Non-canonical scalar field in low anisotropy universe with intermediate inflation

TL;DR

This paper investigates a non-canonical scalar field in an anisotropic universe with intermediate inflation, analyzing its compatibility with observational data and comparing it to canonical inflation models.

Contribution

It introduces a non-canonical scalar field model in anisotropic inflation and assesses its observational viability, highlighting improved compatibility with Planck data.

Findings

The model yields a steep potential suitable for inflation.

It shows good consistency with Planck 2015 observational data.

Comparison with canonical inflation demonstrates advantages in anisotropic settings.

Abstract

The behaviour of a non-canonical scalar field within an anisotropic Bianchi type I, spatially homogeneous, Universe in the framework of the intermediate inflation will be studied. It will be examined on the condition that both the anisotropy and non-canonical sources come together and is there any improvement in compatibility with the observational data originated from plank $2015$?. Based on this investigation it can be observed that automatically a steep potential which can manage inflation in a better way will be obtained. Additionally, as a common procedure for an inflationary study, we shall try to calculate the related inflationary observables such as the amplitude of the scalar perturbations, scalar and tensor spectral indices, tensor-to-scalar ratio, the running spectral index, and the number of e-folds. As an exciting part of our results, we will find that our model has a good consistency compared to data risen by CMB and different Planck results. To justify our claims, the well known canonical inflationary scenario in an anisotropic Bianchi type I Universe also will be evaluated.