Universe Decay, Inflation and the Large Eigenvalue of the Cosmological Constant Seesaw

TL;DR

This paper explores how the large eigenvalue of the cosmological constant seesaw mechanism can lead to a period of inflation followed by universe decay, connecting quantum tunneling, mixing, and various cosmological models.

Contribution

It highlights the physical implications of the large eigenvalue in the cosmological constant seesaw, particularly its role in inflation and universe decay mechanisms.

Findings

Large eigenvalue can induce inflationary phase

Quantum tunneling and mixing parameters govern decay

Connections to string theory and hierarchy problem

Abstract

We discuss implications of the large eigenvalue of the cosmological constant seesaw mechanism extending hep-th/0602112 and hep-th/0604108. While the previous papers focused on the small eigenvalue as a cosmological constant associated with the accelerating Universe, here we draw attention to the physical implications of the large eigenvalue. In particular we find that the large eigenvalue can give rise to a period of inflation terminated by Universe decay. The mechanism involves quantum tunneling and mixing and introduces parameters $\Gamma$, the decay constant, and $\theta$, the mixing angle. We discuss the cosmological constant seesaw mechanism in the context of various models of current interest including chain inflation, inflatonless inflation, string theory, Universe entanglement and different approaches to the hierarchy problem.