Abstract
This paper is devoted to investigate the interacting generalized ghost pilgrim dark energy model in the background of anisotropic universe in general relativity. We analyze the two parameters i.e., hubble parameter and equation of state parameter to explore the cosmological evolution of the Bianchi type universe. We study scalar field dark energy models i.e., quintessence, dilaton, K-essence and tachyon to check the consistency of the current universe with their scalar field and corresponding potentials. Further, we check the compatibility of fractional density of matter and dark energy with recent observations of Plank along with their graphical analysis. It is remarkable to conclude that that both fractional densities admits consistency with Plank data 2018 in all cases of Bainchi type universe.
Highlights
Recent observational data reveals that we are surviving in the accelerated phase of universe [1,2,3]
Page 3 of 20 149 where dot is known as derivative of t and Q is the interaction term between the generalized ghost pilgrim DE (GGPDE) and cold DM (CDM)
The sign interaction term gives the transformation of energies. It gives negative sign if CDM tends to decompose into dark energy (DE) and gives positive sign when DE decays into CDM
Summary
Recent observational data reveals that we are surviving in the accelerated phase of universe [1,2,3]. The acceptable universe model is known as Big Bang. About 13–14 billion years ago, the universe was scattered only to a few millimeters across It was very hot and dense, but it expanded regularly and become vast and cool, into cosmos that we know today. The cosmological constant has been considered as the simplest DE candidate where the cosmological constant model ( C D M) is compatible with current days observations. This model has a problem of cosmological issue like “fine tuning”. The field which naturally found in particle physics like string theory [19] is known as scalar field are utilized as a possible candidate of DE. Vacuum energy is ghost field can be utilized to describe the time varying cosmological constant in a space time [20]
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