Revisiting primordial black holes formation from preheating instabilities: the case of Starobinsky inflation

TL;DR

This paper investigates primordial black hole formation during the preheating phase of Starobinsky inflation, highlighting the role of sub-horizon modes and their evolution into density perturbations capable of collapsing into PBHs.

Contribution

It introduces a detailed analysis of sub-horizon mode evolution during preheating in Starobinsky inflation, expanding the understanding of PBH formation mechanisms without fine-tuning.

Findings

Identification of sub-horizon modes contributing to PBH formation

Comparison of mass fraction calculations using Press-Schechter and Khlopov-Polnarev formalisms

Implications for PBH contribution to dark matter

Abstract

In recent years, the formation of primordial black holes (PBH) in the early universe inflationary cosmology has garnered significant attention. One plausible scenario for primordial black hole (PBH) formation arises during the preheating stage following inflation. Notably, this scenario does not necessitate any ad-hoc fine-tuning of the scalar field potential. This paper focuses on the growth of primordial density perturbation and the consequent possibility of PBH formation in the preheating stage of the Starobinsky model for inflation. The typical mechanism for PBH formation during preheating is based on the collapse of primordial fluctuations that become super-horizon during inflation (type I) and re-enter the particle horizon in the different phases of cosmic expansion. In this work, we show that there exists a certain range of modes that remain in the sub-horizon (not exited) during inflation (type II modes) but evolve identically to type I modes if they fall into the instability band, leading to large density perturbation above the threshold and can potentially also contribute to the PBH formation. We detail the conditions determining the possible collapse of type I and/or type II modes whose wavelengths are larger than the Jeans length we derive from the effective sound speed of scalar field fluctuations. Since the preheating stage is an 'inflaton' (approximately) matter-dominated phase, we follow the framework of the critical collapse of fluctuations and compute the mass fraction using the well-known Press-Schechter and the Khlopov-Polnarev formalisms, and compare the two. Finally, we comment on the implications of our study for the investigations concerned with primordial accretion and consequent PBH contribution to the dark matter.