Abstract
In this paper, we investigate non-Ricci, non-compact Friedmann–Robertson–Walker type Kaluza–Klein cosmology in the presence of pressureless matter and modified holographic Ricci dark energy in the frame work of Brans and Dicke (Phys Rev 124:965, 1961) scalar–tensor theory of gravitation. We solve the field equations of this theory using a hybrid expansion law for the five dimensional scale factor. We have also used a power law and a form of logarithmic function of the scale factor for the Brans–Dicke scalar field. Consequently, we obtain two interesting cosmological models of the Kaluza–Klein universe. We have evaluated the cosmological parameters, namely, the equation of state parameter, the deceleration parameter, and the density parameters. To check the stability of our models we use the squared speed of sound. Some well-known cosmological (omega _{de}–omega ^{prime }_{de} and statefinder) planes are constructed for our models. We have also analyzed the physical behavior of these parameters through graphical representation. It is observed that the FRW type Kaluza–Klein dark energy models presented are compatible with the present day cosmological observations.
Highlights
The discovery of accelerated expansion of the universe is one of the biggest achievement of the twentieth century [1,2]
The scalar–tensor theory of gravitation proposed by Brans and Dicke plays a significant role in the discussion of dark energy cosmology
In this paper, by solving the Brans and Dicke (BD) field equations we have obtained Kaluza–Klein FRW cosmological models filled with baryonic matter and modified holographic Ricci DE (MHRDE)
Summary
The discovery of accelerated expansion of the universe is one of the biggest achievement of the twentieth century [1,2]. Cohen et al [16] recommended that the vacuum energy density is proportional to the Hubble scale i.e., lH ≈ H −1 In this model, they successfully explained both the fine-tuning and the coincidence problems, but it is unable to expound the recent cosmic accelerated expansion. Ricci DE model in which the energy density of DE is a function of the Hubble parameter H and its first order derivative with respect to cosmic time (i.e., H ). C (2018) 78:619 contains the second order derivative of Hubble’s parameter with respect to time (i.e., H ) and is known as modified holographic Ricci DE (MHRDE) This DE model explains the well-known age problem of the old objects.
Sign-in/Register to view highlights & summary Sign-in/Register to access full text options 
Free) 
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a call
