Both illustrations correspond to dark energy dominance. One of the main serious problem concerns the fact that the speed of the energy flow may surpass the speed of light allowing closed causal loops. An additional problem is related to the Hamiltonian which can be unbounded below depending on the cosmological system, but mainly for phantom matter with a negative kinetic energy.
Such a system has a negatively infinite ground state, therefore no stable vacuum solution exists . Other problem is related to Big Rip, i. It is noteworthy that over the years there have been many experiments performed that place upper limits on the time variability of the effective gravitational coupling constant. In general, it was recently observed that for late times, a modified cosmology with varying gravitational coupling constant is in accordance with the observed values of the cosmological parameters.
In summary, if we admit the superstring theory as a true and promising quantum field theory of gravity unifying gravity with all matter interactions, the GB invariant term is the only grouping of curvature-squared interactions for which the low-energy effective action is ghost-free. In the present work our main aim was to explore the novel cosmological features resulting from the presence of the Gauss-Bonnet curvature term in dimensional modified gravity with non-minimal coupling.
We ignored the presence of the dilaton field and the Yang-Mills field strength, therefore our framework is different from the multidimensional scenarios discussed by Kripfganz-Perlt  and Lorentz-Petzold. In order that the equivalence principle is satisfied, we have identified the scalar field as a run-away modulus without direct matter couplings though gravitational dynamics are modified due to the presence of modulus-dependent loop corrections.
We showed that such coupling can trigger the accelerated expansion of the universe without the presence of phantom energy field after a scaling matter era. Besides investigating the late-time cosmological evolution of such models, we also derive quantitative constraints on the scenario of Gauss-Bonnet coupling function. We have choose scaling solutions as we strongly believe that scaling solutions during the dynamical evolution of the universe play a crucial role as they serve to better understand many extended properties.
In other words, the linear curvature term therefore dominates over the contribution of the quadratic term and all other higher order terms if curvature is non-minimally coupled to the scalar field. We have obtained a late time accelerated expansion of the universe without crossing the phantom divide line, i. There exist other specific scenarios of dark energy with striking features capable of explaining the present accelerated expansion of the universe [40,41,42,43,44,45]. The simple model described in this paper belongs to the same sort but holds some new features discussed above. This model needs a firmer theoretical supporting which might come from modified gravity theories.
Other interesting consequences may be revealed in particular the luminosity distance expression and statistical analysis of the data obtained; however, it is a primitive model and work in this direction is under progress. This only shows that such investigations may be useful for a future study. The author would like to thanks the anonymous referees for their useful comments and valuable suggestions.
Peebles and Ratra B, Rev. Concalves and de R. Sa Ribeiro, Gen. Fabris and de R.
Sa Ribeiro Gen. D12 , and references therein. B , and references therein. B , No D18 , 15, D18 , 2, Perlt, Acta Phys. B18 , 11, Kerner Classical and Quantum Gravity 5 , For this purpose, we use flat FRW universe model with perfect fluid matter contents. By taking power law ansatz for scalar field, we discuss the strong, weak, null, and dominant energy conditions in terms of deceleration, jerk, and snap parameters. Some particular cases of this theory like -essence model, modified gravity theories and so forth. The investigation of this hidden unusual nature of DE has been carried out in two ways: Examples of some well-known modified gravity theories include gravity [ 17 , 18 ], scalar-tensor theories like Brans-Dicke BD gravity [ 19 , 20 ], Gauss-Bonnet gravity [ 21 , 22 ], theory [ 23 , 24 ], and gravity [ 25 ].
Modified matter sources are rather interesting but each faces some difficulties and hence could not prove to be very promising.
Modified gravitational theories being large-distance modifications of gravity have brought a fresh insight in modern cosmology. Among these, scalar-tensor theories are considered to be admirable efforts for the investigation of DE characteristics, which are obtained by adding an extra scalar degree of freedom in Einstein-Hilbert action. Scalar field provides a basis for many standard inflationary models, leading to an effective candidate of DE. All of these are some peculiar extensions of the -essence models. Although the -essence scalar models are considered to be the general scalar field theories described by the Lagrangian in terms of first-order scalar field derivatives, that is,.
However, Lagrangian with higher-order scalar field derivatives can be taken into account which fixes the equations of motion obtained by metric and scalar field variations of the Lagrangian density to second-order [ 29 , 30 ]. Horndeski [ 29 ] was the pioneer to discuss the concept of most general Lagrangian with single scalar field. Recently, this action is discussed by introducing a covariant Galilean field with second-order equations of motion [ 30 ].
This theory has fascinated many researchers and much work has been done in this context, for example, [ 31 — 35 ]. The energy conditions have many significant theoretical applications like Hawking Penrose singularity conjecture that is based on the strong energy condition [ 36 ], while the dominant energy condition is useful in the proof of positive mass theorem [ 37 ].
Furthermore, null energy condition is a basic ingredient in the derivation of second law of black hole thermodynamics [ 38 ]. On the cosmological grounds, Visser [ 39 ] discussed various cosmological terms like distance modulus, look back time, deceleration, and statefinder parameters in terms of red shift using energy condition constraints.
Cosmology in Scalar-Tensor Gravity covers all aspects of cosmology in scalar- tensor theories of gravity. Considerable Fundamental Theories of Physics. Cosmology in Scalar-Tensor Gravity covers all aspects of cosmology in scalar- tensor Volume of Fundamental Theories of Physics.
These conditions are originally formulated in the context of GR and then extended to modified theories of gravity. Many authors have explored these energy conditions in the framework of modified gravity and found interesting results [ 40 — 43 ]. Basically, modified gravity theories contain some extrafunctions like higher-order derivatives of curvature term or some functions of Einstein tensor or scalar field, and so forth.
Thus it is a point of debate that how one can constrain the added extra degrees of freedom consistently with the recent observations. The energy conditions can be used to put some constraints on these functions that could be consistent with those already found in the cosmological arena.
Recently, these energy conditions have been discussed in [ 44 ] and [ 45 ] theories.
In this paper, we study the energy condition bounds in a most general scalar-tensor theory. The paper is designed in the following layout. Next section defines the energy conditions in GR as well as in a general modified gravitational framework. Section 3 provides basic formulation of the most general scalar-tensor theory. In the same section, we formulate the energy conditions in terms of some cosmological parameters within such modified framework. In Section 4 , we provide some specific cases of this theory and discuss the corresponding constraints.
Finally, we summarize and present some general remarks. In this section, we discuss the energy conditions in GR framework and then express the respective conditions in a general modified gravity. In GR, the energy conditions come from a well-known purely geometric relationship known as Raychaudhuri equation [ 38 , 46 ] together with the lineament of gravitational attractiveness. In a spacetime manifold with vector fields and as tangent vectors to timelike and null-like geodesics of the congruence, the temporal variation of expansion for the respective curves is described by the Raychaudhuri equation as Here , , , and represent the Ricci tensor, expansion, shear, and rotation, respectively, related with the congruence of timelike or null-like geodesics.
The characteristic of the gravity that is attractive leads to the condition.
For infinitesimal distortions and vanishing shear tensor , that is, zero rotation for any hypersurface of orthogonal congruence , we ignore the second-order terms in Raychaudhuri equation, and consequently integration leads to. It further implies that Since GR and its modifications lead to a relationship of the matter contents, that is energy-momentum tensor in terms of Ricci tensor through the field equations, therefore the respective physical conditions on the energy-momentum tensor can be determined as follows: For perfect fluid with density and pressure defined by the strong and null energy conditions, respectively, are defined by the inequalities and , while the weak and dominant energy conditions are defined, respectively, by and.
Raychaudhuri equation being a geometrical statement works for all gravitational theories. Therefore, its interesting features like focussing of geodesic congruences as well as the attractiveness of gravity can be used to derive the energy constraints in the context of modified gravity. In case of modified gravity, we assume that the total matter contents of the universe act like perfect fluid, and consequently these conditions can be defined in terms of effective energy density and pressure matter sources get modified, and we replace and in 3 by and , resp.
These conditions can be regarded as an extension of the respective conditions in GR given by [ 43 ] For a detailed discussion, we suggest the readers to study a recent paper [ 47 ]. The DE requires negative EoS parameter , for the explanation of cosmic expansion.
Indeed, for cosmological purposes, we are curious for a source with ; in that case, all of the energy conditions require [ 48 ]. The role of possible DE candidates with was pointed out by Caldwell, who referred to null DEC violating sources as phantom components. It is argued that DE models with such as the cosmological constant and the quintessence satisfy the NEC, but the models with predicted for instance by the phantom theory , where the kinetic term of the scalar field has a wrong negative sign, does not satisfy.
However, quintom models can also satisfy NEC as they yield the phantom era for a very short period of time [ 49 ]. Usually, the discussions on energy conditions for cosmological constant are available in literature by introducing it in some other type of matter like electromagnetic field [ 50 ].
The cosmological constant will trivially satisfy all these energy conditions except SEC. The most general scalar-tensor theory in 4 dimensions is given by the action [ 31 — 35 ] where is the scalar field, is the determinant of the metric tensor, denotes the matter part of the Lagrangian, and represents the kinetic energy term defined by. The functions and are all arbitrary functions and. In this action, the term is the Galilean term, can yield the Einstein-Hilbert term and leads to the interaction with Gauss-Bonnet term.
This indicates that it covers not only several DE proposals like -essence, gravity, BD theory and Galilean gravity models, but it also contains 4-dimensional Dvali, Gabadadze, and Poratti DGP model modified , the field coupling with Gauss-Bonnet term, and the field derivative coupling with Einstein tensor as its particular cases.
By varying the action 6 with respect to the metric tensor, the gravitational field equation can be written as where is the modified energy-momentum tensor, is the source of usual matter field that can be described by the perfect fluid, while provides the matter source due to scalar field and hence yields the source of DE, defined in the Appendix. The scalar wave equation for such modified gravity has been described in the literature [ 32 — 35 ].
By inverting 7 , the Ricci tensor can be expressed in terms of effective energy-momentum tensor and its trace as follows: Let us consider the spatially homogeneous, isotropic, and flat FRW universe model with as a scale factor described by the metric The background fluid is taken as perfect fluid given by 4 with , and the null like vector is taken as.
Furthermore, we assume that the scalar field is a function of time only. The Friedmann equations for the generalized scalar-tensor theory in terms of effective energy density and pressure are given by [ 32 — 35 ] where Here , being an arbitrary function of and , acts as a dynamical gravitational constant, and it should be positive for any gravitational theory.
Furthermore, and are density and pressure, respectively, for ordinary matter. We shall discuss its different forms in the next section. In a mechanical framework, the terms velocity, acceleration, jerk, and snap parameters are based on the first four time derivatives of position.
In cosmology, the Hubble, deceleration, jerk, and snap parameters are, respectively, defined as In order to have a more precise picture of these conditions 15 , we use the relations of time derivatives of Hubble parameter in terms of cosmological quantities like deceleration, snap, and jerk parameters as Moreover, we assume that the scalar field evolves as a power of scale factor, that is, [ 51 , 52 ], which leads to Here is a nonzero parameter yields constant scalar field, yields expanding scalar field, and corresponds to contracting scalar field.
Clearly, remains as a positive quantity. Introducing these quantities in the energy conditions given by 15 , it follows that These are the most general energy conditions that can yield the energy conditions for various DE models like -essence and modified theories in certain limits. In order to satisfy these conditions, it must be guaranteed that the function is a positive quantity. However, we have discussed earlier that , being a gravitational constant, would be positive in all cases if it is not so, then we impose this condition and restrict the free parameters.
Clearly, these conditions are only dependent on the Hubble, deceleration parameters and arbitrary functions, namely, , , , and. Once these arbitrary functions are specified, the energy bounds on the selected models can be determined by using these conditions. In order to have a better understanding of these constraints, we can use either the power law ansataz for the scale factor, for example, [ 45 ] or we can use the estimation of present values of the respective parameters available in literature.
In this study, we consider the present value of the Hubble parameter , the scale factor , and the deceleration parameter as suggested by Capozziello et al. Since it is well known that the energy constraints are satisfied for usual matter contents like perfect fluid, therefore we shall focus on validity of the energy constraints for the scalar field terms only either we take vacuum case or assume that the energy conditions for ordinary matter hold.
It is interesting to mention here that the respective energy conditions in GR can be recovered by taking the arbitrary functions , and zero with as constant. Now we discuss application of the derived conditions to some particular cases of this theory. The violation of energy conditions leads to various interesting results. In particular, for a canonical scalar field, violation of these conditions yields instabilities and ghost pathologies. It is important to discuss the violation of these energy conditions in order to check the existence of instabilities in Horndeski theory.
The procedure for FRW universe model in most general scalar-tensor theory based on tensor and scalar perturbations is available in literature [ 31 ]. By introducing perturbed metric, it has been shown that for the avoidance of ghost and gradient instabilities, the tensor perturbations suggest while scalar perturbations impose where the quantities and are defined in [ 31 ]. We simply plug the values in these conditions for the following cases and show that violation of energy conditions leads to the existence of ghost instabilities.
The -essence dynamical models of DE play a dominant role in the solution of various problems in cosmological context [ 54 ]. The action 6 can be reduced to the action for -essence model in GR framework defined by with the following choice of the functions: The -essence models can be classified into three forms: For the choice of arbitrary functions given by 22 , the energy conditions 15 take the following forms: In order to see how the function can be constrained by using the previous energy conditions, we choose a particular model of -essence [ 55 ] as follows: In this case, WEC requires the following conditions: For the interpretation of the previous inequalities, we consider the power law ansatz for the scalar field ; , which further yields.
Consequently, the WEC 25 turns out to be. It is difficult to find the admissible ranges of all constants , , , , and from the previous conditions. In order to find the constraints on these parameters, we consider that these conditions are satisfied for ordinary matter, that is, and. Moreover, we take the present value of Hubble parameter and choose some particular values of the constants and to find the ranges of , , and , consistent with the WEC.