Can structure formation distinguish<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mi>Λ</mml:mi><mml:mi>CDM</mml:mi></mml:math>from nonminimal<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mi>f</mml:mi><mml:mo stretchy="false">(</mml:mo><mml:mi>R</mml:mi><mml:mo stretchy="false">)</mml:mo></mml:math>gravity?

Thakur, Shruti; Sen, Anjan A.

doi:10.1103/physrevd.88.044043

Cited by 50 publications

(7 citation statements)

References 69 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…First, we look at the perturbations which are deep inside the Hubble horizon, i.e., k a ≫ H. To get the equation governing the perturbation δ deep inside the Hubble horizon, we also apply the following approximations [40][41][42]:…”

Section: A Subhorizon Regimementioning

confidence: 99%

Large scale structure formation in Eddington-inspired Born-Infeld gravity

2014

View full text Add to dashboard Cite

We study the large scale structure formation in Eddington-inspired Born-Infeld (EiBI) gravity. It is found that the linear growth of scalar perturbations in EiBI gravity deviates from that in general relativity for modes with large wave numbers (k), but the deviation is largely suppressed with the expansion of the Universe. We investigate the integrated Sachs-Wolfe effect in EiBI gravity, and find that its effect on the angular power spectrum of the anisotropy of the cosmic microwave background (CMB) is almost the same as that in the Lambda-cold dark matter (ΛCDM) model. We further calculate the linear matter power spectrum in EiBI gravity and compare it with that in the ΛCDM model. Deviation is found on small scales (k 0.1h Mpc −1 ), which can be tested in the future by observations from galaxy surveys.

show abstract

Section: A Subhorizon Regimementioning

confidence: 99%

Large scale structure formation in Eddington-inspired Born-Infeld gravity

2014

View full text Add to dashboard Cite

show abstract

“…Cognola et al [40] studied modified f (R) gravities and described inflation and accelerated expansion. Thakur and Sen [41] discussed a non-minimally coupled form of function f (R). Mukherjee and Banerjee [42] studied FRW model with f (R) proportional to (λ + R) n and exp(αR).…”

Section: Introductionmentioning

confidence: 99%

Physical parameters for stable f(R) models

Samanta¹,

Godani

2019

Indian J Phys

View full text Add to dashboard Cite

Nojiri & Odintsov [1] and Hu & Sawicki [2] have studied non-linear functions in modified gravity that explain the cosmic acceleration without cosmological constant, fulfil the conditions of local gravity & stability and pass the solar system tests. In this paper, FRW model, a best fitted and fruitful mathematical model of the physical universe [3-6] is studied in the context of these non-linear functions. The cosmological implications such as Hubble parameter, deceleration parameter, jerk parameter, matter density and the effective equation of state parameter of the universe are plotted with respect to redshift. Subsequently, the age of the universe is predicted in f (R) gravity. All are found to represent the features of present phase of the universe.

show abstract

“…There have been recent attempts to find some form of f (R) which would yield accelerated expansion in two phases, one in an early epoch and the other in the late stage of evolution. Cognola et al (Cognola et al 2009) and Elizalde et at (Elizalde et al 2011) made such attempts with an f (R) which is an exponential function of R. Nojiri and Odintsov (Nojiri and Odintsov 2003b) made an attempt to unify the two phases of accelerated expansion in the realm of a single f (R) gravity model by combining positive and negative powers of R. Possible impacts of the existence of nonlinear terms involving R in the action on the structure formation has been discussed by Thakur and Sen(Thakur and Sen 2013).…”

Section: Introductionmentioning

confidence: 99%