# Cosmological decay of Higgs-like scalars into a fermion channel

## TL;DR

This paper investigates the decay of Higgs-like scalars into fermions in a cosmological setting, deriving non-perturbative survival probabilities and highlighting deviations from Minkowski decay laws due to cosmological effects.

## Contribution

It introduces a non-perturbative method to compute decay probabilities of scalar particles in expanding universes, revealing memory effects and providing bounds on particle survival based on cosmological parameters.

## Key findings

- Derived explicit survival probability formulas accounting for cosmological redshift.
- Identified that phenomenological Minkowski decay laws underestimate particle lifetimes.
- Established an upper bound on survival probability as a function of redshift.

## Abstract

We study the decay of a Higgs-like scalar Yukawa coupled to massless fermions in post-inflationary cosmology, combining a non-perturbative method with an adiabatic expansion. The renormalized survival probability $\mathcal{P}_\Phi(t)$ of a (quasi) particle ``born'' at time $t_b$ and decaying at rest in the comoving frame, $\mathcal{P}_\Phi(t) = \Big[\frac{t}{t_b}\Big]^{-\frac{Y^2}{8\pi^2}}~ e^{ \frac{Y^2}{4\pi^2}\,\big(t/t_b\big)^{1/4} } \,e^{-\Gamma_0\,(t-t_b)}~ \mathcal{P}_\Phi(t_b) $, with $\Gamma_0$ the decay rate at rest in Minkowski space-time. For an ultrarelativistic particle we find $\mathcal{P}_\Phi(t) = e^{-\frac{2}{3}\Gamma_0\,t_{nr}\,(t/t_{nr})^{3/2}}~ \mathcal{P}_\Phi(t_b)$ before it becomes non-relativistic at a time $t_{nr}$ as a consequence of the cosmological redshift. For $t\gg t_{nr}$ we find $\mathcal{P}_\Phi(t) = \Big[\frac{t}{t_{nr}}\Big]^{-\frac{Y^2}{8\pi^2}}~ e^{ \frac{Y^2}{4\pi^2}\,\big(t/t_{nr}\big)^{1/4} }~\Big[\frac{t}{t_{nr}}\Big]^{\Gamma_0 t_{nr}/2} \,e^{-\Gamma_0\,(t-t_{nr})}~ \mathcal{P}_\Phi(t_{nr})$. The extra power is a consequence of the memory on the past history of the decay process. We compare these results to an S-matrix inspired phenomenological Minkowski-like decay law modified by an instantaneous Lorentz factor to account for cosmological redshift. Such phenomenological description \emph{under estimates the lifetime of the particle}. For very long lived, very weakly coupled particles, we obtain an \emph{upper bound} for the survival probability as a function of redshift $z$ valid throughout the expansion history $\mathcal{P}_\Phi(z) \gtrsim e^{-\frac{\Gamma_0}{H_0}\,\Upsilon(z,z_b)}\,\mathcal{P}_\Phi(z_b)$, where $\Upsilon(z,z_b)$ only depends on cosmological parameters and $t_{nr}$.