Evolution of density perturbations in fðrþ theories of gravity
|
|
- Jonah Warren
- 6 years ago
- Views:
Transcription
1 PHYSICAL REVIEW D 77, 2355 (28) Evolution of density perturbations in fðrþ theories of gravity A. de la Cruz-Dombriz,* A. Dobado, + and A. L. Maroto Departamento de Física Teórica I, Universidad Complutense de Madrid, E-284 Madrid, Spain (Received 29 February 28; published 2 June 28) In the context of fðrþ theories of gravity, we study the evolution of scalar cosmological perturbations in the metric formalism. Using a completely general procedure, we find the exact fourth-order differential equation for the matter density perturbations in the longitudinal gauge. In the case of sub-hubble modes, the expression reduces to a second-order equation which is compared with the standard (quasistatic) equation used in the literature. We show that for general fðrþ functions the quasistatic approximation is not justified. However, for those functions adequately describing the present phase of accelerated expansion and satisfying local gravity tests, it provides a correct description for the evolution of perturbations. DOI:.3/PhysRevD PACS numbers: k, 4.5.Kd, x *dombriz@fis.ucm.es + dobado@fis.ucm.es maroto@fis.ucm.es I. INTRODUCTION The present phase of accelerated expansion of the universe [] poses one of the most important problems of modern cosmology. It is well-known that ordinary Einstein s equations in either a matter or radiation dominated universe give rise to decelerated periods of expansion. In order to have acceleration, the total energymomentum tensor appearing on the right-hand side of the equations should be dominated at late times by a hypothetical negative pressure fluid usually called dark energy (see [2] and references therein). However, there are other possibilities to generate a period of acceleration in which no new sources are included on the right-hand side of the equations, but instead Einstein s gravity itself is modified [3]. In one of such possibilities, new functions of the curvature scalar [fðrþ terms] are included in the gravitational action, which amounts to modifiying the left-hand side of the equations of motion. Although such theories are able to describe the accelerated expansion on cosmological scales correctly, they typically give rise to strong effects on smaller scales. In any case viable models can be constructed to be compatible with local gravity tests and other cosmological constraints [4]. The important question that arises is therefore how to discriminate dark energy models from modified gravities using present or future observations. It is known that by choosing particular fðrþ functions, one can mimic any background evolution (expansion history), and, in particular, that of CDM. Accordingly, the exclusive use of observations such as high-redshift Hubble diagrams from supernovae type Ia [], baryon acoustic oscillations [5] or CMB shift factor [6], based on different distance measurements which are sensitive only to the expansion history, cannot settle the question of the nature of dark energy [7]. However, there exist observations of a different type which are sensitive, not only to the expansion history, but also to the evolution of matter density perturbations. The fact that the evolution of perturbations depends on the specific gravity model, i.e., it differs in general from that of Einstein s gravity even though the background evolution is the same, means that observations of this kind will help distinguish between different models for acceleration. In this work we study the problem of determining the exact equation for the evolution of matter density perturbations for arbitrary fðrþ theories. Such a problem had been previously considered in the literature ([8 3]) and approximated equations have been widely used. They are typically based on the so-called quasistatic approximation in which all the time derivative terms for the gravitational potentials are discarded, and only those including density perturbations are kept [4]. From our exact result, we will be able to determine under which conditions such an approximation can be justified. The paper is organized as follows: In Sec. II, we briefly review the perturbations equations for the standard CDM model. In Sec. III we obtain the perturbed equations for general fðrþ theories. In Sec. IV we describe the procedure to obtain the general equation for the density perturbation. In Sec. V we summarize the main viability condition for fðrþ theories. Section VI is devoted to the study of the validity of the quasistatic approximation. In Sec. VII we apply our results to some particular models, and finally in Sec. VIII we include the main conclusions. In Appendixes A and B we have also included complete expressions for the relevant coefficients of the perturbation equation. II. DENSITY PERTURBATIONS IN CDM Let us start by considering the simplest model for dark energy described by a cosmological constant. The cor =28=77(2)=2355(9) Ó 28 The American Physical Society
2 A. DE LA CRUZ-DOMBRIZ, A. DOBADO, AND A. L. MAROTO PHYSICAL REVIEW D 77, 2355 (28) responding Einstein s equations read G ¼ 8GT ; () where G is the Einstein s tensor and T is the energymomentum tensor for matter. In the metric formalism for the CDM model it is possible to obtain a second-order differential equation for the growth of matter density perturbation =. Let us consider the scalar perturbations of a flat Friedmann- Robertson-Walker metric in the longitudinal gauge and in conformal time: ds 2 ¼ a 2 ðþ½ð þ 2Þd 2 ð 2 Þðdr 2 þ r 2 d 2 2 ÞŠ; (2) where ð; ~xþ and ð; ~xþ are the scalar perturbations. From this metric, we obtain the first-order perturbed Einstein s equation: G ¼ 8GT ; (3) where the perturbed energy-momentum tensor reads T ¼ ¼ ; T i j ¼ Pi j ¼ c2 s i j T i ¼ Ti ¼ ðþc2 i v; (4) with the unperturbed energy density and v the potential for velocity perturbations. We assume that the perturbed and unperturbed matter have the same equation of state, i.e., P= c 2 s P =, where c s ¼ for matter perturbations. The resulting differential equation for in Fourier space is written as þ H k4 6~k 2 8~ 2 k 4 ~ð3k 2 þ 9H 2 Þ ~ k4 þ 9~ð2~ 3H 2 Þ k 2 ð9~ 3H 2 Þ k 4 ~ð3k 2 þ 9H 2 ¼ ; (5) Þ where ~ 4G a 2 ¼ H þ H 2 and H a =a with prime denoting derivative with respect to time. We point out that it is not necessary to explicitly calculate potentials and to obtain Eq. (5), but algebraic manipulations in the field equations are enough to get this result. In the extreme sub-hubble limit, i.e., k or equivalently k H,(5) is reduced to the well-known expression þ H 4G a 2 ¼ : (6) In this regime and at early times, the matter energy density dominates over the cosmological constant, and it is easy to show that solutions for (6) grow as aðþ. At late times (near today) the cosmological constant contribution is not negligible and power-law solutions for (6) no longer exist. It is necessary in this case to assume an ansatz for. One which works very well is the one proposed in [7,5]: ðaþ a ¼ e R a a i ½ m ðaþ Šdlna : (7) This expression fits with high precision the numerical solution for with a constant parameter ¼ 6=. III. PERTURBATIONS IN fðrþ THEORIES Let us consider the modified gravitational action S ¼ Z d 4 p x ffiffiffiffiffiffiffi g ðr þ fðrþþ; (8) 6G where R is the scalar curvature. The corresponding equations of motion read G 2 g fðrþþr f R ðrþ g hf R ðrþþf R ðrþ ; ¼ 8GT ; (9) where f R ðrþ ¼dfðRÞ=dR. For the background flat Robertson-Walker metric they read and 3H a 2 ð þ f R Þ 2 ðr þ f Þ 3H a 2 f R ¼ 8G a 2ðH þ 2H 2 Þð þ f R Þ 2 ðr þ f Þ a 2 ðh f R þ f R Þ () ¼ 8Gc 2 s ; () where R denotes the scalar curvature corresponding to the unperturbed metric, f fðr Þ, f R dfðr Þ=dR, and prime means derivative with respect to time. A very useful equation to use in the following calculations is the () and () combination 2ð þ f R Þð H þ H 2 Þþ2H f R f R ¼ 8G ð þ c 2 sþa 2 : (2) Finally we have the conservation equation þ 3ð þ c2 sþh ¼ : (3) Using the perturbed metric (2) and the perturbed energymomentum tensor (4), the first-order perturbed equations, assuming that the background equations hold, may be written as ð þ f R ÞG þðr þr r hþf RR R þ½ðg Þr r ðg Þr r Šf R ½g ð Þ g ð ÞŠ@ f R ¼ 8GT ; (4) The Riemann tensor definition is þ, which has an opposite sign to the one proposed in [6]
3 EVOLUTION OF DENSITY PERTURBATIONS IN fðrþ... PHYSICAL REVIEW D 77, 2355 (28) where f RR ¼ d 2 fðr Þ=dR 2, h r r, and r is the usual covariant derivative with respect to the unperturbed Friedmann-Robertson-Walker metric (see [6] for perturbed metric, connection symbols, and other useful perturbed quantities). Notice that unlike the ordinary Einstein- Hilbert (EH) case, with second-order equations, this is a set of fourth-order differential equations. By computing the covariant derivative with respect to the perturbed metric r ~ of the perturbed energy-momentum tensor ~T, we find the conservation equations ~r ~T ¼ (5) which do not depend on fðrþ. For the linearized Einstein s equations, the components (), ðiiþ, ðiþ ðiþ, and (ij), where i, j ¼, 2,3,i Þ j, in Fourier space, read, respectively, ð þ f R Þ½ k 2 ð þ Þ 3Hð þ Þ þð3h 6H 2 Þ 3H ŠþfR ð 9H þ 3H 3 Þ ¼ 2~; (6) ð þ f R Þ½ þ þ 3H ð þ Þþ3H þðh þ 2H 2 Þ ŠþfR ð3h H þ 3 Þ þ fr ð3 Þ ¼ 2c 2 s ~; (7) ð þ f R Þ½ þ þ H ð þ ÞŠ þ fr ð2 Þ ¼ 2~ð þ c 2 SÞv; (8) þ H þ k 2 3 3H ¼ ; (23) which will be very useful in future calculations. IV. EVOLUTION OF DENSITY PERTURBATIONS Our porpose is to derive a fourth-order differential equation for matter density perturbation alone. This can be performed by means of the following process. Let us consider Eqs. (6) and (8) for a matter dominated universe i.e., c 2 s ¼, and combine them to express the potentials and in terms of f ; ;; g by means of algebraic manipulations. The resulting expressions are the following: ¼ ½3ð þ f R ÞH ð þ ÞþfR þ 2~Š and ¼ where DðH ;kþ ð þ f R ÞðH fr Þþ ð þ f R Þð þ Þþ 2~ k 2 ð 3 Þ ½ð þ f R Þð k 2 3H Þþ3f R H Š ½ 3ð þ f R ÞH ð þ Þ 3f R DðH ;kþ 2~Š½ð þ f R ÞH þ 2fR ð Š þ f R Þð þ Þþ 2~ k 2 ð 3 Þ ½ð þ f R Þð k 2 þ 3H (24) 6H 2 Þ 9H f R Š ; (25) ¼ f RR R; þ f R (9) where R is given by R ¼ 2 a 2 ½3 þ 6ðH þ H 2 Þ þ 3H ð þ 3 Þ k 2 ð 2 ÞŠ: (2) Finally, from the energy-momentum tensor conservation (5), we get to first order: and 3 ð þ c 2 sþ þ k 2 ð þ c 2 sþv ¼ (2) c2 s þ þ c 2 þ v þ H vð 3c 2 sþ¼ (22) s for the temporal and spatial components, respectively. In a dust matter dominated universe, i.e., c 2 s ¼, (2) and (22) can be combined to give DðH ;kþ 6ð þ f R Þ 2 H 3 þ 3H ½f 2 R þ 2ð þ f R Þ 2 H Šþ3ð þ f R Þf R ð 2H 2 þ k 2 þ H Þ: (26) The second step will be to derive Eqs. (24) and (25) with respect to and obtain and algebraically in terms of f ; ; ; ; g. These last results can be substituted in Eqs. (6) and (8) to obtain potentials and just in terms of f ; ;; ; g. So at this stage we are able to express, but we do not do here explicitly, the following: ¼ ð ; ; ; ; Þ; ¼ ð ; ; ; ; Þ; ¼ ð ; ; ; ; Þ; ¼ ð ; ; ; ; Þ; (27) where we mean that the functions on the left-hand side are algebraically dependent on the functions inside the parenthesis on the right-hand side
4 A. DE LA CRUZ-DOMBRIZ, A. DOBADO, AND A. L. MAROTO PHYSICAL REVIEW D 77, 2355 (28) The natural reasoning at this point would be to try to It is very useful to define the parameter H =k since obtain the potentials second derivatives f ; g in terms it will allow us to perform a perturbative expansion of of f; ; g by an algebraic process. The chosen equations to do so will be (9) and (23), the first derivative with Other dimensionless parameters which will be used are the previous and coefficients in the sub-hubble limit. respect to. In(23) it is necessary to substitute and the following: i H ðiþ =H iþ (i ¼, 2, 3) and f i by the expressions obtained in (27), whereas in (9) the f ðjþ R first derivative may be sketched as follows: =ðh j f R Þ (j ¼, 2). Expressing the and coefficients with those dimensionless quantities we may write ¼ f RR R frr fr þ f RR ð þ f RÞ þ f R ð þ f R Þ 2 R: i;eh ¼ X3 ðjþ i;eh i ¼ ; ; 2; (28) j¼ Before deriving, we are going to substitute the that appears in (9) by lower derivatives potentials f; ; ; g,, and its derivatives. To do so we consider in (6) and (8) the first derivatives with respect to where the quantity v has been previously substituted by its expression in (2). Following this process we may express as follows: ¼ ð; ; ; ; ; ; Þ; (29) and now substituting in (9) we can derive that equation with respect to. Solving a two algebraic equations system with Eqs. (23) and (28) and introducing (27) we are able to express f ; g in terms of f; ; ; g: ¼ ð; ; ; Þ; ¼ ð; ; ; Þ: (3) We substitute the results obtained in (3) straightforwardly in (27) in order to express f; ; ; g in terms of f; ; ; g. With the two potentials and their first derivatives as algebraic functions of f; ; ; g,we perform the last step: we consider ð; ; ; Þ and derive it with respect to. The result should be equal to ð; ; ; Þ, so we only need to express together these two results obtaining a fourth-order differential equation for. Note that this procedure is completely general to first order for scalar perturbations in the metric formalism for fðrþ gravities. Once this fourth-order differential equation has been solved, we may go backward, and by using the results for we obtain f ; g from (3) as functions of time. Analogously from (27) the behavior of the potentials f; g and their first derivatives could be determined. The resulting equation for can be written as follows: 4;f iv þ 3;f þð 2;EH þ 2;f Þ þð ;EH þ ;f Þ þð ;EH þ ;f Þ ¼ ; (3) where the coefficients i;f (i ¼ ;...; 4) involve terms with fr and f R, i.e., terms disappearing if we take f R constant. Equivalently, i;eh (i ¼,, 2) contain terms coming from the linear part of f in R. i;f ¼ X7 j¼ i;f ¼ X8 j¼ ðjþ i;f i ¼ 3; 4; ðjþ i;f i ¼ ; ; 2; (32) where two consecutive terms in each series differ in the 2 factor. The expressions for the coefficients are too long to be written explicitly. Instead, in the following sections we will show different approximated formulas useful in certain limits. V. VIABLE fðrþ THEORIES Results obtained so far are valid for any fðrþ theory. However, as mentioned in the introduction, this kind of model is severely constrained in order to provide consistent theories of gravity. In this section we review the main conditions [9]: () f RR > for high curvatures [7]. This is the requirement for a classically stable high-curvature regime and the existence of a matter dominated phase in the cosmological evolution. (2) þ f R > for all R. This condition ensures the effective Newton s constant to be positive at all times and the graviton energy to be positive. (3) f R < ensures ordinary general relativity behavior is recovered at early times. Together with the condition f RR >, it implies that f R should be a negative and monotonically growing function of R in the range <f R <. (4) jf R jat recent epochs. This is imposed by local gravity tests [7], although it is still not clear what is the actual limit on this parameter. This condition also implies that the cosmological evolution at late times resembles that of CDM. In any case, this constraint is not required if we are only interested in building models for cosmic acceleration. VI. EVOLUTION OF SUB-HUBBLE MODES AND THE QUASISTATIC APPROXIMATION We are interested in the possible effects on the growth of density perturbations once they enter the Hubble radius in the matter dominated era. In the sub-hubble limit,it
5 EVOLUTION OF DENSITY PERTURBATIONS IN fðrþ... PHYSICAL REVIEW D 77, 2355 (28) can be seen that the 4;f and 3;f coefficients are suppressed by 2 with respect to 2;f, ;f, and ;f, i.e., in this limit the equation for perturbations reduces to the following second-order expression: þ H þ ð þ f RÞ 5 H 2 ð þ Þð2 2 Þ 6 a 8 f 4 RR ð 2 2Þk 8 8G a 2 ð þ f R Þ 5 ð þ Þþ 24 a 8 f 4 RR ð þ f RÞð 2 2Þk 8 ¼ ; (33) where we have taken only the leading terms in the expansion for the and coefficients. This expression can be compared with that usually considered in literature, obtained after performing strong simplifications in the perturbed equations (6) (9), (2), and (22) by neglecting time derivatives of and potentials (see [4]). Thus in [,8] the authors obtain þ H þ 4 k2 a 2 þ 3 k2 a 2 f RR þf R f RR þf R ~ þ f R ¼ : (34) This approximation has been considered as too aggressive in [] since neglecting time derivatives can remove important information about the evolution. Note also that there exists a difference in a power k 8 between those terms coming from the f part and those coming from the EH part in (33). This result differs from that in the quasistatic approximation where difference is in a power k 2 according to (34). In order to compare the evolution for both equations, we have considered a specific function f test ðrþ ¼ 4R :63, where H 2 units have been used, which gives rise to a matter era followed by a late-time accelerated phase with the correct deceleration parameter today. Initial conditions in the matter era were given at redshift z ¼ 485 where the EH part was dominant. Results for k ¼ 6H are presented in Fig.. We see that, as expected, both expressions give rise to the same evolutions at early times (large redshifts) where they also agree with the standard CDM evolution. However, at late times the quasistatic approximation fails to correctly describe the evolution of perturbations. Notice that the model example satisfies all the viability conditions described in the previous section except for the local gravity tests. As we will show in the following, it is precisely this last condition jf R j that will ensure the validity of the quasistatic approximation. We will now restrict ourselves to models satisfying all the viability conditions, including jf R j. In Appendix A we have reproduced all the and the first four coefficients for each term in (3). These are the dominant ones for sub-hubble modes (i.e., ) once the condition jf R j has been imposed. Thus, keeping only P 4 j¼ ðjþ i¼;...;4;f and ðþ i¼;;2;eh as the relevant contributions for the general coefficients, the full differential equation (3) can be simplified as c 4 iv þ c 3 þ c 2 þ c þ c ¼ ; (35) where the c coefficients are written in Appendix B. We see that indeed in the sub-hubble limit the c 4 and c 3 coefficients are negligible and the equation can be reduced to a second-order expression. As a consistency check, we find that both in a matter dominated universe and in CDM all coefficients vanish identically since f, f 2. For these cases, Eq. (3) becomes Eq. (6) as expected. For instance, in the pure matter dominated case, the coefficients are constant, and they take the following values: ¼ =2, 2 ¼ =2, 3 ¼ 3=4, and 4 ¼ 3=2. Another important feature from our results is that, in general, without imposing jf R j, the quotient ð ;EH þ ;f Þ=ð 2;EH þ 2;f Þ is not always equal to H. In fact only the quotients ðþ ;EH =ðþ 2;EH and ðþ ;f =ðþ 2;f are identically equal to H, which is in agreement with the coefficient in (6). However, for our approximated expressions it is true that c =c 2 H. From expressions in Appendix B, the second-order equation for becomes þ H 4 3 which can also be written as qffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffi qffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffi þ 9 a 2 4 ð þ 2 ÞŠ½ 6f RRk 2 þ 9 a 2 4 ð þ þ 2 ÞŠ qffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffi qffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffi ð ÞH 2 ¼ ; (36) þ 5 a 2 2 ð 24 þ 25 ÞŠ½ 6f RRk 2 þ 5 a 2 2 ð þ 24 þ 25 ÞŠ ½ 6f RRk 2 ½ 6f RRk 2 þ H 4 3 2þ 2 2þ 2 ð 6f RRk 2 þ 9 a 2 4 Þ2 8 6 þ þ 2 ð 6f RRk 2 þ 5 a 2 2 Þ þ 6 ð þ ÞH 2 ¼ : (37) 2þ
6 A. DE LA CRUZ-DOMBRIZ, A. DOBADO, AND A. L. MAROTO PHYSICAL REVIEW D 77, 2355 (28) k = h Mpc - quasistatic ΛCDM k =.67 h Mpc - quasistatic ΛCDM k k z FIG.. k with k ¼ :2 h Mpc for f test ðrþ model and CDM. Both standard quasistatic evolution and Eq. (33) have been plotted in the redshift range from to. Note that the quasistatic expression (34) is only recovered in the matter era (i.e., for H ¼ 2=) or for a pure CDM evolution for the background dynamics. Nevertheless in the considered limit j f R j it can be proven using the background equations of motion that þ 2 (38) and therefore þ 2 þ, which allows simplifying expression (37) to approximately become (34). This is nothing but the fact that for viable models the background evolution resembles that of CDM [9]. In other words, although for general fðrþ functions the quasistatic approximation is not justified, for those viable functions describing the present phase of accelerated expansion and satisfying local gravity tests, it gives a correct description for the evolution of perturbations. VII. SOME PROPOSED MODELS In order to check the results obtained in the previous section, we propose two particular fðrþ theories which allow us to determine at least numerically all the quantities involved in the calculations and therefore to obtain solutions for (3). As commented before, for viable models the background evolution resembles that of CDM at low redshifts and that of a matter dominated universe at high redshifts, i.e., the quantity ðr þ fðrþþ=r tends to one in the high-curvature regime. Nevertheless the fðrþ contribution gives the dominant contribution to the gravitational action for small curvatures, and therefore it may explain the cosmological acceleration. For the sake of concreteness we will fix the model parameters imposing a deceleration parameter today q :6. Thus, our first model (A) will be fðrþ ¼c R p. According to the results presented in [2,9] viable models of this type include both a matter dominated and late-time accelerated universe provided the parameters satisfy c < and <p<. We have chosen c ¼ 4:3 and p ¼ : in H 2 units. This choice does verify all the viability conditions, including jf R j today. For the second model (B), fðrþ ¼ c R e þc 2, we have chosen c ¼ 2:5 4, e ¼ :3, and c 2 ¼ :22 also in the same units. For each model, we compare our result (36) with the standard CDM and the quasistatic approximation (34) (see Figs. 2 and 3). In both cases, the initial conditions are given at redshift z ¼ where is assumed to behave as in a matter dominated universe, i.e., k ðþ /aðþ with no k dependence. We see that for both models the quasistatic k... k =.67 h Mpc - +z +z quasistatic ΛCDM FIG. 2. k with k ¼ :67 h Mpc for fðrþ model A evolving according to (36), CDM and quasistatic approximation given by Eq. (34) in the redshift range from to. The quasistatic evolution is indistinguishable from that coming from (36), but diverges from CDM behavior as z decreases.. FIG. 3. k with k ¼ :67 h Mpc for fðrþ model B evolving according to (36), CDM and quasistatic evolution given by Eq. (34) in the redshift range from to. The quasistatic evolution is indistinguishable from that coming from (36), but diverges from CDM behavior as z decreases
7 EVOLUTION OF DENSITY PERTURBATIONS IN fðrþ... PHYSICAL REVIEW D 77, 2355 (28) today (k) k/h today (k) f(r) model A today (k) f(r) model B FIG. 4. Scale dependence of k evaluated today (z ¼ ) for k=h in the range from to 4. approximation gives a correct description for the evolution which clearly deviates from the CDM case. In Fig. 4 the density contrast evaluated today was plotted as a function of k for both models. The growing dependence of with respect to k is verified. This modified k dependence with respect to the standard matter dominated universe could give rise to observable consequences in the matter power spectrum, as shown in [3], and could be used to constrain or even discard fðrþ theories for cosmic acceleration. VIII. CONCLUSIONS In this work we have studied the evolution of matter density perturbations in fðrþ theories of gravity. We have presented a completely general procedure to obtain the exact fourth-order differential equation for the evolution of perturbations. We have shown that for sub-hubble modes the expression reduces to a second-order equation..9 We have compared this result with that obtained within the quasistatic approximation used in the literature and found that for arbitrary fðrþ functions such an approximation is not justified. However, if we limit ourselves to theories for which jf R j today, then the perturbative calculation for sub- Hubble modes requires taking into account, not only the first terms, but also higher-order terms in ¼ H =k. In that case, the resummation of such terms modifies the equation which can be seen to be equivalent to the quasistatic case but only if the universe expands as in a matter dominated phase or in a CDM model. Finally, the fact that for models with jf R j the background behaves today precisely as that of CDM makes the quasistatic approximation correct in those cases. ACKNOWLEDGMENTS We would like to thank A. Starobinsky for useful comments and J. A. R. Cembranos and J. Beltrán for their continuous encouragement. This work has been partially supported by the DGICYT (Spain) under projects FPA , FPA , and CAM/UCM 939 and by UCM-Santander PR34/ APPENDIX A: AND COEFFICIENTS Coefficients for the iv term: ðþ 4;f 8f4 R ð þ f RÞ 6 f 42 ; 4;f 72f3 R f3 4 ð 2 þ 2 Þ; 4;f 26f2 R f2 6 ð 2 þ 2 Þ 2 ; 4;f 26f Rf 8 ð 2 þ 2 Þ 3 : Coefficients for the term: (A) ðþ 3;f 8f4 R ð þ f RÞ 5 f 4H 2 ½3 þ f R ð3 þ f ÞŠ; 3;f 6f3 R f2 H 4 f8f 2 ð 2 þ 2 Þþ4f ½2 þ 9 2 2ð9 þ 3 ÞŠg; 3;f 72f2 R f H 6 ð 2 þ 2 Þ½ 4f 2 ð 2 þ 2 Þþf ð þ 4 3 ÞŠ; 3;f 26f RH 8 ð 2 þ 2 Þ 2 ½ 2f 2 ð 2 þ 2 Þþf ð7 4 2 þ 2 3 ÞŠ: (A2) Coefficients for the term: ðþ 2;EH ¼ 432ð þ f RÞ H 2 8 ð þ Þð 2 þ 2 Þ 3 ; 2;EH ¼ 296ð þ f RÞ H 2 ð þ Þ 2 ð 2 þ 2 Þ 3 ; 2;EH ¼ 3888ð þ f RÞ H 2 2 ð þ Þ 2 ð 2 þ 2 Þ 3 ; ðþ 2;f 8f4 R ð þ f RÞ 6 f 4H 2 ; 2;f 88f3 R f3 H 2 2 ð 2 þ 2 Þ; 2;f 24f2 R f2 H 2 4 ð 2 þ 2 Þð 28 þ 2 þ 3 2 Þ; 2;f 72f Rf H 2 6 ð 2 þ 2 Þ 2 ð 4 þ 4 þ 5 2 Þ: Coefficients for the term: (A3)
8 A. DE LA CRUZ-DOMBRIZ, A. DOBADO, AND A. L. MAROTO PHYSICAL REVIEW D 77, 2355 (28) ðþ ;EH ¼ 432ð þ f RÞ H 3 8 ð þ Þð 2 þ 2 Þ 3 ; ;EH ¼ 2592ð þ f RÞ H 3 ð þ Þ 2 ð 2 þ 2 Þ 3 ; ;EH ¼ 7776ð þ f RÞ H 3 2 ð þ Þ 3 ð 2 þ 2 Þ 3 ; ðþ ;f 8f4 R ð þ f RÞ 6 f 4H 3 ; ;f 88f3 R f3 H 3 2 ð 2 þ 2 Þ; ;f 24f2 R f2 H 3 4 ð 2 þ 2 Þð 28 þ 2 þ 3 2 Þ; ;f 72f Rf H 3 6 ð 2 þ 2 Þ 2 ð 4 þ 4 þ 5 2 Þ: Coefficients for the term: ðþ ;EH ¼ 432ð þ f RÞ H 4 8 ð þ Þð2 2 Þð 2 þ 2 Þ 3 ; ;EH ¼ 296ð þ f RÞ H 4 ð þ Þ 2 ð þ 4 2 Þð 2 þ 2 Þ 3 ; ;EH ¼ 3888ð þ f RÞ H 4 2 ð þ Þ 2 ð2 2 2Þð 2 þ 2 Þ 3 ; (A4) ðþ ;f 6 3 f4 R ð þ f RÞ 5 f 4H 4 ½2 þ f R ð2 þ 2f f 2 2 Þ 2 Š; ;f 2f3 R f3 H 4 2 ð þ Þð 2 þ 2 Þ; ;f 48f2 R f2 H 4 4 ð þ Þð 2 þ 2 Þð 6 þ 2 þ 7 2 Þ; ;f 44f Rf H 4 6 ð þ Þð 2 þ 2 Þ 2 ð 6 þ 4 þ 2 Þ: (A5) APPENDIX B: c COEFFICIENTS c 4 ¼ f R f ½ f R f k 2 3H 2 ð 2 þ 2 ÞŠ 3 ; c 3 ¼ 3f R H ½ f R f k 2 3H 2 ð 2 þ 2 ÞŠffR 2 f3 k4 þ 6f 2 H 4 ð 2 þ 2 Þ 2 þ f H 2 ð 2 þ 2 Þ½2f R f 2 k 2 þ 3H 2 ð 7 þ þ ÞŠ þ 2f R f H 2 k 2 ð 6 þ 6 þ Þg; c 2 ¼½ f R f k 2 3H 2 ð 2 þ 2 ÞŠ 2 ½fR 2 f2 k4 þ 5f R f H 2 k 2 ð 2 þ 2 Þþ6H 4 ð þ Þð 2 þ 2 ÞŠ; c ¼ H c 2 ; c ¼ 2 3 H 2 ð þ Þ½ f R f k 2 3H 2 ð 2 þ 2 ÞŠ 2 ½2fR 2 f2 k4 þ 9f R f H 2 k 2 ð 2 þ 2 Þþ9H 4 ð2 2 Þð 2 þ 2 ÞŠ: (B) [] A. G. Riess et al. (Supernova Search Team Collaboration), Astron. J. 6, 9 (998); S. Perlmutter et al. (Supernova Cosmology Project Collaboration), Astrophys. J. 57, 565 (999). [2] E. J. Copeland, M. Sami, and S. Tsujikawa, Int. J. Mod. Phys. D 5, 753 (26). [3] S. M. Carroll, V. Duvvuri, M. Trodden, and M. S. Turner, Phys. Rev. D 7, (24); S. M. Carroll et al., Phys. Rev. D 7, 6353 (25); A. Dobado and A. L. Maroto, Phys. Rev. D 52, 895 (995); G. Dvali, G. Gabadadze, and M. Porrati, Phys. Lett. B 485, 28 (2); A. de la Cruz-Dombriz and A. Dobado, Phys. Rev. D 74, 875 (26); J. A. R. Cembranos, Phys. Rev. D 73, 6429 (26); S. Nojiri and S. D. Odintsov, Int. J. Geom. Methods Mod. Phys. 4, 5 (27). [4] T. P. Sotiriou, Gen. Relativ. Gravit. 38, 47 (26); O. Mena, J. Santiago, and J. Weller, Phys. Rev. Lett. 96, 43 (26); V. Faraoni, Phys. Rev. D 74, (26); S. Nojiri and S. D. Odintsov, Phys. Rev. D 74, 865 (26); I. Sawicki and W. Hu, Phys. Rev. D 75, 2752 (27). [5] D. J. Eisenstein et al., Astrophys. J. 633, 56 (25). [6] D. N. Spergel et al. (WMAP Collaboration), Astrophys. J. Suppl. Ser. 7, 377 (27). [7] E. Linder, Phys. Rev. D 72, (25). [8] J. M. Bardeen, Phys. Rev. D 22, 882 (98); J. C. Hwang and H. Noh, Phys. Rev. D 54, 46 (996); S. M. Carroll, I. Sawicki, A. Silvestri, and M. Trodden, New J. Phys. 8, 323 (26); Y. S. Song, W. Hu, and I. Sawicki, Phys. Rev. D 75, 444 (27); S. Carloni, P. K. S. Dunsby, and A. Troisi, Phys. Rev. D 77, 2424 (28); S. Tsujikawa, Phys. Rev. D 77, 2357 (28); S. Tsujikawa, K. Uddin, and R. Tavakol, Phys. Rev. D 77, 437 (28). [9] L. Pogosian and A. Silvestri, Phys. Rev. D 77, 2353 (28). [] P. Zhang, Phys. Rev. D 73, 2354 (26). [] R. Bean, D. Bernat, L. Pogosian, A. Silvestri, and M. Trodden, Phys. Rev. D 75, 642 (27)
9 EVOLUTION OF DENSITY PERTURBATIONS IN fðrþ... PHYSICAL REVIEW D 77, 2355 (28) [2] L. Amendola, R. Gannouji, D. Polarski, and S. Tsujikawa, Phys. Rev. D 75, 8354 (27). [3] A. A. Starobinsky, JETP Lett. 86, 57 (27). [4] B. Boisseau, G. Esposito-Farese, D. Polarski, and A. A. Starobinsky, Phys. Rev. Lett. 85, 2236 (2); G. Esposito-Farese and D. Polarski, Phys. Rev. D 63, 6354 (2). [5] D. Huterer and E. Linder, Phys. Rev. D 75, 2359 (27). [6] M. Giovannini, Int. J. Mod. Phys. D 4, 363 (25). [7] W. Hu and I. Sawicki, Phys. Rev. D 76, 644 (27). [8] S. Tsujikawa, Phys. Rev. D 76, 2354 (27). [9] I. Sawicki and W. Hu, Phys. Rev. D 75, 2752 (27)
Cosmological perturbations in f(r) theories
5 th IBERIAN COSMOLOGY MEETING 30 th March 2010, Porto, Portugal Cosmological perturbations in f(r) theories Álvaro de la Cruz-Dombriz Theoretical Physics Department Complutense University of Madrid in
More informationThermodynamics in modified gravity Reference: Physics Letters B 688, 101 (2010) [e-print arxiv: [gr-qc]]
Thermodynamics in modified gravity Reference: Physics Letters B 688, 101 (2010) [e-print arxiv:0909.2159 [gr-qc]] HORIBA INTERNATIONAL CONFERENCE COSMO/CosPA 2010 Hongo campus (Koshiba Hall), The University
More informationCosmic vector for dark energy: Constraints from supernovae, cosmic microwave background, and baryon acoustic oscillations
PHYSICAL REVIEW D 8, 234 (29) Cosmic vector for dark energy: Constraints from supernovae, cosmic microwave background, and baryon acoustic oscillations Jose Beltrán Jiménez, Ruth Lazkoz, 2 and Antonio
More informationSergei D. Odintsov (ICREA and IEEC-CSIC) Misao Sasaki (YITP, Kyoto University and KIAS) Presenter : Kazuharu Bamba (KMI, Nagoya University)
Screening scenario for cosmological constant in de Sitter solutions, phantom-divide crossing and finite-time future singularities in non-local gravity Reference: K. Bamba, S. Nojiri, S. D. Odintsov and
More informationThermodynamics in Modified Gravity Theories Reference: Physics Letters B 688, 101 (2010) [e-print arxiv: [gr-qc]]
Thermodynamics in Modified Gravity Theories Reference: Physics Letters B 688, 101 (2010) [e-print arxiv:0909.2159 [gr-qc]] 2nd International Workshop on Dark Matter, Dark Energy and Matter-antimatter Asymmetry
More informationA rotating charged black hole solution in f (R) gravity
PRAMANA c Indian Academy of Sciences Vol. 78, No. 5 journal of May 01 physics pp. 697 703 A rotating charged black hole solution in f R) gravity ALEXIS LARRAÑAGA National Astronomical Observatory, National
More informationDomain wall solution and variation of the fine structure constant in F(R) gravity
Domain wall solution and variation of the fine structure constant in F(R) gravity Reference: K. Bamba, S. Nojiri and S. D. Odintsov, Phys. Rev. D 85, 044012 (2012) [arxiv:1107.2538 [hep-th]]. 2012 Asia
More informationTESTING GRAVITY WITH COSMOLOGY
21 IV. TESTING GRAVITY WITH COSMOLOGY We now turn to the different ways with which cosmological observations can constrain modified gravity models. We have already seen that Solar System tests provide
More informationCrossing of Phantom Divide in F(R) Gravity
Crossing of Phantom Divide in F(R) Gravity Reference: Phys. Rev. D 79, 083014 (2009) [arxiv:0810.4296 [hep-th]] International Workshop on Dark Matter, Dark Energy and Matter-antimatter Asymmetry at National
More informationFuture crossing of the phantom divide in f(r) gravity
Future crossing of the phantom divide in f(r) gravity Reference: K. Bamba, C. Q. Geng and C. C. Lee, JCAP 1011, 001 (2010) [arxiv:1007.0482 [astro-ph.co]]. Two-day workshop in the YITP molecule-type workshop
More informationCMB Tensor Anisotropies in Metric f (R) Gravity
CMB Tensor Anisotropies in Metric f (R) Gravity Hassan Bourhrous,, Álvaro de la Cruz-Dombriz, and Peter Dunsby, Astrophysics, Cosmology and Gravity Centre (ACGC), University of Cape Town, 7701 Rondebosch,
More informationTheoretical Models of the Brans-Dicke Parameter for Time Independent Deceleration Parameters
Theoretical Models of the Brans-Dicke Parameter for Time Independent Deceleration Parameters Sudipto Roy 1, Soumyadip Chowdhury 2 1 Assistant Professor, Department of Physics, St. Xavier s College, Kolkata,
More informationarxiv: v1 [gr-qc] 22 Apr 2008
Noether symmetry in f(r) cosmology Babak Vakili Department of Physics, Shahid Beheshti University, Evin, Tehran 19839, Iran June 6, 008 arxiv:0804.3449v1 [gr-qc] Apr 008 Abstract The Noether symmetry of
More informationHolographic unification of dark matter and dark energy
Holographic unification of dark matter and dark energy arxiv:1101.5033v4 [hep-th] 2 Feb 2011 L.N. Granda Departamento de Fisica, Universidad del Valle, A.A. 25360 Cali, Colombia Departamento de Fisica,
More informationA Study of the Variable Equation-of-State Parameter in the Framework of Brans-Dicke Theory
International Journal of Pure and Applied Physics. ISSN 0973-1776 Volume 13, Number 3 (2017), pp. 279-288 Research India Publications http://www.ripublication.com A Study of the Variable Equation-of-State
More informationModified Gravity and the Accelerating Universe Sean Carroll
Modified Gravity and the Accelerating Universe Sean Carroll Something is making the universe accelerate. Could gravity be the culprit, and if so how will we know? Degrees of Freedom We live in a low-energy
More informationD. f(r) gravity. φ = 1 + f R (R). (48)
5 D. f(r) gravity f(r) gravity is the first modified gravity model proposed as an alternative explanation for the accelerated expansion of the Universe [9]. We write the gravitational action as S = d 4
More informationf(r) theory, Cosmology and Beyond
f(r) theory, Cosmology and Beyond Li-Fang Li The institute of theoretical physics, Chinese Academy of Sciences 2011-7-30 1 / 17 Outline 1 Brief review of f(r) theory 2 Higher dimensional f(r) theory: case
More informationBIANCHI TYPE I ANISOTROPIC UNIVERSE WITHOUT BIG SMASH DRIVEN BY LAW OF VARIATION OF HUBBLE S PARAMETER ANIL KUMAR YADAV
BIANCHI TYPE I ANISOTROPIC UNIVERSE WITHOUT BIG SMASH DRIVEN BY LAW OF VARIATION OF HUBBLE S PARAMETER ANIL KUMAR YADAV Department of Physics, Anand Engineering College, Keetham, Agra -282 007, India E-mail:
More informationReconstruction of f(r) Gravity with Ordinary and Entropy-Corrected (m, n)-type Holographic Dark Energy Model
Commun. Theor. Phys. 66 016) 149 154 Vol. 66, No. 1, July 1, 016 Reconstruction of fr) Gravity with Ordinary and Entropy-Corrected m, n)-type Holographic Dark Energy Model Prabir Rudra Department of Mathematics,
More informationModified Gravity and Dark Matter
Modified Gravity and Dark Matter Jose A. R. Cembranos University Complutense of Madrid, Spain J. Cembranos, PRL102:141301 (2009) Modifications of Gravity We do not know any consistent renormalizable Quantum
More informationModified holographic Ricci dark energy model and statefinder diagnosis in flat universe.
Modified holographic Ricci dark energy model and statefinder diagnosis in flat universe. Titus K Mathew 1, Jishnu Suresh 2 and Divya Divakaran 3 arxiv:1207.5886v1 [astro-ph.co] 25 Jul 2012 Department of
More informationarxiv: v2 [gr-qc] 2 Dec 2009
Solar System Constraints on a Cosmologically Viable f(r) Theory Yousef Bisabr arxiv:0907.3838v2 [gr-qc] 2 Dec 2009 Department of Physics, Shahid Rajaee Teacher Training University, Lavizan, Tehran 16788,
More informationF(T) gravity from higher dimensional theories and its cosmology
F(T) gravity from higher dimensional theories and its cosmology Main reference: arxiv:1304.6191 [gr-qc]. To appear in Phys. Lett. B. KMI-IEEC Joint International Workshop -- Inflation, Dark Energy, and
More informationarxiv: v2 [gr-qc] 24 Nov 2014
Kaluza-Klein cosmological model in f(r, T ) gravity with Λ(T ) P.K. Sahoo, B. Mishra, S.K. Tripathy A class of Kaluza-Klein cosmological models in f(r, T ) theory of gravity have been investigated. In
More informationInevitable Ghost and the Degrees of Freedom in f(r, G) Gravity
503 Progress of Theoretical Physics, Vol., No. 3, September 00 Inevitable Ghost and the Degrees of Freedom in fr, G Gravity Antonio De Felice and Takahiro Tanaka Department of Physics, Tokyo University
More informationarxiv:gr-qc/ v5 2 Mar 2006
Acceleration of the universe in the Einstein frame of a metric-affine f(r) gravity arxiv:gr-qc/0510007v5 2 Mar 2006 Nikodem J. Pop lawski Department of Physics, Indiana University, 727 East Third Street,
More informationCosmology: An Introduction. Eung Jin Chun
Cosmology: An Introduction Eung Jin Chun Cosmology Hot Big Bang + Inflation. Theory of the evolution of the Universe described by General relativity (spacetime) Thermodynamics, Particle/nuclear physics
More informationf (R) Cosmology and Dark Matter
f (R) Cosmology and Dark Matter Dark side of the Universe Kyoto, December 14-18, 2015 G. Lambiase Università di Salerno Dipartimento di Fisica E.R. Caianiello & INFN - Naples Italy in collaboration with
More informationConstraining Modified Gravity and Coupled Dark Energy with Future Observations Matteo Martinelli
Coupled Dark University of Rome La Sapienza Roma, October 28th 2011 Outline 1 2 3 4 5 1 2 3 4 5 Accelerated Expansion Cosmological data agree with an accelerated expansion of the Universe d L [Mpc] 16000
More informationFRW models in the conformal frame of f(r) gravity
Journal of Physics: Conference Series FRW models in the conformal frame of fr gravity To cite this article: J Miritzis 2011 J. Phys.: Conf. Ser. 283 012024 View the article online for updates and enhancements.
More informationarxiv: v1 [gr-qc] 9 Sep 2011
Holographic dark energy in the DGP model Norman Cruz Departamento de Física, Facultad de Ciencia, Universidad de Santiago, Casilla 307, Santiago, Chile. Samuel Lepe arxiv:1109.2090v1 [gr-qc] 9 Sep 2011
More informationwith Matter and Radiation By: Michael Solway
Interactions of Dark Energy with Matter and Radiation By: Michael Solway Advisor: Professor Mike Berger What is Dark Energy? Dark energy is the energy needed to explain the observed accelerated expansion
More informationCould dark energy be modified gravity or related to matter?
Could dark energy be modified gravity or related to matter? Rachel Bean Cornell University In collaboration with: David Bernat (Cornell) Michel Liguori (Cambridge) Scott Dodelson (Fermilab) Levon Pogosian
More informationThe early and late time acceleration of the Universe
The early and late time acceleration of the Universe Tomo Takahashi (Saga University) March 7, 2016 New Generation Quantum Theory -Particle Physics, Cosmology, and Chemistry- @Kyoto University The early
More informationQuintessence and scalar dark matter in the Universe
Class. Quantum Grav. 17 (2000) L75 L81. Printed in the UK PII: S0264-9381(00)50639-X LETTER TO THE EDITOR Quintessence and scalar dark matter in the Universe Tonatiuh Matos and L Arturo Ureña-López Departamento
More informationAdvantages and unexpected shortcomings of extended theories of gravity
Institute of Theoretical Physics, Heidelberg June 17 2015 Advantages and unexpected shortcomings of extended theories of gravity Álvaro de la Cruz-Dombriz Collaborators: J. Beltrán, V. Busti, P. K. S.
More informationDark Energy and Dark Matter Interaction. f (R) A Worked Example. Wayne Hu Florence, February 2009
Dark Energy and Dark Matter Interaction f (R) A Worked Example Wayne Hu Florence, February 2009 Why Study f(r)? Cosmic acceleration, like the cosmological constant, can either be viewed as arising from
More informationToward a Parameterized Post Friedmann. Description of Cosmic Acceleration
Toward a Parameterized Post Friedmann Description of Cosmic Acceleration Wayne Hu NYU, October 2006 Cosmic Acceleration Cosmic acceleration, like the cosmological constant, can either be viewed as arising
More informationBraneworlds: gravity & cosmology. David Langlois APC & IAP, Paris
Braneworlds: gravity & cosmology David Langlois APC & IAP, Paris Outline Introduction Extra dimensions and gravity Large (flat) extra dimensions Warped extra dimensions Homogeneous brane cosmology Brane
More informationLecture on Modified Gravity Theories
Lecture on Modified Gravity Theories Main references: [1] K. Bamba, S. Nojiri, S. D. Odintsov and M. Sasaki, Gen. Relativ. Gravit. 44, 1321 (2012) [arxiv:1104.2692 [hep-th]]. [2] K. Bamba, R. Myrzakulov,
More informationarxiv:astro-ph/ v3 31 Mar 2006
astro-ph/61453 Observational constraints on the acceleration of the Universe Yungui Gong College of Electronic Engineering, Chongqing University of Posts and Telecommunications, Chongqing 465, China and
More information4 Evolution of density perturbations
Spring term 2014: Dark Matter lecture 3/9 Torsten Bringmann (torsten.bringmann@fys.uio.no) reading: Weinberg, chapters 5-8 4 Evolution of density perturbations 4.1 Statistical description The cosmological
More informationStability of the Einstein static universe in the presence of vacuum energy
PHYSICAL REVIEW D 80, 043528 (2009) Stability of the Einstein static universe in the presence of vacuum energy Saulo Carneiro 1,2, * and Reza Tavakol 1, 1 Astronomy Unit, School of Mathematical Sciences,
More informationAntonio L. Maroto Complutense University Madrid Modern Cosmology: Early Universe, CMB and LSS Benasque, August 3-16, 2014
Antonio L. Maroto Complutense University Madrid Modern Cosmology: Early Universe, CMB and LSS Benasque, August 3-16, 2014 A.L.M and F. Prada to appear Albareti, Cembranos, A.L.M. arxiv:1404.5946 and 1405.3900
More informationCosmic Acceleration from Modified Gravity: f (R) A Worked Example. Wayne Hu
Cosmic Acceleration from Modified Gravity: f (R) A Worked Example Wayne Hu Aspen, January 2009 Outline f(r) Basics and Background Linear Theory Predictions N-body Simulations and the Chameleon Collaborators:
More informationIntroduction to Cosmology
Introduction to Cosmology João G. Rosa joao.rosa@ua.pt http://gravitation.web.ua.pt/cosmo LECTURE 2 - Newtonian cosmology I As a first approach to the Hot Big Bang model, in this lecture we will consider
More informationRelic Gravitons, Dominant Energy Condition and Bulk Viscous Stresses
TUPT-03-99 april 1999 arxiv:gr-qc/9903113v1 31 Mar 1999 Relic Gravitons, Dominant Energy Condition and Bulk Viscous Stresses Massimo Giovannini 1 Institute of Cosmology, Department of Physics and Astronomy
More informationTesting vector-tensor gravity with current cosmological observations
Journal of Physics: Conference Series PAPER OPEN ACCESS Testing vector-tensor gravity with current cosmological observations To cite this article: Roberto Dale and Diego Sáe 15 J. Phys.: Conf. Ser. 1 View
More informationSteady-State Cosmology in the Yilmaz Theory of Gravitation
Steady-State Cosmology in the Yilmaz Theory of ravitation Abstract H. E. Puthoff Institute for Advanced Studies at Austin 43 W. Braker Ln., Suite 3 Austin, Texas 78759 Yilmaz has proposed a modification
More informationarxiv:astro-ph/ v3 18 Apr 2005
Phantom Thermodynamics Revisited A. Kwang-Hua CHU P.O. Box 30-15, Shanghai 200030, PR China arxiv:astro-ph/0412704v3 18 Apr 2005 Abstract Although generalized Chaplygin phantom models do not show any big
More informationParameterizing. Modified Gravity. Models of Cosmic Acceleration. Wayne Hu Ann Arbor, May 2008
Parameterizing Modified Gravity Models of Cosmic Acceleration Wayne Hu Ann Arbor, May 2008 Parameterizing Acceleration Cosmic acceleration, like the cosmological constant, can either be viewed as arising
More informationCMB Polarization in Einstein-Aether Theory
CMB Polarization in Einstein-Aether Theory Masahiro Nakashima (The Univ. of Tokyo, RESCEU) With Tsutomu Kobayashi (RESCEU) COSMO/CosPa 2010 Introduction Two Big Mysteries of Cosmology Dark Energy & Dark
More informationarxiv:gr-qc/ v2 14 Mar 2007
Conditions for the cosmological viability of f(r) dark energy models Luca Amendola INAF/Osservatorio Astronomico di Roma, Via Frascati 33 00040 Monte Porzio Catone (Roma), Italy Radouane Gannouji and David
More informationExamining the Viability of Phantom Dark Energy
Examining the Viability of Phantom Dark Energy Kevin J. Ludwick LaGrange College 11/12/16 Kevin J. Ludwick (LaGrange College) Examining the Viability of Phantom Dark Energy 11/12/16 1 / 28 Outline 1 Overview
More informationModified Gravity. Santiago E. Perez Bergliaffa. Department of Theoretical Physics Institute of Physics University of the State of Rio de Janeiro
Modified Gravity Santiago E. Perez Bergliaffa Department of Theoretical Physics Institute of Physics University of the State of Rio de Janeiro BSCG 14 Summary What is modified gravity (MG)? Relevance:
More informationCosmological Dynamics from Modified f(r) Gravity in Einstein Frame
Cosmological Dynamics from Modified f(r) Gravity in Einstein Frame Daris Samart 1 Fundamental Physics & Cosmology Research Unit The Tah Poe Academia Institute (TPTP), Department of Physics Naresuan University,
More informationToward a Parameterized Post Friedmann. Description of Cosmic Acceleration
Toward a Parameterized Post Friedmann Description of Cosmic Acceleration Wayne Hu NYU, November 2006 Cosmic Acceleration Cosmic acceleration, like the cosmological constant, can either be viewed as arising
More informationPoS(FFP14)170. Loop Quantum Effects on a Viscous Dark Energy Cosmological Model. N.Mebarki1. S.Benchick
Loop Quantum Effects on a Viscous Dark Energy Cosmological Model Laboratoire de Physique Mathematique et Subatomique, Mentouri University Route Ain El Bey, Constantine 25000, Algeria E-mail: nnmebarki@yahoo.fr
More informationarxiv: v1 [astro-ph] 16 Jun 2007
Cosmological Constraints on f(r) Acceleration Models Yong-Seon Song, Hiranya Peiris, and Wayne Hu Kavli Institute for Cosmological Physics, Department of Astronomy & Astrophysics, and Enrico Fermi Institute,
More informationHolographic Cosmological Constant and Dark Energy arxiv: v1 [hep-th] 16 Sep 2007
Holographic Cosmological Constant and Dark Energy arxiv:0709.2456v1 [hep-th] 16 Sep 2007 Chao-Jun Feng Institute of Theoretical Physics, Academia Sinica Beijing 100080, China fengcj@itp.ac.cn A general
More informationarxiv: v2 [astro-ph] 10 Nov 2008
Cosmological constraints from Hubble parameter on f(r) cosmologies arxiv:84.2878v2 [astro-ph] 1 Nov 28 F. C. Carvalho 1,2 E.M. Santos 3 J. S. Alcaniz 1,4 J. Santos 5 1 Observatório Nacional, 2921-4 Rio
More informationCanadian Journal of Physics. Anisotropic solution in phantom cosmology via Noether symmetry approach
Anisotropic solution in phantom cosmology via Noether symmetry approach Journal: Canadian Journal of Physics Manuscript ID cjp-2017-0765.r2 Manuscript Type: Article Date Submitted by the Author: 07-Dec-2017
More informationarxiv: v1 [gr-qc] 16 Aug 2011
Massless particle creation in a f(r) accelerating universe S. H. Pereira and J. C. Z. Aguilar Universidade Federal de Itajubá, Campus Itabira Rua São Paulo, 377 35900-373, Itabira, MG, Brazil arxiv:1108.3346v1
More informationTesting gravity on Large Scales
EPJ Web of Conferences 58, 02013 (2013) DOI: 10.1051/ epjconf/ 20135802013 C Owned by the authors, published by EDP Sciences, 2013 Testing gravity on Large Scales Alvise Raccanelli 1,2,a 1 Jet Propulsion
More informationVU lecture Introduction to Particle Physics. Thomas Gajdosik, FI & VU. Big Bang (model)
Big Bang (model) What can be seen / measured? basically only light _ (and a few particles: e ±, p, p, ν x ) in different wave lengths: microwave to γ-rays in different intensities (measured in magnitudes)
More informationQuintessence with induced gravity
REVISTA MEXICANA DE FÍSICA S 53 (4) 137 143 AGOSTO 2007 Quintessence with induced gravity J.L. Cervantes-Cota and J. Rosas Ávila Depto. de Física, Instituto Nacional de Investigaciones Nucleares, Apartado
More informationTowards a future singularity?
BA-TH/04-478 February 2004 gr-qc/0405083 arxiv:gr-qc/0405083v1 16 May 2004 Towards a future singularity? M. Gasperini Dipartimento di Fisica, Università di Bari, Via G. Amendola 173, 70126 Bari, Italy
More informationarxiv:gr-qc/ v1 6 Nov 2006
Different faces of the phantom K.A. Bronnikov, J.C. Fabris and S.V.B. Gonçalves Departamento de Física, Universidade Federal do Espírito Santo, Vitória, ES, Brazil arxiv:gr-qc/0611038v1 6 Nov 2006 1. Introduction
More informationThe function q(z) as a consistency check for cosmological parameters
arxiv:0904.4496v1 [gr-qc] 28 Apr 2009 The function q(z) as a consistency check for cosmological parameters Maria Luiza Bedran April 28, 2009 Abstract In the Friedmann cosmology the deceleration of the
More informationExamining the Viability of Phantom Dark Energy
Examining the Viability of Phantom Dark Energy Kevin J. Ludwick LaGrange College 12/20/15 (11:00-11:30) Kevin J. Ludwick (LaGrange College) Examining the Viability of Phantom Dark Energy 12/20/15 (11:00-11:30)
More informationarxiv:astro-ph/ v2 25 Oct 2004
The CMB Spectrum in Cardassian Models Tomi Koivisto 1,2, Hannu Kurki-Suonio 3 and Finn Ravndal 2 1 Helsinki Institute of Physics, FIN-00014 Helsinki, Finland 2 Department of Physics, University of Oslo,
More informationarxiv: v1 [hep-th] 3 Apr 2012
Impulsive gravitational waves of massless particles in extended theories of gravity Morteza Mohseni Physics Department, Payame Noor University, 9395-3697 Tehran, Iran (Dated: June 8, 08) arxiv:04.0744v
More informationMATHEMATICAL TRIPOS Part III PAPER 53 COSMOLOGY
MATHEMATICAL TRIPOS Part III Wednesday, 8 June, 2011 9:00 am to 12:00 pm PAPER 53 COSMOLOGY Attempt no more than THREE questions. There are FOUR questions in total. The questions carry equal weight. STATIONERY
More informationCosmological interaction of vacuum energy and dark matter
Author: Facultat de Física, Universitat de Barcelona, Diagonal 645, 828 Barcelona, Spain. Advisor: Joan Solà Peracaula Models which allow for an evolving cosmological constant are an alternative to the
More informationf(t) modified teleparallel gravity as an alternative for holographic and new agegraphic dark energy models
Research in Astron. Astrophys. 2013 Vol. 13 No. 7, 757 771 http://www.raa-journal.org http://www.iop.org/journals/raa Research in Astronomy and Astrophysics f() modified teleparallel gravity as an alternative
More informationA Framework for. Modified Gravity. Models of Cosmic Acceleration. Wayne Hu EFI, November 2008
A Framework for Modified Gravity Models of Cosmic Acceleration Wayne Hu EFI, November 2008 Candidates for Acceleration Cosmological constant (cold dark matter) model ΛCDM is the standard model of cosmology
More informationarxiv: v1 [gr-qc] 19 Jun 2010
Accelerating cosmology in F(T) gravity with scalar field K.K.Yerzhanov, Sh.R.Myrzakul, I.I.Kulnazarov, R.Myrzakulov Eurasian International Center for Theoretical Physics, Eurasian National University,
More informationAstroparticle physics the History of the Universe
Astroparticle physics the History of the Universe Manfred Jeitler and Wolfgang Waltenberger Institute of High Energy Physics, Vienna TU Vienna, CERN, Geneva Wintersemester 2016 / 2017 1 The History of
More informationCanadian Journal of Physics. FLRW Cosmology of Induced Dark Energy Model and Open Universe
Canadian Journal of Physics FLRW Cosmology of Induced Dark Energy Model and Open Universe Journal: Canadian Journal of Physics Manuscript ID cjp-2016-0827.r3 Manuscript Type: Article Date Submitted by
More informationarxiv: v3 [gr-qc] 8 Sep 2016
Cosmic Acceleration From Matter Curvature Coupling Raziyeh Zaregonbadi and Mehrdad Farhoudi Department of Physics, Shahid Beheshti University, G.C., Evin, Tehran 19839, Iran September 2, 2016 arxiv:1512.05604v3
More informationarxiv: v1 [gr-qc] 31 Jan 2014
The generalized second law of thermodynamics for the interacting in f(t) gravity Ramón Herrera Instituto de Física, Pontificia Universidad Católica de Valparaíso, Casilla 4059, Valparaíso, Chile. arxiv:1401.8283v1
More informationarxiv: v2 [gr-qc] 27 Aug 2012
Cosmological constraints for an Eddington-Born-Infeld field ariv:1205.1168v2 [gr-qc] 27 Aug 2012 Antonio De Felice, 1, 2 Burin Gumjudpai, 1, 2 and Sanjay Jhingan 3 1 ThEP s CRL, NEP, The Institute for
More informationWeek 2 Part 2. The Friedmann Models: What are the constituents of the Universe?
Week Part The Friedmann Models: What are the constituents of the Universe? We now need to look at the expansion of the Universe described by R(τ) and its derivatives, and their relation to curvature. For
More informationPlane Symmetric Solutions in f(r, T) Gravity
Commun. Theor. Phys. 5 (201) 301 307 Vol. 5, No. 3, March 1, 201 Plane Symmetric Solutions in f(r, T) Gravity M. Farasat Shamir Department of Sciences and Humanities, National University of Computer and
More informationarxiv: v1 [physics.gen-ph] 8 Aug 2018
Geometric interpretation of the dark energy from projected hyperconical universes arxiv:188.9793v1 [physics.gen-ph] 8 Aug 18 R. Monjo 1 1 Department of Algebra, Geometry and Topology, Faculty of Mathematics,
More informationarxiv: v2 [gr-qc] 19 Oct 2018
Observational constraints on the jerk parameter with the data of the Hubble parameter arxiv:85.85v [gr-qc] 9 Oct 8 Abdulla Al Mamon, and Kauharu Bamba, Department of Mathematics, Jadavpur University, Kolkata-7,
More informationConstraints on reconstructed dark energy model from SN Ia and BAO/CMB observations
Eur. Phys. J. C (2017) 77:29 DOI 10.1140/epjc/s10052-016-4590-y Regular Article - Theoretical Physics Constraints on reconstructed dark energy model from SN Ia and BAO/CMB observations Abdulla Al Mamon
More informationStability of Stellar Filaments in Modified Gravity Speaker: Dr. Zeeshan Yousaf Assistant Professor Department of Mathematics University of the Punjab
Stability of Stellar Filaments in Modified Gravity Speaker: Dr. Zeeshan Yousaf Assistant Professor Department of Mathematics University of the Punjab Lahore-Pakistan Hot Topics in Modern Cosmology, XIIth
More informationDark energy cosmology in F(T) gravity
Dark energy cosmology in F(T) gravity PLB 725, 368 (2013) [arxiv:1304.6191 [gr-qc]] KMI 2013 Dec. 12, 2013 Sakata-Hirata Hall Nagoya University Nagoya University Presenter : Kazuharu Bamba (KMI, Nagoya
More informationThe Cosmology of. f (R) Models. for Cosmic Acceleration. Wayne Hu STScI, May 2008
The Cosmology of f (R) Models for Cosmic Acceleration Wayne Hu STScI, May 2008 Why Study f(r)? Cosmic acceleration, like the cosmological constant, can either be viewed as arising from Missing, or dark
More informationarxiv:gr-qc/ v2 3 Feb 2006
Constraining f(r) gravity in the Palatini formalism arxiv:gr-qc/0512017v2 3 Feb 2006 Thomas P. Sotiriou SISSA-International School of Advanced Studies, via Beirut 2-4, 34014, Trieste, Italy INFN, Sezione
More informationAn analogy between four parametrizations of the dark energy equation of state onto Physical DE Models
An analogy between four parametrizations of the dark energy equation of state onto Physical DE Models Ehsan Sadri Physics Department, Azad University Central Tehran Branch, Tehran, Iran Abstract In order
More informationarxiv:hep-th/ v2 6 Oct 2005
, Modified Gauss-Bonnet theory gravitational alternative for dark energy arxiv:hep-th/589v 6 Oct 5 Shin ichi Nojiri, and Sergei D. Odintsov, Department of Applied Physics, National Defence Academy, Hhirimizu
More informationPAPER 73 PHYSICAL COSMOLOGY
MATHEMATICAL TRIPOS Part III Wednesday 4 June 2008 1.30 to 4.30 PAPER 73 PHYSICAL COSMOLOGY Attempt no more than THREE questions. There are FOUR questions in total. The questions carry equal weight. STATIONERY
More informationCosmological dynamics of viable f(r) theories of gravity
Cosmological dynamics of viable f(r) theories of gravity Sulona Kandhai 1 and Peter K. S. Dunsby 1, 1 Astrophysics, Cosmology and Gravity Centre (ACGC), Department of Mathematics and Applied Mathematics,
More informationGalileon Cosmology ASTR448 final project. Yin Li December 2012
Galileon Cosmology ASTR448 final project Yin Li December 2012 Outline Theory Why modified gravity? Ostrogradski, Horndeski and scalar-tensor gravity; Galileon gravity as generalized DGP; Galileon in Minkowski
More informationAspects of multimetric gravity
Aspects of multimetric gravity Manuel Hohmann Teoreetilise füüsika labor Füüsikainstituut Tartu Ülikool 4. september 2012 Manuel Hohmann (Tartu Ülikool) Multimetric gravity 4. september 2012 1 / 32 Outline
More informationMimetic dark matter. The mimetic DM is of gravitational origin. Consider a conformal transformation of the type:
Mimetic gravity Frederico Arroja FA, N. Bartolo, P. Karmakar and S. Matarrese, JCAP 1509 (2015) 051 [arxiv:1506.08575 [gr-qc]] and JCAP 1604 (2016) no.04, 042 [arxiv:1512.09374 [gr-qc]]; S. Ramazanov,
More informationPAPER 71 COSMOLOGY. Attempt THREE questions There are seven questions in total The questions carry equal weight
MATHEMATICAL TRIPOS Part III Friday 31 May 00 9 to 1 PAPER 71 COSMOLOGY Attempt THREE questions There are seven questions in total The questions carry equal weight You may make free use of the information
More information