_{\ast }^2}+\frac{\mathrm{\partial} ^2 b}{\mathrm{\partial} y_{\ast }^2}+\frac{\mathrm{\partial} ^2 b}{\mathrm{\partial} z_{\ast }^2}\right)=\left(\frac{\mathrm{\partial} ^2 b}{\mathrm{\partial} x^2}+\frac{\mathrm{\partial} ^2 b}{\mathrm{\partial} y^2}+\frac{\mathrm{\partial} ^2 b}{\mathrm{\partial} z^2}\right).\nonumber \\ \end{eqnarray} (11)We use a Cartesian system of coordinates only. The variable r is not a coordinate; it is a distance between an observer and the BBH, which is calculated as $$r = \sqrt{x^2+y^2+z^2}$$, for example, Landau and Lifshitz (1975). The r distance is actually a parameter that defines a value of the BBH perturbation at a given location. It should be noted that the cosmological constant that depends on time was considered in, for example, Weinberg (1989) and Szydlowski and Stachowski (2015). Inhomogeneous cosmological models with the scalefactor a, which depends on space coordinates, were considered in numerous papers (Tolman 1934, 1969; Zel'dovich and Grishchuk 1984; Bolejko et al. 2011). It is useful to note that the equation (11) is derived for a general form of the disturbing function b(t, r). The scalar cosmological function Λ(t, r) should not depend on a coordinate system. That is why we can calculate the cosmological function in any coordinate system: either comoving coordinates or physical coordinates of the fixed system of coordinates. A similar equation for a disturbed metric was earlier derived, for example, by Dodelson (2003, see equation 5.27) for density perturbations. In our case, the perturbation is related to a varying gravitational mass of the system. Note the difference between equation (5.27) of Dodelson (2003) and our equation (10). Equation (5.27) of Dodelson (2003) is written only for the perturbed quantities, and the zero-level approximation (the Friedmann equation for a(t)) is split off. We do not decompose the equation (10) into two approximation. The smallness of function b(t, r) does not mean that the terms with b(t, r) will be smaller than terms with large fraction a(t, r). In case of exponential change of the gravitational mass (3), we get from equation (11) for α ≫ c/r \begin{equation} \Lambda (t,r)\approx \frac{\alpha ^{2}}{c^{2}}b(t,r)=\frac{\alpha ^{2}}{c^{2}}\frac{2GM(t,r)}{rc^{2}}=\frac{\alpha ^{2}}{c^{2}}\frac{r_{0}}{r}, \end{equation} (12)where the Schwarzschild radius r0 = 2GM(t, r)/c2. It is logical to relate the α parameter to the time of the Universe existence after the Big Bang, T: α = f/T, where f is the dimensionless coefficient. f = 1 means that the BBH mass has changed by e times since the Big Bang. Using the cosmological time, we get from equation (12): \begin{equation} \Lambda (t,r)=\frac{f^{2}}{c^{2}T^{2}}\frac{r_{0}}{r} \approx 0.7 \times 10^{-56}f^{2}\frac{r_{0}}{r} \end{equation} (13)(in cm− 2), where T ≈ 4 × 1017 s. It should be noted that the term $$\frac{\dot{a}}{a}\dot{b}$$ in equation (10) is proportional to the exponent α, whereas term Λ(t, r)c2/3 is proportional the squared exponent α2. In the case of fast change of the gravitational mass, i.e. f 2 ≫ f or f ≫ 1, the term $$\frac{\dot{a}}{a} \dot{b}$$ can be neglected and equation (10) concurs with the classical Friedman equation (6), where the cosmological constant is replaced by the cosmological function (11). The second modified Friedmann equation is derived by differentiating equation (10) over time (for more details, see Appendix A): \begin{equation} \frac{\ddot{a}}{a}=\frac{\Lambda (t,r)c^{2}}{3}+\frac{8{\pi }G{\rho }}{3}-\frac{\ddot{b}}{2}+ \frac{\frac{{\dot{\Lambda }(t,r)}c^{2}}{6}+\frac{4{\pi }G{\dot{\rho }}}{3}}{\sqrt{\frac{\Lambda (t,r)c^{2}}{3}+\frac{8{\pi }G{\rho }}{3}}}. \end{equation} (14)The quantity ρ is the mean density of the observed Universe, whereas the terms with Λ(t, r) and b̈ depend on a varying gravitational mass of the BBH located near the observed horizon. Using equation (12), we get $$\ddot{b}= \Lambda (t,r)c^{2}$$. Then equation (14) can be rewritten as \begin{equation} \frac{\ddot{a}}{a}=-\frac{\Lambda (t,r)c^{2}}{6}+\frac{8{\pi }G{\rho }}{3}+ \frac{\frac{{\dot{\Lambda }(t,r)}c^{2}}{6}+\frac{4{\pi }G{\dot{\rho }}}{3}}{\sqrt{\frac{\Lambda (t,r)c^{2}}{3}+\frac{8{\pi }G{\rho }}{3}}}. \end{equation} (15) The second modified Friedmann equation is quite similar to the classical equation (7), where the cosmological function Λ(t, r) is given by (11). Let us consider the case when the term with the cosmological function dominates the term with mean density of the Universe. Assuming an exponential change of the mass of the BBH (3), we get $$\dot{\Lambda }(t,r)=\alpha \Lambda (t,r)$$. Then, equation (15) transforms into the following equation: \begin{equation} \frac{\ddot{a}}{a}=-\frac{\Lambda (t,r)c^{2}}{6}-\frac{\alpha }{2}\sqrt{\frac{\Lambda (t,r)c^{2}}{3}}. \end{equation} (16) Using equation (10), we get $$\Lambda (t,r)c^{2}=3(H^{2}+H\dot{b})$$, where $$H=\frac{\dot{a}}{a}$$ is the Hubble constant. Then, equation (16) can be rewritten as follows: \begin{equation} \frac{\ddot{a}}{a}=-\frac{1}{2}(H^{2}+H\dot{b}+{\alpha }\sqrt{H^{2}+H\dot{b}})\approx -\frac{1}{2}(H^{2}+{\alpha }H). \end{equation} (17)When we write the approximate expression, we assume that we can neglect the term $$H\dot{b}$$ as compared with others. It follows from equation (17) that acceleration for a comoving observer is positive $$\ddot{a}>0$$ if α < −H, that there is sufficiently fast increase of the gravitational mass of the BBH. It follows from equation (12) that the second term in the second Friedmann equation (16) depends on the distance to the BBH as a square root: $$\sqrt{\Lambda (t,r)c^{2}/3} \propto \sqrt{r_{0}/r}$$. The weaker dependence on the distance as compared with the first term results in prevailing the second term on large distances over the first term thus determining the dynamics of expanding of the Universe. 5 DISCUSSION Equation (13) shows that the cosmological function is expressed through a dimensionless quantity f 2r0/r composed of two parameters of our model f and r0/r. The cosmological function is equal to the observed value of the cosmological constant (2) if \begin{equation} f^{2} \frac{r_{0}}{r} \approx 1.6. \end{equation} (18)Our basic assumption of weak gravitational fields means that r0/r ≪ 1, i.e. an observer is located far away from the BBH. Then, $$f \gg \sqrt{1.6} \approx 1.3$$. Assuming that a value of f ∼ 10, we get from (18) the following estimate r0/r ∼ 0.02. If we assume that the distance, r ∼ 50 billion light-years, i.e. the size of the Universe by the order of the magnitude (Davis and Lineweaver 2004), we get the following estimate of the radius of the BBH: r0 ∼ 1 billion light-years. This radius corresponds to the mass of the BBH of ∼6 × 1054 gm. Using equation (18), we can now validate our assumption of negligibly small derivatives of a(t, r) over space coordinates as compared with those of b(t, r), that is, \begin{equation} b^{\prime \prime } \gg a^{\prime \prime } \ {{\rm and}}\ b^{\prime \prime } \gg b^{\prime } a^{\prime }, \end{equation} (19)where the prime denotes a derivative over a space coordinate. The relationships of equation (19) can be estimated as follows: \begin{equation} \left(\frac{\alpha }{c}\right)^2 \frac{r_0}{r}\gg \frac{1}{r^2}\ {\rm and}\ \left(\frac{\alpha }{c}\right)^2 \frac{r_0}{r}\gg \frac{\alpha }{c} \frac{r_0}{r}\frac{1}{r}. \end{equation} (20)Substituting equation (18) into equation (20), we obtain the following estimates: \begin{equation} \frac{1.6}{(cT)^2}\gg \frac{1}{r^2} \ {\rm and}\ \frac{f}{cT} \gg \frac{1}{r}\ {\rm or}\ {\alpha } \gg \frac{c}{r}. \end{equation} (21)The conditions of equation (21) are satisfied for r ∼ 50 billion light-years (a size of the Universe) and f = 10. There is an idea that a fraction of the black holes survives the stage of maximal contracting of the universe (Clifton et al. 2017). These relict black holes can produce the supermassive black holes in the galaxy centres and are responsible for the effects of ‘dark matter’. This idea is in a qualitative agreement with our assumption about the existence of the BBH. The first Friedmann equation (6) characterizes an isotropic and homogeneous model of the Universe. All locations of an observer are equivalent. It can be shown (McVittie 1956) that galaxies move away from each other similarly in all comoving coordinate systems with the same expansion rate defined by the Hubble constant. The modified Friedman equations with the cosmological function (11) are derived for two combined metrics: the basic FRW metric and the additional modified Schwarzschild metric. These metrics are considered in a single system of coordinates. If an observer moves to another coordinate system, the traditional terms of the Friedmann equations should not change; they are derived for the classical isotropic and homogeneous universe. However, the cosmological function Λ(t, r) should change because it depends on a distance, r, from the origin of the Schwarzschild system of coordinates. The Schwarzschild metric is a kind of the anisotropic background for the shifted observer. Comparing the modified Friedmann equations with the classical ones, we conclude that the modified equations are valid for an observer at any location. However, the new cosmological term that depends on the distance from the BBH thus changes when the observer moves from one location to another. Thus, positive relative acceleration of observable galaxies is result of difference in deceleration of galaxies in non-stationary gravitational field of the BBH. This paper is devoted to a mathematical solution of the Einstein equations for an expanding universe with a varying gravitational mass. This solution allows us to generalize the Friedmann equations for the varying gravitational mass. A consideration of observational cosmological aspects (CMB spectra, generation of large structures of the Universe, etc.) is beyond of the scope of this work. 6 CONCLUSIONS We generalized the Friedmann equations for a model of the Universe with a varying gravitational mass. We managed to derive an expression for the cosmological constant directly from the Einstein equations. The model leads to the following conclusions: The modified Friedmann equation is equivalent to the classical Friedmann equations when the perturbation b(r, t) → 0. This allows us to suggest that the modified Friedmann equations do not contradict to all observational cosmological effects. A major distinction of the modified Friedmann equations from the classical equations is that the modified equations give us an expression for the cosmological constant based on physical quantities that is derived from the Einstein equations. Estimates of the cosmological constant based on this expression give values that are quantitatively close to the observed value. The cosmological principle of isotropy and homogeneity of the Universe is not universal. The Universe is isotropic and homogeneous locally only. Possible effects of anisotropy and inhomogeneity of the Universe can be observable for distant objects. A disturbance of the FRW metric is caused by a very BBH located near the observed horizon of the Universe. The disturbance of the FRW metric results in an effective cosmological constant in the modified Friedmann equations. This effective cosmological constant is analogous to the dark energy term in the classical Friedmann equations. Estimates of this effective cosmological constant show that its value is close to observed cosmological constant by the order of magnitude, provided reasonable assumptions about the dimensionless parameters of the model have been made. The observed positive acceleration of the expansion of the Universe corresponds to an increase of the gravitational mass of the BBH. In the future, this increase of the BBH can stop the expansion of the Universe and cause its collapse. We believe that a cyclic model of Universe can be developed on the basis of cyclic transformation of black holes, baryons, and electromagnetic and gravitation radiation. Our conclusions are supported by a few observations that are related to anisotropic and inhomogeneous effects in cosmology (Erickcek, Carrol & Kamionkovski 2008; Stavrinos, Kouretsis & Stathakopoulos 2008; Hoftuft et al. 2009; Javanmardi et al. 2015; Zhao and Santos 2016; Ade et al. 2016b; Riess et al. 2016; Schwarz et al. 2016; Colin et al. 2017). Besides that, a change of the gravitational mass of the Universe could be verified by observations of the monopole component of non-stationary gravitational field. What would be the waveform of the monopole component, accompanying the detected transverse gravitational waves (Abbot et al. 2016)? 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S., 1934, PNAS , 20, 169 https://doi.org/10.1073/pnas.20.3.169 CrossRef Search ADS PubMed Tolman R. S., 1969, Relativity, Thermodynamics and Cosmology . Clarendon Press, Oxford Tourrenc Ph., 1997, Relativity and Gravitation . Cambridge Univ. Press, Cambridge Weinberg S., 1972, Gravitation and Cosmology . Wiley, New York Weinberg S., 1989, Rev. Mod. Phys. , 61, 1 https://doi.org/10.1103/RevModPhys.61.1 CrossRef Search ADS Zel'dovich Ya.B., Grishchuk L. P., 1984, MNRAS , 207, 23P https://doi.org/10.1093/mnras/207.1.23P CrossRef Search ADS Zhao W., Santos L., 2016, preprint (arXiv:1604.05484) APPENDIX A: DERIVATION OF THE MODIFIED FRIEDMANN EQUATIONS Let us consider the Einstein equations (1) without the cosmological constant and derive the Friedmann equations for the disturbed FRW metric (9) with a function b(t, r) assumed to be small. Thus, we neglect all the products of the Christoffel symbols that are proportional to the squared function b(t, r). Elsewhere, we also neglect all terms that contain a non-linear combination of b(t, r). The zero component of the Einstein equations is \begin{equation} R_{00}-\frac{1}{2}g_{00}R=-\frac{8 \pi G}{c^{4}}T_{00}. \end{equation} (A1)We can get the following expression for the zero-index component of the left-hand side of the Einstein equations (1) (see chapter 100 in Tolman 1969) : \begin{eqnarray} &&{ R_{00}-\frac{1}{2}g_{00}R = -\left(\frac{1}{2g_{11}}\frac{\mathrm{\partial} g_{11}}{c\mathrm{\partial} t}\right) \left(\frac{1}{2g_{22}}\frac{\mathrm{\partial} g_{22}}{c\mathrm{\partial} t}\right)} \nonumber\\ &&- \left(\frac{1}{2g_{11}}\frac{\mathrm{\partial} g_{11}}{c\mathrm{\partial} t}\right) \left(\frac{1}{2g_{33}}\frac{\mathrm{\partial} g_{33}}{c\mathrm{\partial} t}\right)- \left(\frac{1}{2g_{22}}\frac{\mathrm{\partial} g_{22}}{c\mathrm{\partial} t}\right) \left(\frac{1}{2g_{33}}\frac{\mathrm{\partial} g_{33}}{c\mathrm{\partial} t}\right) \nonumber\\ &&- g_{00}\left(\frac{1}{2g_{11}g_{22}}\frac{\mathrm{\partial} ^2 g_{22}}{\mathrm{\partial} x_{\ast }^2} +\frac{1}{2g_{11}g_{33}}\frac{\mathrm{\partial} ^2 g_{33}}{\mathrm{\partial} x_{\ast }^2}+ \frac{1}{2g_{11}g_{22}}\frac{\mathrm{\partial} ^2 g_{11}}{\mathrm{\partial} y_{\ast }^2}\right. \nonumber\\ &&+ \left. \frac{1}{2g_{22}g_{33}}\frac{\mathrm{\partial} ^2 g_{33}}{\mathrm{\partial} y_{\ast }^2}+ \frac{1}{2g_{11}g_{33}}\frac{\mathrm{\partial} ^2 g_{11}}{\mathrm{\partial} z_{\ast }^2}+ \frac{1}{2g_{22}g_{33}}\frac{\mathrm{\partial} ^2 g_{22}}{\mathrm{\partial} z_{\ast }^2}\right). \end{eqnarray} (A2) A combination of the second derivatives in (A2) is an effective cosmological constant, which can be named as the ‘cosmological function’ because it depends on time and spatial coordinate: \begin{eqnarray} \Lambda (t,r)&=&\frac{1}{2g_{11}g_{22}}\!\frac{\mathrm{\partial} ^2 g_{22}}{\mathrm{\partial} x_{\ast }^2} \!+\!\frac{1}{2g_{11}g_{33}}\frac{\mathrm{\partial} ^2 g_{33}}{\mathrm{\partial} x_{\ast }^2}\!+\! \frac{1}{2g_{11}g_{22}}\frac{\mathrm{\partial} ^2 g_{11}}{\mathrm{\partial} y_{\ast }^2} \nonumber\\ &&+ \frac{1}{2g_{22}g_{33}}\!\frac{\mathrm{\partial} ^2 g_{33}}{\mathrm{\partial} y_{\ast }^2}\!+\! \frac{1}{2g_{11}g_{33}}\frac{\mathrm{\partial} ^2 g_{11}}{\mathrm{\partial} z_{\ast }^2}\!+\! \frac{1}{2g_{22}g_{33}}\!\frac{\mathrm{\partial} ^2 g_{22}}{\mathrm{\partial} z_{\ast }^2}. \end{eqnarray} (A3)It should be noted that g00 ≈ −1 in our approximation. Equalling (A2) to the zero-index component of the energy-momentum tensor, we get the following expression: \begin{equation} 3\left[\left(\frac{\dot{a}}{a}\right)^{2}+\frac{\dot{a}}{a}\dot{b}\right]={\Lambda (t,r)}c^2+8{\pi }G{\rho }. \end{equation} (A4)The terms on the left-hand side of equation (A4) are derived from the products of the derivatives over time in (A2). The additional term with $$\dot{b}$$ is significant at differentiating equation (A4) over time to derive the second Friedman equation. Solving equation (A4) with respect to the ratio, $$\frac{\dot{a}}{a}$$, we get the following expression: \begin{equation} \frac{\dot{a}}{a}=\pm \sqrt{\frac{\Lambda (t,r)c^{2}}{3}+\frac{8{\pi }G{\rho }}{3}+\frac{\dot{b}^2}{4}}-\frac{\dot{b}}{2}. \end{equation} (A5)The upper sign in equation (A5) and elsewhere corresponds to the case of an expanding universe (the Hubble constant is positive), and the bottom sign corresponds to a collapsing universe (the Hubble constant is negative). Squaring (A5), we get the first modified Friedmann equation: \begin{eqnarray} \left(\frac{\dot{a}}{a}\right)^{2}\!=\!\frac{\Lambda (t,r)c^{2}}{3}\!+\!\frac{8{\pi }G{\rho }}{3}\!+\!\frac{\dot{b}^2}{2} \mp \dot{b} \sqrt{\frac{\Lambda (t,r)c^{2}}{3}\!+\!\frac{8{\pi }G{\rho }}{3}\!+\!\frac{\dot{b}^2}{4}}.\nonumber\\ \end{eqnarray} (A6)To get the second modified Friedmann equation, let us differentiate equation (A5) with respect to time. Then, using equation (A6) we get the second modified Friedmann equation: \begin{eqnarray} \!\frac{\!\ddot{a}}{a}&=& \!\!\frac{\Lambda c^{2}}{3}\!+\!\!\frac{8{\pi }G{\rho }}{3}\!+\!\!\frac{\dot{b}^2\!-\!\ddot{b}}{2}\!\mp \!\frac{\!\frac{c^2}{3}(\dot{b} \Lambda \!-\!\frac{\dot{\Lambda }}{2})\!+\!\frac{8\pi G}{3}(\dot{b} \!\rho \!-\!\frac{\dot{\rho }}{2})\!+\!\frac{\dot{b}}{4}(\dot{b}^2\!-\!\ddot{b})}{\!\sqrt{\!\frac{\!\Lambda c^{2}}{3}\!+\!\frac{8{\pi }G{\rho }}{3}\!+\!\frac{\!\dot{b}^2}{4}}}.\nonumber\\ \end{eqnarray} (A7) For weak gravitational fields b(t, r) ≪ 1, we can neglect all terms with $$\dot{b}$$ and b̈ except for the term $$-\ddot{b}/2$$. In this approximation, we get the second modified Friedmann equation in the form of equation (14) that is provided in the main text. © 2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society

Monthly Notices of the Royal Astronomical Society – Oxford University Press

**Published: ** May 1, 2018

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