Deformed Starobinsky model in gravity's rainbow

In the context of gravity's rainbow, we study the deformed Starobinsky model in which the deformations take the form $f(R)\sim R^{2(1-\alpha)}$, with $R$ the Ricci scalar and $\alpha$ a positive parameter. We show that the spectral index of curvature perturbation and the tensor-to-scalar ratio can be written in terms of $N,\,\lambda$ and $\alpha$, with $N$ being the number of {\it e}-foldings, $\lambda$ a rainbow parameter. We compare the predictions of our models with Planck data. With the sizeable number of {\it e}-foldings and proper choices of parameters, we discover that the predictions of the model are in excellent agreement with the Planck analysis. Interestingly, we obtain the upper limit and the lower limit of a rainbow parameter $\lambda$ and a positive constant $\alpha$, respectively.

known as the rainbow functions. It is worth noting that the rainbow functions are chosen in such a way that they produce, at a low-energy IR limit /M → 0, the standard energy-momentum relation and they are required to satisfyf ( ) → 1 andg( ) → 1 where M is the energy scale that quantum effects of gravity become important.
Notice that the gravity's rainbow is motivated by modification of usual dispersion relation in the UV limit and captures a modification of the geometry at that limit. Hence, the geometry of the space-time in gravity's rainbow depends on energy of the test particles. Therefore, each test particle of different energy will feel a different geometry of space-time. This displays a family of metrics, namely a rainbow metrics, parametrized by to describe the background of the space-time instead of a single metric. In gravitys rainbow, the modified metric can be expressed as with the energy dependence of the frame fieldẽ µ ( ) can be written in terms of the energy independence frame field e µ asẽ 0 ( ) = e 0 /f ( ) andẽ i ( ) = e i /g( ) where i, 1, 2, 3. In the cosmological viewpoint, the conventional FLRW metric for the homogeneous and isotropic universe is replaced by a rainbow metric of the form where a(t) is a scale factor. For convenience, we chooseg( ) = 1 and only focus on the spatially flat case. As suggested in Ref. [12], this formalism can be generalized to study semi-classical effects of relativistic particles on the background metric during a longtime process. For the very early universe, we consider the evolution of the probes energy with cosmic time, denoted as (t). Hence the rainbow functionsf ( ) depends on time implicitly through the energy of particles.
In recent years, gravity's rainbow has attracted a lot of attentions and became the subject of much interest in the literature. In the context of such gravity, the various physical properties of the black holes are investigated, see e.g. [14][15][16][17][18][19][20][21]. In addition, the effects of the rainbow functions have also been discussed in several other scenarios, see for instance [22][23][24]. Moreover, the gravity's rainbow was investigated in Gauss-Bonnet gravity [25], massive gravity [26] and f (R) gravity [27].
More specifically, the gravitys rainbow has also been used for analyzing the effects of rainbow functions on the Starobinsky model of f (R) gravity [9].
One of the intriguing features of the Starobinsky model [10] is that gravity itself is directly responsible for the inflationary period of the universe without resorting to the introduction of new ad hoc scalar fields. The authors of Ref. [11] studied quantum-induced marginal deformations of the Starobinsky gravitational action of the form R 2(1α) , with R the Ricci scalar and α a positive parameter smaller than one half. The model predicted sizable primordial tensor modes. In the present work, we consider the model proposed by Ref. [11] in the context of gravity's rainbow.
This paper is organized as follows: In section II, we revisit the formalism in f (R) theory [7,8] in the framework of gravity's rainbow [9]. We then focus on the deformed Starobinskys model [11] in which f (R) takes the form f (R) ∼ R 2(1−α) . We take a short recap of a cosmological linear perturbation in the context of the gravitys rainbow generated during inflation and calculate the spectral index of scalar perturbation and the tensor-to-scalar ratio of the model in section III. In section IV, we compare the predicted results with Planck data. We conclude our findings in the last section.

II. f (R) THEORIES WITH GRAVITY'S RAINBOW EFFECT
As is well known, the modification to general relativity are expected to be plausible in very early universe where possible corrections to Einstein's theory may in principle emerge at high curvature.
One of the simplest classes of such modifications is f (R) theories where the Einstein-Hilbert term in the action is replaced by a generic function of the Ricci scalar. We start with the traditionally 4-dimensional action in f (R) gravity [7,8].
where κ 2 = 8πG, g is the determinant of the metric g µν , and the matter field Lagrangian L M depends on g µν and matter fields Ψ M . We can derive the field equation by varying the action (3) with respect to g µν to obtain [7,8] where F (R) = ∂f (R)/∂R and the operator is defined by Traditionally, the energy-momentum tensor of the matter fields is given by T and the (i, j)-component of Eq.(4) reads It is worth noting that the above two equations are modified by the rainbow function and these equations can be transformed to the standard ones when settingf = 1. Let us next consider the deformed Starobinsky model in which f (R) takes the following form [11]: where 1/(6M 2 ) = 2hm 4α−2 pl and we assume that α is a real parameter with 2|α| < 1 and h is a dimensionless parameter. It is worth noting that the Starobinsky model is recovered when α = 0. Note that in the standard Starobinsky scenario the R 2 plays a key role in the very early universe instead of relativistic matter. In the scalar field framework, the Starobinsky theory can be equivalent to the system of one scalar field (an inflaton). It is reasonable if we assume here that the inflaton dominates the very early universe and hence in what follows we can neglect the contributions from matter and radiation, i.e. ρ M = 0 and P M = 0.
The combination of Eqs.(5), (6) and (7) give us the following system of differential equations: Note here that when setting α = 0 our results given in Eqs. (9) and (10) nicely convert to those present in Ref. [9]. In addition, when setting both α = 0 andf (t) = 1 our results here reduce to those obtained in the Starobinsky model. Usingf ≈ (H/M ) λ , we obtain Since we are only interested in an inflationary solution, it is natural to assume the slow-roll approximation, namely the terms containingḦ and higher power inḢ can be neglected in this particular regime. Therefore the Eq. (11) is reduced tȯ Setting only α = 0, we obtain the same result given in Ref. [9]. Moreover, setting both α and λ to vanish, the result converts to the standard Starobinsky model [10]. Despite the fact that one can numerically solve this equation for the Hubble parameter during inflation, we can find a simple analytical solution to this equation provided the second term on the RHS can be ignored since we are considering a small deviation from the Starobinsky model. Given this further approximation one obtains and where H i and a i are respectively the Hubble parameter and the scale factor at the onset of inflation (t = t i ). The slow-roll parameter 1 is defined by 1 ≡ −Ḣ/H 2 which in this case can be estimated to the first order of α as 1 H −2(λ+1)M 2λ+2 6(λ + 1) Note that this parameter is less than unity during inflation (H 2 M 2 ) and we find when setting . One can simply determine the end of inflation (t = t f ) by the The number of e-foldings from t i to t f is then given by Using the expressions (16) and (15) the parameter N is thus given by to the first order of α: .
Note that when λ = 0 = α the result is the same as that of the Starobinsky model.

III. COSMOLOGICAL PERTURBATION IN GRAVITY'S RAINBOW REVISITED
In this section, we will take a short recap of a cosmological linear perturbation in the context of the gravity's rainbow generated during inflation proposed by Ref. [9]. We here begin with a scalar perturbation (since scalar and tensor evolve separately at the linear level) via the following perturbed flat FRW metric taking into account the rainbow effect wheref (t) denotes the rainbow function. Notice that this perturbed metric has been written in the Newtonian gauge. Let us define a new variable A ≡ 3(HΦ +Ψ). With the metric (19) and Eq. (4), we obtain the following system of equations [9] − ∇ 2 Ψ a 2 +f 2 HA = − andȦ Note that the equations given above can be used to describe evolution of the cosmological scalar perturbations. In what follows, we will solve these equations within the inflationary framework.
We first study scalar perturbations generated during inflation and consider not to take into account and from the equation (20), we find Using the background equation (7), we find from Eq.(22) Substituting Eq. (23) and (24) into Eq.(25), we find in Fourier space that the curvature perturbation satisfies the following equation where k is a comoving wave number and Q s is defined by Introducing new variables z s = a √ Q s and u = z s R, Eq.(26) can be reduced and then can be expressed as where a prime denotes a derivative with respect to the new time coordinates η = (af ) −1 dt. In order to determine the spectrum of curvature perturbations we define slow-roll parameters as where E ≡ 3Ḟ 2 /2κ 2 . As a result, Q s can be recast as Here parameters i are assumed to be nearly constant during the inflation andf (H/M ) λ . These allow us to calculate η as η with Therefore we find the solution of Eq.(28) written in terms of a linear combination of Hankel where c 1 , c 2 are integration constants and H (1) ν R (k|η|), H ν R (k|η|) are the Hankel functions of the first kind and the second kind respectively. In the asymptotic past kη → −∞, we find from Eq.(33) u → e −ikη / √ 2k. This implies c 1 = 1 and c 2 = 0 giving the following solutions By defining the power spectrum of curvature perturbations and using Eq.(34) and u = z s R, we obtain where we have used H (1) ν R (k|η|) → −(i/π)Γ(ν R )(k|η|/2) −ν R for k|η| → 0. Since R is frozen after the Hubble radius crossing, P R should be evaluated at k = aH. Now we define the spectral index n R as The spectral index can be written in terms of the slow-roll parameters as where during the inflationary epoch, we have assumed that | i | 1. Notice that the spectrum is nearly scale-invariant when | i | are much smaller than unity, i.e. n R 1. Subsequently, the power spectrum of curvature perturbation takes the form Note that we obtain the standard result when setting λ = 0 [8]. We next consider the tensor perturbation. In general h ij can be generally written as where e + ij and e × ij are the polarization tensors corresponding to the two polarization states of h ij . Let k be in the direction along the z-axis, then the non-vanishing components of polarization tensors are e + xx = −e + yy = 1 and e × xy = e × yx = 1. Without taking into account the scalar and vector perturbation, the perturbed FLRW metric can be written as Using Eq.(4), we can show that the Fourier components h χ satisfy the following equation where χ denotes polarizations + and ×. Following a similar procedure to the case of curvature perturbation, let us introduce the new variables z t = a √ F and u χ = z t h χ / √ 2κ 2 . Therefore Eq.
(42) can be written as Notice that for a massless scalar field u χ has dimension of mass. By choosing˙ i = 0, we obtain where Similarly the solution to Eq.(43) can be also expressed in terms of a linear combination of Hankel functions. Taking into account polarization states, the power spectrum of tensor perturbations P T after the Hubble radius crossing reads where we have usedf (H/M ) λ . Therefore ν t can be estimated by assuming that the slow-roll parameters are very small during inflation as In addition, the spectral index of tensor perturbations is determined via The power spectrum P T can also be rewritten as The tensor-to-scalar ratio r can be obtained as Substituting Q s from Eq.(30), we therefore obtain Let us next examine relations among the slow-roll parameters. Having assumed that | i | 1 during the inflation and matter field, Eq. (7) gives us Compared with the Starobinsky model, we have similar form of f (R) = R + R 2(1−α) 6M 2 . Here inflation occurred in the limit R M 2 and |Ḣ| H 2 . We can approximate F (R) (12H 2f 2 ) 1−2α (1 − α)/3M 2 . By assuming that | i | 1 during the inflation, this leads to (54) Since n R − 1 −2(λ + 2) 1 + 2 3 − 2 4 and r = 48 2 3 , one obtains the spectral index of scalar perturbations and the tensor-to-scalar ratio rewritten in terms of 1 as follows: n R − 1 −4(1 + 2α(λ + 1)) 1 and r 48(λ + 1) 2 2 1 .
Let t k be the time at the Hubble radius crossing (k = aH). From Eq.(13), as long as the condition The number of e-fold from t = t k to the end of the inflation can be estimated as N k 1/2 1 (t k ). We also find from Eq.(54) to the leading order of α that According to the relation (18), both n R and r can be rewritten in terms of the number of e-foldings as and Notice that the spectral index of scalar perturbations n R does depend on both α and the rainbow parameter, λ.

IV. CONTACT WITH OBSERVATION
In this section, we compare our predicted results with Planck 2015 data. We find from with Planck'15 results for TT, TE, EE, +lowP and assuming ΛCDM+r [5].
We also consider the situation in which the values of N are arbitrary but keep λ and α fixed.
From Fig.(2), we observe that in order for the predictions to be satisfied the Planck data at one sigma level a value of λ can not be greater than 4.0 and 3.6 with α = 0.01 and 0.0001, respectively. The 2018 recent release of the Planck cosmic microwave background (CMB) anisotropy measurements [6] determines the spectral index of scalar perturbations to be n s = 0.9649 ± 0.0042 at 68% CL and the 95% CL upper limit on the tensor-to-scalar ratio is further tightened by combining with the BICEP2/Keck Array BK14 data to obtain r 0.002 < 0.064. We use these updated parameters to constrain our model parameters. Let us consider Eq.(58) and then we obtain the upper limit of a parameter λ = λ * as Interestingly, this upper limit can be used to constrain the value of α. Substituting the value of λ * into Eq.(57), we obtain the lower limit of α = α * as α * > 2.65 × 10 −2 (1.33 × 10 −2 (5.48N − 75) + 1.00) .
and α * > 6.06×10 −3 for N = 60. In addition, we compare the theoretical predictions in the (r−n s ) plane for different values of λ and N but keep α fixed with Planck'15 results displayed in Fig.(3).
We find that using α = 0.006 and λ = 3.38 the predictions in the (r − n s ) plane lie in the one sigma confidence level only when N = [60, 70]. Using parameters of the base ΛCDM cosmology reported by Planck 2018 [5] for P R at the scale k = 0.05 Mpc −1 , we find from Eq.(66) that the massM is constrained to bẽ Using N = 60, λ = 3.38 we discover at the scale ofM that h ≈ 1.13 × 10 5 . However, h is in general scale-dependent. The explicit computations via heat kernel methods [13] shows that a logarithmic form of h can be induced by leading order quantum fluctuations. The RG improved treatment of h can be found in Ref. [11].

V. CONCLUSION
In this work, we studied the deformed Starobinsky model in which the deformations take the form R 2(1−α) , with R the Ricci scalar and α a positive parameter [11]. We started by revisiting the formalism in f (R) theory [7,8] in the framework of gravity's rainbow [9]. We took a short recap of a cosmological linear perturbation in the context of the gravitys rainbow generated during inflation and calculated the spectral index of scalar perturbation and the tensor-to-scalar ratio predicted by the model. We Regarding our present work, the study the cosmological dynamics of isotropic and anisotropic universe in f (R) gravity, see e.g. [8,31,32] and references therein, via the dynamical system technique can be further studied. Interestingly, the swampland criteria in the deformed Starobinsky model can be worth investigating by following the work done by Ref. [28]. The reheating process in the present work is worth investigating [29,30].