IOP : Freeze-in from Preheating

Garcia, Marcos A.G.; Olive, Keith A.; Verner, Sarunas; Kaneta, Kunio; Mambrini, Yann

doi:10.1088/1475-7516/2022/03/016

Article
Report number	arXiv:2109.13280 ; UMN-TH-4101/21 ; FTPI-MINN-21/19 ; CERN-TH-2021-121
Title	Freeze-in from Preheating
Author(s)	Garcia, Marcos A.G. (Madrid, IFT ; Madrid, Autonoma U. ; INFN, Padua ; U. Padua (main)) ; Kaneta, Kunio (Tokyo Woman's Christian U.) ; Mambrini, Yann (IJCLab, Orsay ; CERN) ; Olive, Keith A. (Minnesota U., Theor. Phys. Inst.) ; Verner, Sarunas (Minnesota U., Theor. Phys. Inst.)
Publication	2022-03-08
Imprint	2021-09-27
Number of pages	39
Note	39 pages, 13 figures
In:	JCAP 2203 (2022) 016
DOI	10.1088/1475-7516/2022/03/016
Subject category	astro-ph.CO ; Astrophysics and Astronomy ; hep-ph ; Particle Physics - Phenomenology
Abstract	We consider the production of dark matter during the process of reheating after inflation. The relic density of dark matter from freeze-in depends on both the energy density and energy distribution of the inflaton scattering or decay products composing the radiation bath. We compare the perturbative and non-perturbative calculations of the energy density in radiation. We also consider the (likely) possibility that the final state scalar products are unstable. Assuming either thermal or non-thermal energy distribution functions, we compare the resulting relic density based on these different approaches. We show that the present-day cold dark matter density can be obtained through freeze-in from preheating for a large range of dark matter masses.
Copyright/License	preprint: (License: arXiv nonexclusive-distrib 1.0) publication: © 2022-2025 IOP Publishing Ltd and Sissa Medialab

$\it Evolution of the energy densities during reheating of the inflaton (solid red) and radiation produced by inflaton decays to fermions (dashed, orange) and annihilations to bosons (blue). In the latter, we show separately the case when the effective masses of the decay products are ignored (dotted) and included (dashed-dotted). The total energy density of the decay/annihilation products is also shown (black solid). We set $y = \sigma = 10^{-7}$, $\rho_{\rm end}=2\times 10^{-11}\, M_P^4$ and $\lambda=2.05\times 10^{-11}$, assuming T-attractor inflation boundary conditions. The arrow points toward the region where $\mathcal{R}>1$, indicating the region where non-perturbative effects are expected to affect the evolution of $\rho_R$. The `moment' of reheating is defined when $\rho_\phi = \rho_R$, which occurs at $a/a_{\rm end} \simeq 2.4 \times 10^{10}$.$ $\it Instantaneous energy density in relativistic bosons during reheating sourced via the coupling $\frac{\sigma}{2}\phi^2\chi^2$ for values of $\sigma/\lambda = 10, \, 100$, and $1000$. We show the energy density $\rho_R=\rho_{\chi}$ determined perturbatively when the $\phi$-induced mass of $\chi$ is ignored (dotted blue), accounting for this induced mass (dashed-dotted blue), and computed non-perturbatively (solid black) as a function of the scale factor. We also show the energy density $\rho_R=\rho_{\chi}+\rho_f$ when $\chi$ decays rapidly assuming the coupling $y_\chi = 1$ (dashed purple).$ $\it Instantaneous energy density in relativistic bosons during reheating sourced via the coupling $\frac{\sigma}{2}\phi^2\chi^2$ for values of $\sigma/\lambda = 10, \, 100$, and $1000$. We show the energy density $\rho_R=\rho_{\chi}$ determined perturbatively when the $\phi$-induced mass of $\chi$ is ignored (dotted blue), accounting for this induced mass (dashed-dotted blue), and computed non-perturbatively (solid black) as a function of the scale factor. We also show the energy density $\rho_R=\rho_{\chi}+\rho_f$ when $\chi$ decays rapidly assuming the coupling $y_\chi = 1$ (dashed purple).$ Show more plots

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