Minimal-supersymmetric extended inflation field in Horava-Lifshitz gravity

TL;DR

This paper investigates inflation within Horava-Lifshitz gravity incorporating minimal supersymmetry, deriving modified Friedmann equations and analyzing scalar and tensor perturbations, with results consistent with recent observational constraints.

Contribution

It introduces a minimal-supersymmetric extension of inflation in Horava-Lifshitz gravity and derives the resulting modifications to inflationary perturbations and their observational implications.

Findings

Tensor-to-scalar ratio is very small, between 10^{-9} and 10^{-3}.

Results are largely independent of the gravity theory for dark energy EoS ω=-1/3.

The model's predictions align with recent BICEP2/Keck and Planck observations.

Abstract

We study the Friedmann inflation in general covariant Horava-Lifshitz (HL) gravity without the projectability conditions and with detailed and non-detailed balance conditions. Accordingly, we derive modifications in the Friedmann equations due to a single-scalar field potential describing minimal-supersymmetrically extended inflation. By implementing two time-independent equations of state (EoS) characterizing the cosmic background geometry filled up with dark energy, the dependence of the tensorial and scalar density fluctuations and their ratios on the inflation field are determined. The latter refer to the time evolution of the inflationary field relative to the Hubble parameter. Furthermore, the ratios of tensorial-to-spectral density fluctuations are calculated in dependence on the spectral index. For cold dark energy EoS $\omega=-1/3$, we find that the tensorial-to-spectral density fluctuations are not depending on the different theories of gravity and the results are very small relative to the recent BICEP2/Keck Array-Planck observations, $10^{-9} \lessapprox r \lessapprox 10^{-3}$. We have also calculated the tensorial and scalar perturbations of the primordial spectra.