Primordial black holes in non-canonical scalar field inflation driven by quartic potential in the presence of bump

TL;DR

This paper explores how a non-canonical inflation model with a quartic potential and a bump can produce primordial black holes and detectable gravitational waves, highlighting the effects of model parameters and fine-tuning.

Contribution

It introduces a novel non-canonical inflationary framework with a bump in the potential, demonstrating its capability to generate PBHs and associated GWs with specific parameter tuning.

Findings

A viable inflationary era driven by quartic potential in non-canonical framework.

Bump feature causes inflaton slowdown, amplifying small-scale scalar perturbations.

Predicted gravitational wave spectra are within reach of current detectors.

Abstract

Here, generation of Primordial Black Holes (PBHs) from quartic potential in the presence of a tiny bump in non-canonical inflationary model has been inquired. It is demonstrated that, a viable inflationary era can be driven through the quartic potential in non-canonical framework with a power-law Lagrangian density. Furthermore, setting a suitable function of inflaton field as a correction term (like a bump) to the quartic potential, causes the inflaton to slow down for a while. In such a short time span, the amplitude of the scalar perturbations power spectrum on small scales grows up sufficiently versus CMB scales. In addition to the bump feature, the enhancing effect of the $\alpha$ parameter of the Lagrangian on the amplitude of the scalar power spectrum has been shown. Fine tuning of three parameter Cases of the model results in generating of three Cases of PBHs. In addition, we investigate the secondary Gravitational Waves (GWs) produced during generation of PBHs and show that their contemporary density parameter spectra $(\Omega_{\rm GW_0})$ can be tracked down by GWs detectors.