Warm Higgs\u2013Starobinsky inflation

Daris Samart,Phongpichit Channuie,Patinya Ma-Adlerd

doi:10.1140/epjc/s10052-022-10073-x

Daris Samart, Phongpichit Channuie + Show 1 more

Open Access

https://doi.org/10.1140/epjc/s10052-022-10073-x

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Abstract

In this work, we investigate the Higgs–Starobinsky (HS) model in the context of warm inflation scenario. The dissipative parameter as a linear form of temperature of warm inflation is considered with strong and weak regimes. We study the HS model in the Einstein frame using the slow-roll inflation framework. The inflationary observables are computed and then compared with the Plank 2018 data. With the sizeable number of e-folds and proper choices of parameters, we discover that the predictions of warm HS model present in this work are in very good agreement with the latest Planck 2018 results. More importantly, the parameters of the HS model are also constrained by using the data in order to make warm HS inflation successful.

Highlights

The main idea of the HS model is that the Higgs field does couple to the graviton (Ricci scalar) at large coupling and this leads to the R2 emerging from the quantum correction between Higgs and graviton at least at one-loop level
Salient features of the HS are that there is no physics beyond standard model of particle physics and the higher curvature term R2 of the Starobinsky inflation is automatically generated by the quantum correction effect
We have demonstrated a class of warm inflation scenario using HS gravity with a linear temperature of the dissipative parameter

Summary

The HS action

The gravitational action of the HS model with non-minimal coupling to the Ricci scalar and the self-interacting Higgs field is given by SJ =. The conformal factor, 2, plays important role on transformation of the gravitational action from the Jordan frame to the Einstein frame. The scalaron field, φ, in the HS model is introduced via φ = Mp. Using the definition of the scalaron field, one can write the effective potential of the scalaron in the Einstein frame as 1 − e−. Using the definition of the scalaron field, one can write the effective potential of the scalaron in the Einstein frame as 1 − e− This is the standard Starobinsky scalaron potential in the Einstein frame and we will employ this potential in the analysis of the warm inflation scenario throughout this work

Cosmological equations in warm inflation scenario

64 N 5 8 55

Q2N πQ

Confrontation with the Planck 2018 data

Conclusion