Abstract
In this paper, we explore the evolution of baryon asymmetry as well as the hypermagnetic field in the early universe with an assumption that the flavon of the Froggatt-Nielsen carries an asymmetry. Through the decay of the flavon to Standard Model fermions, this asymmetry is transferred to fermions, where the right-handed electron keeps its asymmetry while its Yukawa interaction is out of thermal equilibrium. Through the existence of the flavon, we can ensure that the freezing-in temperature of the right-handed electron is closer to the electroweak phase transition than the Standard cosmology scenario. With this trick, the asymmetry in the right-handed electron is saved for a longer time. Moreover, the injection of the asymmetry to the right-handed electron is gradual, which helps the preservation of the asymmetry in the right-handed sector significantly. Due to the intimate relationship between fermion number violation and the helicity of the hypermagnetic field, some of the asymmetry is used to amplify the hypermagnetic field which itself helps to preserve the remnant asymmetry through keeping the Yukawa processes out of thermal equilibrium. We find the sweet region of the parameter space that can produce the right asymmetry in the baryons while generating a large hypermagnetic field by the time of the electroweak phase transition.
Highlights
One of the most intriguing questions of particle physics is the observation of matter-antimatter asymmetry
We explore the evolution of baryon asymmetry as well as the hypermagnetic field in the early universe with an assumption that the flavon of the Froggatt-Nielsen carries an asymmetry
Through the decay of the flavon to Standard Model fermions, this asymmetry is transferred to fermions, where the right-handed electron keeps its asymmetry while its Yukawa interaction is out of thermal equilibrium
Summary
One of the most intriguing questions of particle physics is the observation of matter-antimatter asymmetry. We are interested in scenarios where the initial seed of the hypermagnetic field amplitude (HMFA) is small, and through the existence of baryonic asymmetry, we get a large value of HMFA (∼1020 G) by the time of EWPT. The difference between the freeze-in temperature of righthanded electron, TR ≃ 105 GeV, and the temperature at which EWPT occurs (TEW) is large enough that the weak sphalerons have enough time to wash out the asymmetry. To avoid this problem, one solution is to change the cosmological evolution.
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