Abstract
We consider various models realizing baryogenesis during the electroweak phase transition (EWBG). Our focus is their possible detection in future collider experiments and possible observation of gravitational waves emitted during the phase transition. We also discuss the possibility of a non-standard cosmological history which can facilitate EWBG. We show how acceptable parameter space can be extended due to such a modification and conclude that next generation precision experiments such as the ILC will be able to confirm or falsify many models realizing EWBG. We also show that, in general, collider searches are a more powerful probe than gravitational wave searches. However, observation of a deviation from the SM without any hints of gravitational waves can point to models with modified cosmological history that generically enable EWBG with weaker phase transition and thus, smaller GW signals.
Highlights
The main point we wish to make comes from the fact that early cosmological evolution of the universe is rather poorly constrained by experiments
We consider various models realizing baryogenesis during the electroweak phase transition (EWBG). Our focus is their possible detection in future collider experiments and possible observation of gravitational waves emitted during the phase transition
Observation of a deviation from the SM without any hints of gravitational waves can point to models with modified cosmological history that generically enable EWBG with weaker phase transition and smaller GW signals
Summary
Our modification is the addition of a new scalar field S with the potential. The field-dependent masses are identical to the Standard Model, and the new scalar mass takes the form m2S (φ). The coefficients read n{h,χ,W,Z,t} = {1, 3, 6, 3, −12}, n{h,χ,W,Z,t} = {1, 3, 2, 1, 1}, Ci = 3/2 for i = h, χ, t, S and Ci = 5/6 for i = W, Z, while coefficients for the new scalar are listed in table 1. More careful resummation techniques of the thermal corrections have similar effect [34]. This is most important in the coloured scalar case due to potentially large QCD corrections. Our results qualitatively agree with two-loop results from [35] and we conclude that higher order corrections would not change our results dramatically
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