Issue 
A&A
Volume 529, May 2011



Article Number  A26  
Number of page(s)  14  
Section  Cosmology (including clusters of galaxies)  
DOI  https://doi.org/10.1051/00046361/201016057  
Published online  23 March 2011 
A conventional approach to the darkenergy concept
^{1}
Department of Mechanical EngineeringTechnological Education Institute of Serres, 621.24 Serres, Greece
email: kleidis@teiser.gr
^{2}
Department of Astronomy, Aristoteleion University of Thessaloniki, 541.24 Thessaloniki, Greece
email: spyrou@astro.auth.gr
Received: 3 November 2010
Accepted: 14 January 2011
Motivated by results implying that the constituents of dark matter (DM) might be collisional, we consider a cosmological (toy) model, in which the DM itself possesses some sort of thermodynamic properties. In this case, not only can the matter content of the Universe (the baryonic component, which is tightly gravitationallybounded to the dark one, also being included) be treated as a classical gravitating fluid of positive pressure, but, together with all its other physical characteristics, the energy of this fluid’s internal motions should be taken into account as a source of the universal gravitational field. In principle, this form of energy can compensate for the extra (dark) energy, needed to compromise spatial flatness, while the postrecombination Universe remains everdecelerating. What is more interesting, is that, at the same time (i.e., in the context of the collisionalDM approach), the theoretical curve representing the distance modulus as a function of the cosmological redshift, μ(z), fits the Hubble diagram of a multiused sample of supernova Ia events quite accurately. A cosmological model filled with collisional DM could accommodate the majority of the currentlyavailable observational data (including, also, those from baryon acoustic oscillations), without the need for either any dark energy (DE) or the cosmological constant. However, as we demonstrate, this is not the case for someone who, although living in a Universe filled with selfinteracting DM, insists on adopting the traditional, collisionlessDM approach. From the point of view of this observer, the cosmologicallydistant lightemitting sources seem to lie farther (i.e., they appear to be dimmer) than expected, while the Universe appears to be either accelerating or decelerating, depending on the value of the cosmological redshift. This picture, which, nowadays, represents the common perception in observational cosmology, acquires a more conventional interpretation within the context of the collisionalDM approach.
Key words: dark matter / dark energy
© ESO, 2011
1. Introduction
The beginning of the 21st century was one of the most exciting epochs for cosmology as a science. According to observational data on the temperature variations in the cosmic microwave background (CMB) that became in public at that epoch (de Bernardis et al. 2000; Jaffe et al. 2001; Padin et al. 2001; Stompor et al. 2001; Netterfield et al. 2002), now, we are quite confident that the Universe can be adequately described by a spatially flat RobertsonWalker (RW) cosmological model.
As a consequence, the total energy density, ε, of the Universe matterenergy content, in units of the energy density ε_{c} = ρ_{c}c^{2} (equivalent to the critical restmass density, , where H_{0} is the Hubble parameter at the present epoch, c is the velocity of light, and G is Newton’s universal constant of gravitation), should be very close to unity, , i.e., much larger than the measured quantity, (Komatsu et al. 2009).
At the same time, highprecision distance measurements, performed with the aid of the supernovae Ia (SNe Ia) standard candles, indicated that, in any cosmological model with vanishing cosmological constant, Λ, the faroff lightemitting sources appear to be dimmer than expected (Riess et al. 1998; Perlmutter et al. 1999).
The observational data then seemed to favour a Universe of collisionless content (i.e., filled with matter in the form of dust) and Λ ≠ 0, in which Ω_{M} ≃ 0.3 and (Riess et al. 2001, 2004). Since a nonvanishing cosmological constant (necessarily) involves a repulsive (gravitational) force (see, e.g., Sahni 2004), the apparent dimming of the distant lightemitting sources was attributed to a relatively recent phase of accelerated expansion (see, e.g., Linder 2008).
The onset of the dimming of the cosmologically distant indicators used (hence, the associated transition from acceleration to deceleration), takes place at a relatively low value of the cosmological redshift, z, the socalled transition redshift, z_{t}, which, nowadays, is being (observationally) set at z_{t} = 0.46 ± 0.13 (Riess et al. 2004, 2007). In this case, the cosmological constant can be determined observationally, since, on theoretical grounds, (see, e.g., Perivolaropoulos 2007, Eq. (21)), i.e., the transition redshift depends on the value of Λ. The particlephysics vacuum does contribute an effective cosmological constant, which could serve (also) as compensation to the extra energy needed to flatten the Universe (Sahni & Starobinsky 2000). Unfortunately, the energydensity attributed to such a source is 10^{123} times larger than what is observed (see, e.g., Padmanabhan 2003; Sahni 2004).
Hence, it became evident that, for the abovementioned observational results to be reconciled within a unified theoretical framework, a different approach (i.e., other than the cosmological constant) was needed.
In this context, theorists have focused on two main areas: (i) the introduction of an exotic, negativepressure fluid, the dark energy (Caldwell et al. 1998), occasionally referred to as quintessence (Carroll 1998); and (ii) the consideration of alternativegravity theories, such as the scalartensor theories (EspositoFarese & Polarski 2001) and the f(R)gravity (Capozziello et al. 2003), together with several braneworld scenarios, including DGPgravity (Dvali et al. 2000) and the landscape scenario (Bousso & Polchinski 2000).
Other physicallymotivated models, predicting an accelerated expansion, have also appeared in the literature, involving holographic gravity (Cohen et al. 1999; Li 2004; Pavón & Zimdahl 2005), Chaplygin gas (Kamenshchik et al. 2001; Bean & Doré 2003; Sen & Scherrer 2005), Cardassian cosmology (Freese & Lewis 2002; Wang et al. 2003), theories of compactified internal dimensions (Perivolaropoulos 2003), and massvarying neutrinos (Fardon et al. 2004; Peccei 2005).
However, most of these attempts were inhibited by the socalled coincidence problem, i.e., the need to explain why the Universe transferred from deceleration to acceleration so recently (see, e.g., Perivolaropoulos 2007).
It has been more than a decade since the first observations, which provoked the aforementioned scientific (r)evolution, became in public, and, still, no undisputed theoretical framework has been developed to accommodate them (for a detailed review see, e.g., Caldwell & Kamionkowski 2009). In the meantime, the need for an extra (dark) energy component has been confirmed by other observational methods, including galaxy clusters dynamics (Allen et al. 2004), the integrated SachsWolfe (ISW) effect (Boughn & Crittenden 2004), and baryon acoustic oscillations (BAO) (Eisenstein et al. 2005; Percival et al. 2010). In spite of the wealth of references, previous studies have been far from exhaustive (see, e.g., Albrecht et al. 2006; Peacock et al. 2006) and, perhaps, we should keep our options open, also, to more conventional interpretations (see, e.g., Buchert 2000, 2001; Kolb et al. 2006; Celerier 2007; Ellis 2009).
On the other hand, much evidence has already been accumulated in support of a (nonbaryonic) DM component in the Universe mattercontent (see, e.g., Tegmark et al. 2006; Spergel et al. 2007). Among other pieces of evidence, this support includes flattened galactic rotation curves (Begeman et al. 1991; Borriello & Salucci 2001), the weak gravitational lensing of distant galaxies by (some dark) foreground structure (Hoekstra et al. 2002), and the weak modulation of strong lensing around individual massive elliptical galaxies (Moustakas & Metcalf 2003). On the scale of galaxy clusters, observations (of radial velocities, weak lensing, and Xray emission) indicate a total mass density almost ten times higher than the corresponding density in baryons (Bahcall & Fan 1998; Kashlinsky 1998; Tyson et al. 1998). On cosmological scales, the anisotropies observed in the CMB have led to an estimate of the totalmass density of the order of Ω_{M}h^{2} = 0.1358 ± 0.0037, where h is the Hubble parameter in units of 100 km s^{1} Mpc^{1} (Komatsu et al. 2009). In contrast, measurements of the lightchemicals’ abundances (Olive et al. 2000) have led to an estimate of the baryonicmass density of the order of Ω_{B}h^{2} = 0.02273 ± 0.00062. The combination of these results suggests that, more than 85% (by mass) of the matter in the Universe consists of nonluminous and nonbaryonic material.
Although we do not know for certain how the DM came to be formed, a sizeable relic abundance of weaklyinteracting massive particles (WIMPs) is generally expected to have been produced as a byproduct of the Universe’s hot youth (see, e.g., Kolb & Turner 1990, p. 369). These particles decouple from radiation much earlier than purebaryonic matter does. Hence, very soon after recombination (t_{R}), the baryons fall into deep potential wells of the already evolved DMperturbations and become bounded to them, i.e., for t > t_{R}, there are no freelyfloating baryons around (Olive 2003).
Among the various candidates for DM constituents, the thermal WIMPs remain one of the most attractive. They appear, generically, in theories of weakscale physics beyond the standard model, while giving the appropriate relic abundance (Srednicki et al. 1988; Gondolo & Gelmini 1991). These particles are also helpful to consider in terms of direct and indirect detection of DM (see, e.g., Jungman et al. 1996; Bertone et al. 2005), because they must have some connection to standardmodel particles (see, e.g., Hooper 2009). In addition to debating their precise nature, the scientific community used to argue that the WIMPs should be collisionless.
However, many results from highenergy particle detectors, such as the ATIC (Chang et al. 2008) and PAMELA (Adriani et al. 2009), combined with data from the Wilkinson microwave anisotropy probe (WMAP) survey (Hooper et al. 2007), have revealed an unusually high electronpositron production in the Universe, much more than anticipated by SNe explosions or cosmicray collisions. These results have led many scientists to argue that among the best candidate sources of these highenergy events are the annihilations of WIMPs (see, e.g., Barger et al. 2008; Bergstrom et al. 2008; Cirelli & Strumia 2008; Regis & Ullio 2008; Baushev 2009; Cholis et al. 2009a,b; Fornasa et al. 2009; Fox & Poppitz 2009; Kane et al. 2009; Zurek 2009, for an extensive, though incomplete list), i.e., that the DM constituents can be slightly collisional (see, e.g., Spergel & Steinhardt 2000; ArkaniHamed et al. 2009; Cirelli et al. 2009; Cohen & Zurek 2010), although, some studies disagree with this interpretation (see, e.g., Feng et al. 2010).
A cosmological model filled with selfinteracting DM could be a relatively inexpensive solution to the DE problem, and, several ways of accommodating both the DM and the DE into a unified theoretical framework have been considered (see, e.g., Zimdahl et al. 2001; Bilić et al. 2002; Balakin et al. 2003; Scherrer 2004; Lima et al. 2008; Basilakos & Plionis 2009, 2010; Dutta & Scherrer 2010). In this context, we suggest that, phenomenologically, the selfinteracting DM could attribute to the Universe mattercontent some sort of fluidlike properties, and (so) lead to a conventional approach to the DE concept.
The main outstanding problem of the current cosmological picture is that the Universe must contain an amount of energy that is considerably higher than the equivalent of the total restmass of its matter content. However, if the DM constituents collided with each other frequently enough, enabling their (kinetic) energy to be redistributed, i.e., if the DM itself possessed some sort of thermodynamic properties, a conventional extraenergy component might be present in the Universe, given by the energy of the internal motions of the collisionalDM fluid.
On this basis, it is worth examining the evolution and the dynamical characteristics of a cosmological model (not necessarily reflecting our own Universe), in which (in principle) there is no DE at all. The matterenergy content of this model consists solely of two components, i.e., the DM (dominant) and the baryonic one (subdominant), both having the abundances attributed to them by analyses of the fiveyear survey of the WMAP (Dunkley et al. 2008; Komatsu et al. 2009). Accordingly, we demonstrate that these two components are (by themselves) sufficient (i) to reproduce the result that (today) Ω = 1; (ii) to account for the observed dimming of the distant lightemitting sources; and (iii) to explain the apparent accelerated expansion of the Universe. All the above provided that, macroscopically, these two constituents (basically the dark one) form a gravitating fluid with a thermodynamical content. In this case, together with all the other physical characteristics, the energy of this fluid’s internal motions should (also) be taken into account as a source of the universal gravitational field. Although speculative, the idea that the extra (dark) energy needed to flatten the Universe could be attributed to the internal motions of a collisionalDM fluid is (at least) intriguing.
This paper is organized as follows. In Sect. 2, we explore the dynamical characteristics of a cosmological model driven by an ideal fluid, consisting (mainly) of (thermodynamicallyinvolved) DM, with positive pressure, the volume elements of which perform adiabatic flows. Accordingly, after deriving the corresponding scale factor, we determine the functional form of several parameters of cosmological significance, each one depending on the cosmological redshift, such as the luminosity distance and the distance modulus of the cosmologicallydistant lightemitting sources, together with the Hubble and the deceleration parameters, which characterize the cosmic expansion. The corresponding results suggest that, in the context of the collisionalDM treatment, the extra (dark) energy (needed to compromise spatial flatness) can be compensated by the energy of the internal motions of this fluid, while, the postrecombination Universe remains everdecelerating. However, as we demonstrate in Sect. 3, this is not the case for someone who (although living in a Universe filled with collisional DM) insists on adopting the traditional (collisionlessDM) approach. From the point of view of this observer, besides the need for an extraenergy component (for confronting the CMBbased observational results), the cosmologicallydistant lightemitting sources seem to lie farther (i.e., they appear to be dimmer) than expected, while the Universe appears to be either accelerating or decelerating, depending on the value of the cosmological redshift. Finally, we conclude in Sect. 4.
2. A Universe filled with collisional dark matter
It is generally accepted that the study of the CMB has proven to be a powerful tool in exploring the postrecombination Universe. According to the various CMBoriented observational data, the Universe has emerged out of the radiation epoch as a spatiallyflat RW model (see, e.g., de Bernardis et al. 2000) (1)where η is the conformal time and S(η) is the scale factor. As a consequence, the value of the Hubble parameter at the present epoch is, by definition, given by (2)(see, e.g., Peacock 1999, p. 77). The evolution of this model depends on the nature of the source that drives the universal gravitational field, i.e., its matterenergy content.
Along the lines of the collisionalDM approach, in specifying the Universe matterenergy content, we assume that, in principle, there is no DE at all. Instead, we admit that the DM, together with the small, baryonic “contamination” (the latter is too tightly gravitationallybounded to the former), possess fluidlike properties. In this sense, the collisions of the WIMPs maintain a tight coupling between them and their energy can be redistributed, i.e., the DM itself also possesses some sort of thermodynamical content. In this case, the evolution of the postrecombination Universe is no longer driven by dust, but, by a gravitating fluid of positive pressure, p, satisfying the equation of state (3)where ρ is the restmass density (the part, equivalent to the energy density ρc^{2}, that remains unaffected by the internal motions of the cosmic fluid) and is a dimensionless constant, which measures the square of the speed of sound, c_{s}, in units of c^{2}. Now, the fundamental units of the Universe mattercontent are the volume elements of the collisionalDM fluid (elements of fluid, each one consisting always of the same particles).
The motions of the volume elements in the interior of a continuous medium are governed by the equations (4)where Greek indices refer to the fourdimensional spacetime (in connection, Latin indices refer to the threedimensional spatial slices), the semicolon denotes covariant derivative, and T^{μν} is the energymomentum tensor of the Universe mattercontent, i.e., basically (but not solely), of the collisionalDM fluid.
Confining ourselves to the particular case of a perfect fluid, T^{μν} takes on the standard form (5)where u^{μ} = dx^{μ}/ds is the fourvelocity (u_{μ}u^{μ} = 1) at the position of a fluid’s volume element, g^{μν} are the contravariant components of the Universe metric tensor, and ε is this fluid’s totalenergy density. In an (ideal) equilibrium state, i.e., in the absence of shear, viscocity and heat conductivity, ε is decomposed to (6)(for a detailed analysis see, e.g., Fock 1959, pp. 81 − 83 and 91 − 94), where Π is the potential energy per unit restmass, associated with the infinitesimal deformations (expansions or/and compressions) of the fluid. Upon consideration of adiabatic processes, Π coincides with the energy of this fluid’s internal motions (per unit restmass), thus defining ρΠ as the corresponding energy density, associated with the thermodynamical content of the (collisional) DM.
Along these lines, the equations represented by Eq. (4) are the hydrodynamic flows of the volume elements in the interior of a perfectfluid source (7)where the comma denotes a partial derivative and is the Kronecker symbol. The equations given in Eq. (7) can be cast in the more convenient form (8)where are the Christoffel symbols corresponding to the Universe metric tensor, g_{μν}, and h^{κλ} = g^{κλ} − u^{κ}u^{λ} is the projection operator.
However, in a maximally symmetric cosmological setup, there is no real difference between hydrodynamic flows and the ballistic motions along the (nonintersecting) geodesic trajectories x^{μ} = const., since the equations of motion given by Eq. (8) are trivially satisfied by the fluid’s volume elements with u^{μ} = (1,0,0,0). In other words, in comoving coordinates, both sides of Eq. (8) vanish identically, resulting in the geodesic equations (9)and the equations of the ballistic trajectories (10)Notice however that, in this case, Eq. (10) is satisfied only because of the form of the metric tensor in Eq. (1), i.e., even if p_{,λ} does not vanish. Hence, in comoving coordinates, the geodesic motions and the hydrodynamic flows of the cosmological model given by Eq. (1) are, practically, indistinguishable. Therefore, a comoving observer of the cosmic expansion also traces the hydrodynamic flow of the homogeneous cosmic fluid and the Weyl’s postulate is valid (see, e.g., Narlikar 1983, p. 91).
As a consequence, the dynamical evolution of the model given by Eq. (1) is governed by the Friedmann equation (with Λ = 0) of the classical FriedmannRobertsonWalker (FRW) cosmology (11)where (12)is the Hubble parameter as a function of the scale factor, and the prime denotes differentiation with respect to η.
Nevertheless, inherently, there is an essential difference between our model and the rest of the classical FRW cosmologies. In our case, the basic matter constituents (although they may resemble test particles receding from each other) are the volume elements of a collisionalDM fluid, i.e., they possess some sort of internal structure, hence thermodynamical content. Therefore, the functional form of ε in Eq. (11) is no longer given by ρc^{2} alone, but by Eq. (6) (see also Narlikar 1983, pp. 61, 62).
In this model, the first law of thermodynamics for adiabatic flows, given by, (13)(see, e.g., Chandrasekhar 1965), results in (14)where the constants ρ_{0} and Π_{0} are assumed to denote the corresponding presenttime values. Accordingly, the totalenergy density of the Universe matterenergy content is written in the form (15)On the other hand, for every value of w, the conservation law , in terms of the metric tensor of Eq. (1), yields (16)which, upon consideration of Eqs. (3) and (6), results in (17)where S_{0} is the value of S(η) at the present epoch. Equation (17) represents the conservation of the total mass in a cosmological model in which matter dominates, i.e., for every η within the postrecombination epoch (see, e.g., Tsagas et al. 2008).
With the aid of Eqs. (15) and (17), Eq. (11) is written in the form (18)Now, combining Eqs. (2) and (18), we obtain (19)At the present epoch, where S = S_{0} and H = H_{0}, we have (20)from which, the presenttime value of the internal energy per unit restmass, Π_{0}, emerges as (21)Since Ω_{M} < 1, Eq. (21) suggests that, at the present epoch, the energy density, ρ_{0}Π_{0}, of the internal motions of a gravitating perfect fluid (consisting, mainly, of collisional DM and a small baryonic contamination) dominates over the corresponding restmass quantity, i.e., (22)But, what is more important, is that, at the same time, the combination of Eqs. (6) and (21) results in the following value of the totalenergy density parameter (23)In view of Eq. (23), the extra (dark) energy, needed to flatten the Universe, can be provided by the energy of the internal motions of a thermodynamicallyinvolvedDM fluid.
On the other hand, upon consideration of Eq. (21), Eq. (19) is written in the form (24)Equation (24) can be solved, explicitly, in terms of the error function (see Appendix A). However, it can become particularly transparent (and useful) if we take into account that, since 0 ≤ w ≤ 1 and Ω_{M} ≃ 0.3, the combination wΩ_{M} can be quite small, i.e., wΩ_{M} ≪ 1. In this case, we may take the natural logarithm on both sides of Eq. (24), to obtain (25)Within the postrecombination era, , hence . Therefore, as long as wΩ_{M} ≪ 1, we have (26)so that, to terms linear in wΩ_{M}, Eq. (24) results in (27)In this case, using Eq. (12), we can solve Eq. (27), to determine the scale factor of the collisionalDM model (1), as follows (28)where we have defined the presenttime value, η_{0}, of the conformal time, η, as (29)For w ≠ 0, Eq. (28) is the natural generalization of the corresponding collisionlessDM model, the wellknown Einsteinde Sitter (EdS) Universe (S ~ η^{2}) (see, e.g., Peacock 1999, pp. 77, 83 and 142 − 144).
Eventually, in the collisionalDM model given by Eq. (1), the cosmological redshift parameter is defined as (30)thus Eq. (27) is written in the form (31)We note the striking functional similarity between Eq. (31) and the corresponding result for a darkenergy fluid with equation of state in the form of Eq. (3) (cf. Eqs. (13) and (14) of Perivolaropoulos 2007). In our case, however, w ≥ 0 and, therefore, on the approach to z = 0, H(z) decreases monotonically. In other words, a cosmological model filled with collisional DM, necessarily, decelerates its expansion.
This can be readily verified, by expressing the corresponding deceleration parameter, q, in terms of H and z, as (32)(cf. Eq. (16) of Perivolaropoulos 2007), which, in view of Eq. (31), yields (33)independently of z, even for w = 0. In other words, the model of a gravitating perfectfluid source, as it stands, i.e., either pressureless (geodesic motions) or not (hydrodynamic flows), seems to be inappropriate for explaining the apparent accelerated expansion of the Universe.
The actual reason is that it does not have to account for any acceleration at all. As we demonstrate in the next section, in a Universe filled with collisional (i.e., thermodynamicallyinvolved) DM, the observed dimming of the distant lightemitting sources can be explained without the assumption of the accelerated expansion.
3. Mistreating the dark matter as collisionless
When the (unexpected) dimming of the SNe Ia standard candles was first discovered, the common perception about the cosmos, to the best of our knowledge, was that the DM constituents are collisionless, thus the various motions in the Universe were (necessarily) interpreted as geodesic motions of test particles receding from each other, i.e., (34)Tilde variables are used, to distinguish the various quantities in Eq. (34) from the corresponding quantities used in Eq. (9), thus reflecting that the physical content of a collisionlessDM Universe (in which both the pressure and the energy of the internal motions are assumed to be negligible and, therefore, disregarded) is entirely different from that of the thermodynamicallyinvolvedDM model (where p,Π ≠ 0).
In other words, the dynamical properties of a dust model are no longer described by g_{μν}, i.e., Eq. (1), but rather in terms of another metric tensor, , for which the corresponding (spatiallyflat) lineelement is written in the form (35)Clearly, the evolution of this model is given in terms of the scale factor R(η). From the point of view of an observer who (mis)treats the DM as collisionless, is the metric tensor upon which he/she should rely on, in interpreting observations.
However, we recall that, for this observer, the accumulated evidence in favour of spatial flatness (necessarily) leads to the assumption of an extra (dark) energy component, in contrast to the collisionalDM case, where this assumption would no longer be necessary. In the latter case, the appropriate candidate to provide the extra energy needed to flatten the Universe is already included in the model (the energy of the internal motions).
Furthermore, in the collisionlessDM scenario, every theoretical effort to interpret the (apparent) dimming of the SNe Ia standard candles, naturally, should also be based on and the cosmologically relevant parameters arising from it. Accordingly, a possible explanation could be that, recently, the Universe accelerated its expansion (Riess et al. 1998; Perlmutter et al. 1999). This assumption, however, attributes unnecessarilyexotic properties to the extra amount of energy needed to account for the spatial flatness (e.g., it should be repulsive in nature, i.e., of negative pressure, etc.). Therefore, we cannot help but wondering whether there is another (more conventional) explanation to be found (also) within the context of the collisionalDM model.
In what follows, we demonstrate that both the observed dimming of the distant lightemitting sources and the accelerated expansion of the Universe could be only apparent, based on the misinterpretation of several cosmologicallyrelevant parameters, by someone who (although living in a Universe filled with collisional DM) insists on adopting the traditional (collisionlessDM) approach.
To explore this possibility, we note that the collisionalDM treatment of the Universe’s matter content (in terms of which p ≠ 0 and the motions of its constituents are, in principle, hydrodynamic flows) can be related to the collisionlessDM approach where and the corresponding motions are, necessarily, geodesics, by means of a conformal transformation of the metric tensor (Kleidis & Spyrou 2000; Spyrou 2005; Spyrou & Tsagas 2004, 2010). Accordingly, from the original metric, g_{μν}, in terms of which the hydrodynamic flows have their wellknown form given by Eq. (8), we can transfer the problem to a virtual metric, , in terms of which the volume elements of the fluid move along geodesiclike trajectories, i.e., their velocityvector obeys Eqs. (34) (in connection, see Synge 1937; Lichnerowicz 1967, pp. 24 − 29 and 54 − 61; Carter 1979). The appropriate (conformal) transformation for such a transition is (36)where, upon consideration of isentropic flows, the conformal factor F(x^{κ}) takes on the functional form (Kleidis & Spyrou 2000) (37)with being an arbitrary (integration) constant. From Eq. (37), it becomes evident that F(x^{κ}) is, essentially, the specific enthalpy of the ideal fluid under consideration.
Verozub (2008) extrapolated these results to include every Riemannian spacetime and not just the metric attributed to a bounded, perfectfluid source. In particular, he showed that the adiabatic hydrodynamic motion of an idealfluid element in a spacetime with metric tensor g_{μν}, takes place along the geodesic lines of a Riemannian manifold with metric tensor given by the combination of Eqs. (36) and (37).
With the aid of the technique developed by Kleidis & Spyrou (2000), we then determine the scale factor of the spatiallyflat cosmological model in Eq. (35), i.e., the scale factor of the Universe as inferred by someone who, although living in a collisionalDM Universe (where p,Π > 0 and ), misinterprets the DM as collisionless .
In principle, one can (always) use a (conformal) transformation to remove (from the rhs of Eqs. (8)) either the pressure gradient, which measures the response to nongravitational forces, or the pressure itself (see, e.g., Lichnerowicz 1967, p. 26). Nevertheless, something like this (usually) comes with a price (see, e.g., Bruneton & EspositoFarese 2007): the new metric, in terms of which the DM appears to be pressureless, is no longer a solution of general relativity (GR), but, rather, a solution to a modified theory of gravity. The reason is that, in terms of this new metric (i.e., after the transformation (36) is applied), the action of the original gravitational field is also modified, acquiring extra terms in addition to the EinsteinHilbert Lagrangian (see Appendix B). In other words, every effort to treat a collisionalDM fluid as pressureless, cannot be accomplished in the context of GR. As a consequence, R(η) is no longer a solution of the original Friedmann equation, given by Eq. (11).
In view of Eq. (36), the scale factor of the Universe as it is inferred by a supporter of the collisionlessDM scenario, R(η), is related to the corresponding quantity of the collisionalDM model, S(η), as follows (38)where, by virtue of Eqs. (7), (17), and (30), F(x^{κ}) is given, in terms of z, by (39)In Eq. (39), the arbitrary integration constant, , can be determined, by demanding that, in the (isobaric) pressureless case, these two models should coincide, i.e., . In other words, for w = 0 = p, R(η) = S(η,w = 0), which represents the EdS model. Hence, F(w = 0) = 1.
For p = const. = p_{0}, the first law of thermodynamics given in Eq. (13) yields (40)which, in the particular case of dust, where p_{0} = 0, results in Π = const. = Π_{0}. Now, from Eq. (19) it becomes evident that, at the present epoch, Π (= Π_{0}) is (also) given by Eq. (21), even for w = 0. Accordingly, inserting Eq. (21) into Eq. (37), we find that, the condition F(w = 0) = 1 leads to (41)As a consequence, Eq. (39) results in (42)Using Eqs. (38) and (42), we can then express several cosmologically relevant parameters of the collisionalDM model in terms of their collisionlessDM counterparts, such as the cosmological redshift, the luminosity distance, and the distance modulus of the various lightemitting sources, together with the Hubble and the deceleration parameters, which characterize the cosmic expansion.
3.1. The cosmological redshift
A supporter of the collisionlessDM scenario would define the corresponding cosmological redshift parameter, , as (43)which, upon consideration of Eq. (38), is written in the form (44)where (45)Taking into account Eq. (42), Eq. (44) results in (46)Confining ourselves to relatively low values of the cosmological redshift parameter (e.g., z < 5), to ensure that the combination 3wΩ_{M}ln(1 + z) remains sufficientlylower than unity even for relatively large values of the combination wΩ_{M} (e.g., wΩ_{M} ~ 0.1, i.e., ), we can apply the technique used in Eqs. (25) − (27), to obtain (47)In this case, we note that, for every (fixed) value of the cosmological redshift z, i.e., as defined in the collisionalDM model, the corresponding collisionlessDM quantity is always a little bit smaller .
In other words, on observing a lightemitting source of the collisionalDM model, an observer who adopts the collisionlessDM scenario (realizing redshifts as instead of z), necessarily admits that this source lies a little bit farther (z) than expected .
3.2. The luminosity distance and the distance modulus
Nowadays, the most direct and reliable method for determining, observationally, the (relatively) recent history of the Universe expansion, is to measure the redshift and the apparent luminosity (equivalently, the apparent magnitude, m) of cosmologicallydistant indicators (standard candles), whose absolute luminosity (equivalently, the absolute magnitude, M) is assumed to be known.
SN Ia events constitute one of the most suitable cosmological standard candles (Plionis et al. 2009). With the aid of these events, a number of scientific groups have attempted to find evidence in support of a recentlyaccelerating stage of the Universe (Garnavich et al. 1998; Riess et al. 1998, 2001, 2004, 2007; Perlmutter et al. 1999; Knop et al. 2003; Tonry et al. 2003; Astier et al. 2006; WoodVasey et al. 2007; Kowalski et al. 2008; Hicken et al. 2009). In each and every one of these surveys, the SN Ia events, at peak luminosity, appear to be dimmer (i.e., they seem to lie farther away) than expected. This result was, eventually, accommodated within the context of the concordance model, by a DE fluid of negative pressure, with Ω_{X} ~ 0.7 (see, e.g., Spergel et al. 2003; Tonry et al. 2003). However, in view of Eq. (47), there may be also another, more conventional interpretation.
Photons travel along null geodesics, , which remain unaffected by conformal transformations. Accordingly, in both the collisionalDM and collisionlessDM approaches, the radial distance of a lightemitting source (in comoving coordinates) is the same, i.e., (48)where η_{r} and η_{e} are the conformal times of reception and emission of light, respectively (usually, η_{r} = η_{0}).
In this case, with the aid of Eq. (47), the formula determining the luminosity distance in a spatiallyflat collisionalDM model (49)(see, e.g., Peacock 1999, p. 92) can be expressed in terms of the corresponding collisionlessDM quantity (50)as (51)This relation is very interesting. It suggests that, in a Universe containing collisional DM (i.e., as long as w ≠ 0), there exists a characteristic (transition) value of the cosmological redshift, (52)such that, the luminosity distance of the various lightemitting sources located at z > z_{c}, is always larger than what is inferred by a supporter of the collisionlessDM scenario. Therefore, an observer who treats the DM as collisionless (measuring distances in terms of ) necessarily admits that any standard candle located at z > z_{c} lies farther than expected, i.e., .
The same also happens in the case of the distance moduli corresponding to d_{L} and . The Kcorrected distance modulus, μ(z) = m − M, of a lightemitting source in the collisionalDM model is given by (53)(see, e.g., Narlikar 1983, Eqs. (13.10) and (13.12), p. 359), where d_{L} is measured in megaparsecs (Mpc). In a similar fashion, (54)is the distance modulus of the same source, as defined by someone who, although living in the collisionalDM model, insists on adopting the (traditional) collisionlessDM approach. Subtracting Eqs. (53) and (54) by parts, and using Eq. (51), we obtain (55)According to Eq. (55), any lightemitting source of the collisionalDM Universe located at z > z_{c}, from the point of view of an observer who insists on adopting the collisionlessDM approach (treating the various distance moduli in terms of ), appears to be dimmer than expected, i.e., .
We cannot help but notice the prominent similarity between the characteristic value z_{c} and the transition redshift, z_{t}, which, according to a supporter of the collisionlessDM scenario, signals the onset of the dimming of the SNe Ia standard candles, something that is interpreted (by such an observer) as an entry into a phase of accelerated expansion. As we see, what actually happens in a collisionalDM model is that, from the point of view of someone who incorrectly assumes the DM as collisionless (i.e., measuring cosmological distances in terms of instead of the trulymeasured quantity d_{L}), an inflection point in the versus z diagram (namely, z_{c}) will arise anyway. For wΩ_{M} = 0.1, i.e., (the DM consists of relativistic particles), the characteristic transition value in Eq. (52) is set at z_{c} = 0.37, while, for lower values of w, z_{c} reaches up to 0.39. These results lie within the observationally traced range of values concerning z_{t}, namely z_{t} = 0.46 ± 0.13 (Riess et al. 2004, 2007). In other words, the spatiallyflat collisionalDM model given by Eq. (28) does not suffer from the coincidence problem.
Therefore, if the DM possesses some sort of thermodynamical content, then, it is possible that (i) the “infernous” discrepancy between the expected value of the distance modulus of a SN Ia standard candle and the corresponding observed one (μ); and (ii) the accompanying inflection point, z_{t}, that signals the transition from deceleration to acceleration, may both arise only because many cosmologists (although living in a collisionalDM model) insist, instead, on adopting the (traditional) collisionlessDM approach. In the next section, we demonstrate that this is exactly what happens in a collisionalDM Universe.
3.3. The Hubble and the deceleration parameters
By virtue of Eq. (38), the Hubble parameter inferred by a supporter of the collisionlessDM scenario, , is written in terms of H as (56)from which, a much more interesting relation can be obtained in terms of the cosmological redshift. By taking into account that (57)Eq. (56) is written in the form (58)which, in view of Eq. (42), results in (59)or else (60)where we have also used Eq. (31). We note that, to terms linear in wΩ_{M}, (61)i.e., within the context of the collisionlessDM approach, at the present epoch (when z = 0), the Universe expands only as long as , and, in any case, at a lower rate than the collisionalDM treatment (H_{0}) implies. In view of Eq. (47), i.e., at relatively low values of z, Eq. (60) can be written in terms of , as (62)We verify that, to terms linear in wΩ_{M}, Eq. (61) is (also) valid at .
By analogy with Eq. (32), a supporter of the collisionlessDM scenario would define the corresponding deceleration parameter, , as (63)which, by virtue of Eq. (62), yields (64)Now, the condition for accelerated expansion is translated to from which, to terms linear in wΩ_{M}, we obtain (67)From Eq. (66) it becomes evident that, from the point of view of someone who insists on adopting the collisionlessDM approach, at cosmological redshifts (68)This relation is very interesting: it suggests that, if the Universe mattercontent is treated as a collisionalDM fluid with w being larger than a critical value, w_{c}, such that (69)(i.e., w > w_{c} ≈ 0.238), then, from the point of view of someone who incorrectly assumes the DM as collisionless, there exists a transition value, , of , below which, the postrecombination Universe (as being realized by such an observer) is accelerating, independently of any notion of DE or the cosmological constant.
In other words, if the Universe evolution is driven by a collisionalDM fluid with w > w_{c}, then, the apparent acceleration of the cosmic expansion could (very well) be due to a misinterpretation of several cosmologicallyrelevant parameters, by an observer who (although living in a cosmological model filled with collisional DM) insists on adopting the collisionlessDM approach. At the same time, for this observer, the cosmologically distant indicators would appear to be dimmer than expected (cf. Eq. (55)).
We recall here that the recent observational data concerning the SNe Ia standard candles set the transition redshift between accelerated and decelerated expansion at z_{t} = 0.46 ± 0.13 (Riess et al. 2004). In this case, the combination of Eqs. (47) and (67) results in the nonlinear algebraic equation involving the transition value, z_{t}, of the trulymeasured quantity z(70)Equation (69) can be solved numerically with respect to the combination wΩ_{M}. Accordingly, we verify that the value (71)reproduces (exactly) the above observational result for z_{t}.
By virtue of Eq. (70), we note that , i.e., compatibility of the collisionalDM approach with the observational data, currently available, suggests that, in Eq. (3), the pressure of the cosmic fluid under consideration is due to radiation. Nevertheless, in view of Eq. (17), the evolution of the restmass density indicates that, for every value of w, the spatiallyflat model given by Eq. (28) is matterdominated. Taken together, these results imply that the DM itself, being responsible for the nonvanishing pressure, consists of relativistic particles (“hot” DM). We verify this result by overplotting Eq. (55) in the Hubble (μ versus z) diagram of a SN Ia dataset.
3.4. Application to a sample of SN data
An extended sample of 192 SN Ia events has been used by Davis et al. (2007) to scrutinize the viability of various DE scenarios. This sample^{1} consists of 45 SNe from a nearby SN Ia dataset (Hamuy et al. 1996; Riess et al. 1999; Jha et al. 2006), 57 events from SNLS – the SuperNova Legacy Survey (Astier et al. 2006), 60 intermediateredshift events from ESSENCE – the Equation of State: SupErNovae trace Cosmic Expansion program (WoodVasey et al. 2007), and 30 highz SNe from the Gold07 sample (Riess et al. 2007).
To overplot Eq. (55) on the μ versus z diagram of this dataset, first of all, we need to determine the functional form of the luminosity distance (and, through it, the corresponding form of the distance modulus, ), used by someone who, although living in a collisionalDM model, insists on the collisionlessDM approach. This observer performs calculations in the (traditional) framework of a pressureless Universe, adopting the corresponding formula of the luminosity distance. In a spatiallyflat model, this formula is given by (see, e.g., Carroll et al. 1992) (72)representing the luminosity distance in the EdS Universe, the (conformally) pressureless counterpart of the collisionalDM model given by Eq. (28).
However, we need to stress that, in a collisionalDM Universe, the measured quantity (corresponding to the cosmological redshift) is z and not , as it is (falsely) admitted by someone who (mis)treats the DM as collisionless. Therefore, in order to include, also, the function in the Hubble diagram of the SN Ia dataset used by Davis et al. (2007), we have to express in terms of the trulymeasured quantity, z. It can be done (appropriately) by inserting Eqs. (47) and (61) into Eq. (71), to obtain (73)However, as we have already mentioned, this is not the case for a supporter of the collisionlessDM scenario. In depicting Eq. (54) – with being given by Eq. (71) – on the μ versus z diagram of a sample of SN events, this observer (admitting that w = 0), unavoidably, misinterprets the measured quantity z as (and the quantity H_{0} as ). In other words, the theoretical formula of the luminosity distance that is used by someone who, although living in a (spatiallyflat) collisionalDM model, insists on adopting the collisionlessDM approach is (incorrectly) written in the form of Eq. (71) with simply replaced by z(74)instead of that given by Eq. (72). In what follows, we admit that H_{0} = 70.5 km s^{1} Mpc^{1} (Komatsu et al. 2009), hence 2c/H_{0} = 8509.8 Mpc.
We then overplotted in the Hubble diagram of the SN Ia dataset used by Davis et al. (2007) the theoretical curves corresponding to the distance moduli: μ(z) for wΩ_{M} = 0.16 (green solid line); (also for wΩ_{M} = 0.16) with being given by Eq. (72) (orange solid line); and with being given by Eq. (73) (dashed line). The outcome is presented in Fig. 1. We observe that, the (appropriately translated in terms of z) collisionlessDM quantity – with being given by Eq. (72) (orange solid line) is quite far from being able to reproduce these data, although, for z ≤ 1.75, it is much closer to the “real world” (the μ versus z distribution of the SN Ia data available) than the incorrectly used quantity – with being given by Eq. (73) (dashed line).
Fig. 1 Hubble diagram of the SN Ia sample used by Davis et al. (2007). Overplotted are the theoretical curves, corresponding to the distance moduli: μ(z) for wΩ_{M} = 0.16 (green solid line); (also for wΩ_{M} = 0.16) with being given by Eq. (72) (orange solid line); and with being given by Eq. (73) (dashed line). We observe that, after the thermodynamical content of a collisionalDM fluid is taken into account, the theoretical curve representing the distance modulus, μ(z) (Eq. (55)), fits the entire dataset quite accurately (green line). 

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The situation changes, completely, when someone takes into account the thermodynamical content of a collisionalDM fluid with wΩ_{M} = 0.16, thus using Eq. (55) instead of Eq. (54) alone. In this case, the function μ(z) (green solid line) seems to fit the entire dataset under consideration quite accurately.
As we observe in Fig. 2, apart from a small number of SN events (4 of 192), the entire dataset used by Davis et al. (2007) lies within the stripe formed by the theoretical curves μ(z), corresponding to wΩ_{M} = 0.10 (red solid line) and wΩ_{M} = 0.19 (blue solid line), while the best fit to this sample appears to be achieved for wΩ_{M} = 0.16 (green line). In a spatiallyflat cosmological model, it is clear that, the collisionalDM treatment is not only much closer to, but, actually, can reproduce quite accurately the μ versus z distribution of the SN Ia sample used by Davis et al. (2007).
Fig. 2 Overplotted in the Hubble diagram of the SN Ia sample used by Davis et al. (2007), are the theoretical curves of the distance modulus in the collisionalDM model, i.e., Eq. (55), for several values of the combination wΩ_{M}. Almost the entire dataset lies within the stripe formed by the curves μ(z), corresponding to wΩ_{M} = 0.10 (red solid line) and wΩ_{M} = 0.19 (blue solid line), while, the best fit to this sample is achieved for wΩ_{M} = 0.16 (green line). Once again, the dashed line represents the (incorrectly used) theoretical curve with being given by Eq. (73). 

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Nevertheless, there is a “delicate point” in this treatment. For wΩ_{M} ≥ 0.10, we have . In other words, compatibility of the collisionalDM approach with the currently available observational data, suggests that the cosmic fluid (i.e., above all, the DM itself) consists of relativistic particles.
Taken together, these results strongly suggest that, if the DM constitutes a perfect fluid (of relativistic particles) with thermodynamical content, then, what is interpreted as the “dimming” of the SNe Ia standard candles might only be apparent, provided that the cosmologists no longer insist on adopting the collisionlessDM approach.
In other words, in a Universe filled with collisional (and relativistic) DM, the unexpected dimming of the distant lightemitting sources can be explained in a more conventional way, than that implemented within the context of the accelerated expansion. Hence, before inventing any new theory, it is useful to allow for a suitable use of the (so far) neglected degrees of freedom (energy of the internal motions, pressure, etc.). As we have shown, these internal physical characteristics can reveal their influence on several parameters of cosmological significance (scale factor, cosmological redshift, luminosity distance, Hubble and deceleration parameters) and yield a consistent alternative to the currentlyaccepted DE concept.
3.5. An independent confirmation from BAO’s data analysis
Among the various (currently available) techniques for tracing the expansion history of the Universe, baryon acoustic oscillations (BAO) appear to have the lowest level of systematic uncertainty (Albrecht et al. 2006).
BAO is a series of peaks and troughs, with wavenumber (approximately) 0.06 h (Mpc)^{1} (Eisenstein et al. 2005), arising, on large scales, in the power spectrum of matter fluctuations after recombination. They occur because the primordial cosmological perturbations excite sound waves in the relativistic plasma of the early Universe (Silk 1968; Peebles & Yu 1970; Sunyaev & Zel’dovich 1970; Bond & Efstathiou 1984, 1987; Holtzman 1989; Hu & Sugiyama 1996). This process continues for a short timeinterval after recombination, until the epoch known as baryondrag epoch (z_{d} ≃ 1089), when, eventually, the baryons are released from the Compton “drag” of photons (Eisenstein & Hu 1998).
The BAO’s wavenumber is related to the comoving distance of the sound horizon at the baryondrag epoch, r_{s}, which depends on both the totalmass density of the Universe and the corresponding baryonic quantity (see, e.g., Wang 2006). WMAP constraints on Ω_{M}h^{2} and Ω_{B}h^{2} (Komatsu et al. 2009) suggest that r_{s}(z_{d}) ≃ 153.5 Mpc. In other words, BAO are met on relativelylarge scales, which, at the present epoch, are (still) in the linear regime. It is, therefore, expected that, these acoustic signatures should be present (also) in the distribution of galaxies (Goldberg & Strauss 1998; Meiksin et al. 1999; Seo & Eisenstein 2005; Eisenstein et al. 2007).
Since the comoving distance of the sound horizon at the baryondrag epoch is known, we can use BAO as standard rulers, to determine the functional form of the distance – redshift relation in the Universe. In particular, by determining observationally the apparent size of a BAO’s peak (it is identified as a clustering within a galaxy distribution), we can extract reliable estimates of the Hubble parameter, as well as the angular diameter distance, at the cosmological redshift, in which, this acoustic signature is observed (Blake & Glazebrook 2003; Hu & Haiman 2003; Seo & Eisenstein 2003).
The spectroscopic Sloan Digital Sky Survey (SDSS) Data Release 7 (DR7) represents the final set of galaxies, observed using the original SDSStarget selection criteria (York et al. 2000). When combined with the data released from the 2degree Field (2dF) galaxyredshift survey (Colless et al. 2003), the resulting sample comprises 89 3319 galaxies and covers a solid angle of 9100 deg^{2}. An analysis of the clustering of galaxies within this sample, inferred BAO signals in the power spectrum measured in several slices of the cosmological redshift (Percival et al. 2010).
To minimize the systematic errors arising from treating the lineofsight dilation in an equivalent manner to the transverse one (a common bias, involving the socalled AlcockPaczyński 1979, effect), cosmologists defined the distance measure (75)(Eisenstein et al. 2005; Percival et al. 2007), where Z is the observationallydetermined (i.e., spectroscopicallymeasured) value of the cosmological redshift of a largescale structure, and (76)is the corresponding angular diameter distance in a spatiallyflat cosmological model (see, e.g., Peacock 1999, p. 22). The combination of Eqs. (74) and (75) results in (77)where, once again, r is the radial distance (in comoving coordinates) of the structure formation under consideration.
According to Percival et al. (2010), there exists a robust, statisticallyindependent (distance) constraint, arising from BAO’s data, which involves the value of the ratio (78)Clearly, in a collisionalDM model, Eq. (77) represents the trulymeasured value of f. In this case, we ask ourselves what is observed by someone who, although living in a collisionalDM model, insists on adopting the (traditional) collisionlessDM approach.
To answer this question, we note that, when, either the collisionalDMoriented observer or the corresponding collisionlessDM one, spectroscopically measures the cosmological redshift of a particular largescale structure, they both refer to the same quantity, Z. Accordingly, a supporter of the collisionlessDM scenario would express Eq. (76) in the form (79)where we have also used Eq. (48). Equation (78) differs from Eq. (76) only in the definition of the presenttime value of the scale factor and in the functional dependence of the Hubble parameter on Z. In this case, upon consideration of Eqs. (45) and (60), we obtain Now, as far as a supporter of the collisionlessDM scenario is concerned, the BAO’s constraint given by Eq. (77) is translated as (82)which for, wΩ_{M} = 0.10, results in (83)and for wΩ_{M} = 0.16, we have that (84)Both values of lie within the range of values [1.671,1.801 ] of the measured quantity, f, given by Eq. (77). Therefore, as far as a supporter of the collisionlessDM scenario is concerned, the observational constraint, , inferred from BAO’s data, is (at least) compatible with (if not almost identical to) the corresponding constraint, f, obtained within the context of the collisionalDM model.
However, when the collisionlessDMoriented observer attempts to verify Eq. (81) (or Eq. (82)) theoretically, a controversy arises. This observer applies Eq. (78) to the EdS Universe (the pressureless counterpart of the collisionalDM model under study), which accommodates the standard (w = 0) cold dark matter (SCDM) cosmology. In this case, (85)hence, a supporter of the collisionlessDM scenario obtains (86)(see, also, Percival et al. 2010). Clearly, there is a difference between the theoretical result of Eq. (84) and the observational one given by Eq. (81) (or Eq. (82)). As far as the supporter of the collisionlessDM scenario is concerned, one way to compensate this difference, is to impose the existence of an extra (dark) energy component or the cosmological constant. However, even when he/she does so, i.e., within the context of the ΛCDM model, the theoretical value of the distance constraint, , induced by the signature of BAO on cosmic structure, reaches up to (87)(Eisenstein et al. 2005; Percival et al. 2010). Although marginally, lies outside the range of values of the trulymeasured quantity, f, given by Eq. (77). In view of the abovementioned results, we may conclude that, within the context of the collisionalDM approach, the BAO’soriented observational data require (and acquire) a more sophisticated interpretation than the one provided by the (collisionless) ΛCDM model.
4. Discussion
We have examined the possibility that the extra (dark) energy needed to flatten the Universe is represented by the energy of the internal motions of a collisionalDM fluid. Accordingly, we have considered the evolution of a cosmological (toy) model driven by a gravitating fluid (consisting of DM – dominant – and baryonic matter – subdominant) with thermodynamical content. As a consequence, the energy of this fluid’s internal motions has also been taken into account as a source of the universal gravitational field. Accordingly, we have asked ourselves, whether this model can also accommodate the apparent dimming of the cosmologically distant indicators and the associated phase of accelerated expansion.
In particular, since observational data indicates that WIMPs (of which the DM is believed to consist) can be collisional, we have assumed that the matter of the Universe (although resembling test particles receding from each other) can be represented by the volume elements of a (classical) collisionalDM fluid with some sort of internal structure, hence thermodynamical content. In this way, we have been able to determine the “correct” form of the scale factor, which (under the assumption that the DM is thermodynamically involved) governs the evolution of the Universe (modeled as a spatiallyflat RW spacetime), in addition to a series of parameters of cosmological significance.
Our findings are quite promising. In principle, the energy of the internal motions of the collisionalDM fluid can account for the (extra) DE, so that, at the present epoch, Ω = 1 (cf. Eq. (23)), while the postrecombination Universe remains everdecelerated (cf. Eq. (33)).
We next attempted to determine what is inferred by someone who, although living in a collisionalDM model, insists on adopting the (traditional) collisionlessDM approach.
To do so, we have applied the technique developed by Kleidis & Spyrou (2000). With the aid of this technique, we have derived the (conformal) transformation (cf. Eqs. (38) and (42)), which relates the collisionalDM description of a cosmological model (in terms of which p,Π > 0 and ) to the corresponding collisionlessDM (pressureless) approach. With such a “tool” at hand, we have explored the way that a supporter of the collisionlessDM scenario interprets observations carried out in a collisionalDM Universe. In passing, we note that, within the context of general relativity, every effort to treat a collisionalDM model as pressureless is questioned (Appendix B).
The debate between collisional and collisionlessDM approach is, definitely, in favor of the former. In particular, for every value of the cosmological redshift (z), as it is defined in the collisionalDM model, the corresponding collisionlessDM quantity, , is always a little bit smaller (cf. Eq. (47)). As a consequence, in the collisionalDM model there is a characteristic value of the cosmological redshift, z_{c} (cf. Eq. (52)), above which, the luminosity distance of the various lightemitting sources is always higher than what is inferred by an observer who treats the DM as pressureless (cf. Eq. (51)). In other words, from the point of view of someone who (although living in a collisionalDM model) insists on adopting the (traditional) collisionlessDM approach, the cosmologicallydistant indicators, located at z > z_{c}, seem to lie farther away (i.e., appear dimmer) than expected (cf., also, Eq. (55)).
The similarity between the characteristic value z_{c} and the (observationallytraced) transition redshift, z_{t}, which, according to a supporter of the collisionlessDM scenario, signals the onset of the dimming of the SNe Ia standard candles, is obvious.
On the other hand, after the thermodynamical content of a collisionalDM fluid is taken into account, the theoretical curve representing the distance modulus, μ(z) (now given by Eq. (55)), fits the Hubble diagram of an extended sample of SN Ia standard candles quite accurately (green solid line in Fig. 1), in contrast to the corresponding collisionlessDM quantity, , given either (appropriately) by the combination of Eqs. (54) and (72) (orange solid line in Fig. 1) or (incorrectly) by the combination of Eqs. (54) and (73) (dashed line in Fig. 1). In fact, a cosmological model filled with collisional DM could accommodate the majority of the currentlyavailable observational data, including, also, those related to BAO, without the need for any dark energy or the cosmological constant (cf. Eqs. (81) and/or (82)).
At the same time, from the point of view of an observer who treats the DM as collisionless, the Universe appears to be either accelerating or decelerating, depending on the value of the cosmological redshift (cf. Eq. (67)).
In this case, the quantity w, which, in the collisionalDM approach, parameterizes the various flows, also plays another (more interesting) role. As we have found, for wΩ_{M} ≥ 0.0714, there exists a (theoreticallydetermined) transition value, , of the (collisionlessDMoriented) cosmological redshift, , such that, for , we have , i.e., from the point of view of someone who adopts the (traditional) collisionlessDM approach, the Universe is accelerating, without the need for any DE or the cosmological constant. Accordingly, taking into account the observational result that the transition redshift between accelerated and decelerated expansion is set at the value z_{t} = 0.46 ± 0.13 of the truly measured quantity z, we have determined the precise value of the combination wΩ_{M}, for which the collisionalDM approach to the postrecombination Universe is compatible with observations, i.e., (wΩ_{M})_{t} = 0.0932 ± 0.0060. This result is in complete agreement with what is implied by Fig. 2, i.e., . In other words, compatibility of the collisionalDM treatment under study with the observational data currently available, suggests that the DM itself consists of relativistic particles (hot DM).
In conclusion, the assumption that the DM constituents can be both collisional and relativistic, could provide a reasonable and conventional explanation for several open aspects of modern cosmology, including: (i) the extra (dark) energy needed to flatten the Universe, which can be compensated by the energy of the internal motions of the collisionalDM fluid; (ii) the observed dimming of the SNe Ia standard candles and the apparent accelerated expansion of the Universe, both of which might be due to the misinterpretation of several cosmologically relevant parameters by those observers who, although living in a collisionalDM Universe, insist on adopting the collisionlessDM approach. The absence of any ad hoc finetuning in our study, makes the above (purely theoretical) results very promising.
In spite of all the above advantages of our model, we have to point out that this is, definitely, a toy model. The collisionalDM approach, developed in this article, can (and should) be debated, at least, along the following lines:

(i)
The collisionalDM treatment of the Universe does notalleviate the age problem, but, rather, makes it harder. In themodel given by Eq. (28), the coordinate time,t, is related to the corresponding conformal quantity (η) by (88)Admitting that, at the present epoch (when t = t_{0} and η = η_{0}) H_{0} ≈ 70.5 km s^{1} Mpc^{1} (Komatsu et al. 2009), we find that, within the context of the model given by Eq. (28), the age of the Universe is (89)i.e., less than 9.3 billion years. Clearly, Eq. (87) could be a serious drawback of the spatiallyflat collisionalDM model.

(ii)
The compatibility of the collisionalDM approach with the observational data currently available (cf. Eq. (70) and/or Fig. 2), suggests that the matter content of the dark sector consists of hot DM. For the time being, the conventional theory of hot DM does not appear to conform with the largescale structure of the Universe (see, e.g., Hooper 2009), although there are recent studies that appear to challenge this result (see, e.g., Farrar & Peebles 2004; Gubser & Peebles 2004). Nevertheless, a hotDM model looks much less exotic than most of the (currentlyinvestigated) DE scenarios.
In any case, the assumption that the Universe matter content (basically its DM component) can be collisional (in the sense that it also possesses some sort of thermodynamical content), is to be seen as a natural effort to take into account all the (so far, practically, neglected) internal physical characteristics of a classical cosmological fluid as sources of the universal gravitational field.
As we have shown, under this assumption, one can compensate for the majority of the recent observational data, inferring that Ω ≃ 1, as well as the “unexpected” dimming of the SNe Ia standard candles and the “apparent” accelerated expansion of the Universe, not to mention the compatibility with BAO’s data analysis, without the need for any DE or the cosmological constant, and (certainly) without suffering from the coincidence problem. From the point of view of someone who (although living in the collisionalDM model) insists on adopting the collisionlessDM approach, an inflection point (in the versus z diagram) arises, anyway, at relatively low values of the cosmological redshift.
Although speculative, the idea that the DE (needed to flatten the Universe) could be attributed to the internal motions of a collisionalDM fluid, is (at least) intriguing and should be explored further and scrutinized in the search for conventional alternatives to the DE concept.
Available at http://www.ctio.noao.edu/essence or at http://braeburn.pha.jhu.edu/~ariess/R06
Acknowledgments
The authors would like to thank Professors George F. R. Ellis and Manolis Plionis, together with Drs. Leandros Perivolaropoulos and Christos G. Tsagas, for their constructive critisism, many illuminating discussions and useful comments on an earlier version of this article, as well as on this kind of research, in general. We also thank the anonymous referee for his/her kind comments and his/her useful suggestions, which improved this paper’s final form. Finally, financial support by the Research Committe of the Technological Education Institute of Serres, under grant SAT/ME/15121071/01, is gratefully acknowledged.
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Appendix A
In this Appendix, we present the exact solution to Eq. (24) in the text and its subsequent reduction to Eq. (28). In paricular, upon consideration of Eq. (12), Eq. (24) reads (A.1)and can be cast in the (more convenient) form (A.2)In an expanding Universe, Eq. (A2) is valid for every η within the past lightcone (where S < S_{0}) and it can be solved in terms of the error function (see, e.g., Abramowitz & Stegun 1970, p. 297) as Equation (A3) becomes particularly transparent (and useful) if we restrict ourselves to the limiting case, where wΩ_{M} ≪ 1.
For wΩ_{M} ≪ 1, the argument of the error function in Eq. (A3) becomes very large. In this case, the special function under consideration behaves as (A.5)(see, e.g., Lebedev, Eq. (2.2.4), p. 19) and, therefore, Eq. (A3) results in (A.6)We now take the natural logarithm on both sides of Eq. (A5), to obtain (A.7)Within the postrecombination era, , hence . Therefore, as long as wΩ_{M} ≪ 1, Eq. (26) holds, hence Eq. (A6) is written in the form (A.8)which, in view of the definition given by Eq. (29), results in (A.9)that is, Eq. (28).
Appendix B
In curved spacetime, the EinsteinHilbert (EH) action, which governs the dynamical evolution of the gravitational field, g_{μν}, within the context of GR, is given by (see, e.g., Papapetrou 1973, Eq. (33.29), p. 122) (B.1)where g is the determinant of the metric tensor g_{μν}, ℛ is the scalar curvature, κ = 8πG/c^{4}, and is the trace of the energymomentum tensor of the Universe matterenergy content. In a similar fashion, the action of the gravitational field in terms of , i.e., after the transformation indicated in Eq. (36) is performed, is written in the form (B.2)which, upon consideration of Eqs. (36) and (39) of Kleidis & Spyrou (2000), results in (B.3)where ΔF = g^{μν}F_{;μν} is the d’Alembert operator with respect to the original metric, g_{μν}. It is evident that, every effort to express in terms of the original gravitational field, g_{μν}, yields the appearence of extra terms in the gravitational action, in addition to the EH one. In this way, variation of Eq. (B3) with respect to g^{μν} does not lead to the Einstein field equations of GR (i.e., those derived from Eq. (B1)), thus (necessarily) resulting in a modified theory of gravity (in connection, see, e.g., Bruneton & EspositoFarese 2007).
All Figures
Fig. 1 Hubble diagram of the SN Ia sample used by Davis et al. (2007). Overplotted are the theoretical curves, corresponding to the distance moduli: μ(z) for wΩ_{M} = 0.16 (green solid line); (also for wΩ_{M} = 0.16) with being given by Eq. (72) (orange solid line); and with being given by Eq. (73) (dashed line). We observe that, after the thermodynamical content of a collisionalDM fluid is taken into account, the theoretical curve representing the distance modulus, μ(z) (Eq. (55)), fits the entire dataset quite accurately (green line). 

Open with DEXTER  
In the text 
Fig. 2 Overplotted in the Hubble diagram of the SN Ia sample used by Davis et al. (2007), are the theoretical curves of the distance modulus in the collisionalDM model, i.e., Eq. (55), for several values of the combination wΩ_{M}. Almost the entire dataset lies within the stripe formed by the curves μ(z), corresponding to wΩ_{M} = 0.10 (red solid line) and wΩ_{M} = 0.19 (blue solid line), while, the best fit to this sample is achieved for wΩ_{M} = 0.16 (green line). Once again, the dashed line represents the (incorrectly used) theoretical curve with being given by Eq. (73). 

Open with DEXTER  
In the text 
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