Effects of Multi-Field Phantom Inflation in Big Rip

TL;DR

This paper explores multi-field phantom inflation models with power-law scale factors, analyzing their parameters and comparing predictions with current cosmological observations, suggesting consistency with observed data and implications for dark energy behavior at the Big Rip.

Contribution

It introduces a multi-field phantom inflation model with a power-law scale factor and evaluates its parameters against observational data, providing new insights into the universe's behavior near the Big Rip.

Findings

Model parameters are consistent with CMB, BAO, and Hubble data.

Dark energy EOS parameter remains finite at the Big Rip.

Universe is in a phantom inflationary phase before the Big Rip.

Abstract

In this paper we study the behavior of the multi-field in phantom inflation, when massive scalar fields work collectively, in which the scale factor is a power law. We evaluate its parameter values by applying certain constraints on our model parameters, and we investigate that before the Big Rip singularity occurs the universe is in phantom inflationary phase. Furthermore, we calculate these values for this period then compare with current observations of CMB, BAO and observational Hubble data. We find that results may be consistent with observations. This implies that in the dark-energy equation of state (EOS) parameter $\omega_{DE}$ at the Big Rip remains finite, with the divergence of pressure and dark energy density.