Scalar Field Condensate Baryogenesis Model in Different Inflationary Scenarios

TL;DR

This paper evaluates the Scalar Field Condensate baryogenesis model across various inflationary scenarios, identifying conditions under which it produces the observed baryon asymmetry and highlighting models requiring dilution mechanisms.

Contribution

It provides a comprehensive analysis of the SCF baryogenesis model's effectiveness in different inflationary contexts, including over 70 parameter sets and multiple inflation scenarios.

Findings

SCF baryogenesis exceeds observed baryon asymmetry in some models, requiring dilution.

Successful baryon asymmetry generation occurs in Modified Starobinsky, low-reheat chaotic, SUGRA, and Quintessential inflation.

Many models produce too much baryon asymmetry, indicating the need for additional dilution mechanisms.

Abstract

We calculate the baryon asymmetry value generated in the Scalar Field Condensate (SCF) baryogenesis model obtained in several inflationary scenarios and different reheating models. We provide analysis of the baryon asymmetry value obtained for more than 70 sets of parameters of the SCF model and the following inflationary scenarios, namely: new inflation, chaotic inflation, Starobinsky inflation, MSSM inflation, quintessential inflation. We considered both cases of efficient thermalization after inflation and also delayed thermalization. We have found that SFC baryogenesis model produces baryon asymmetry by orders of magnitude bigger than the observed one for the following inflationary models: new inflation, new inflation model by Shafi and Vilenkin, MSSM inflation, chaotic inflation with high reheating temperature and the simplest Shafi-Vilenkin chaotic inflationary model. For these models strong diluting mechanisms are needed to reduce the resultant baryon excess at low energies to its observational value today. We have found that a successful generation of the observed baryon asymmetry is possible by SCF baryogenesis model in Modified Starobinsky inflation, chaotic inflation with low reheating temperature, chaotic inflation in SUGRA and Quintessential inflation.