Beauty is more attractive: particle production andmoduli trapping with higher dimensional interaction

Enomoto, Seishi; Iida, Satoshi; Maekawa, Nobuhiro; Matsuda, Tomohiro

doi:10.1007/jhep01(2014)141

Cited by 19 publications

(34 citation statements)

References 35 publications

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“…(A.5) and (A.6) refers to the first order WKB mode functions χ WKB k = exp(iω k )/ √ 2ω k , which is needed to cancel a divergence in the effective potential (see e.g. [43,74]). In addition, we assume that the relaxion field is homogeneous in space, i.e.…”

Section: A Equations Of Motionmentioning

confidence: 99%

Higgs relaxation after inflation

Fonseca

Morgante

Servant

2018

J. High Energ. Phys.

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We show that the mechanism of cosmological relaxation of the electroweak scale can take place independently of the inflation mechanism, thus relieving burdens from the original relaxion proposal. What eventually stops the (fast-rolling) relaxion field during its cosmological evolution is the production of particles whose mass is controlled by the Higgs vacuum expectation value. We first show that Higgs particle production does not work for that purpose as the Higgs field does not track the minimum of its potential in the regime where Higgs particles get efficiently produced through their coupling to the relaxion. We then focus on gauge boson production. We provide a detailed analysis of the scanning and stopping mechanism and determine the parameter space for which the relaxion mechanism can take place after inflation, while being compatible with cosmological constraints, such as the relaxion dark matter overabundance and Big Bang Nucleosynthesis. We find that the cutoff scale can be as high as two hundreds of TeV. In this approach, the relaxion sector is responsible for reheating the visible sector. The stopping barriers of the periodic potential are large and Higgs-independent, facilitating model-building. The allowed relaxion mass ranges from 200 MeV up to the weak scale. In this scenario, the relaxion field excursion is subplanckian, and is thus many orders of magnitude smaller than in the original relaxion proposal.

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Section: A Equations Of Motionmentioning

confidence: 99%

Higgs relaxation after inflation

Fonseca

Morgante

Servant

2018

J. High Energ. Phys.

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“…Therefore, we assume for the reheating temperature T R ≪ m 0 < m η , which does not constitute an additional limiting factor. 17…”

Section: Conclusion and Discussionmentioning

confidence: 99%

“…In this paper, we have assumed that higher interactions are very small and negligible. Preheating with higher interactions is partially analyzed in Ref [17][18][19]13.…”

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confidence: 99%

Asymmetric preheating

Enomoto

Matsuda

2018

Int. J. Mod. Phys. A

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We study the generation of the matter-antimatter asymmetry during bosonic preheating, focusing on the sources of the asymmetry. If the asymmetry appears in the multiplication factor of the resonant particle production, the matter-antimatter ratio will grow during preheating. On the other hand, if the asymmetry does not grow during preheating, one has to find out another reason. We consider several scenarios for the asymmetric preheating to distinguish the sources of the asymmetry. We also discuss a new baryogenesis scenario, in which the asymmetry is generated without introducing neither loop corrections nor rotation of a field.

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“…This is a very encouraging result, for it suggests that out-of-equilibrium patches may be feasible candidates to become the seeds of large-angle CMB anomalies, thus offering an avenue to account for the latter without having to invoke an alternative scenario more unlikely that the very existence of anomalies. Yet another feature worth stressing is that one can expect to obtain H * τ t ≥ O(1) without having to impose that the χ field belongs to large GUT groups [60]. On the contrary, the expectation when χ belongs to large GUT groups is that H * τ t ≪ O(1), in which case the emergence of patches becomes a very unlikely event, as Fig.…”

Section: Beyond the Absorbing Barriermentioning

confidence: 99%

Hidden in the background: a local approach to CMB anomalies

Sánchez

Juan²

2016

J. Cosmol. Astropart. Phys.

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Abstract. We investigate a framework aiming to provide a common origin for the large-angle anomalies detected in the Cosmic Microwave Background (CMB), which are hypothesized as the result of the statistical inhomogeneity developed by different isocurvature fields of mass m ∼ H present during inflation. The inhomogeneity arises as the combined effect of (i) the initial conditions for isocurvature fields (obtained after a fast-roll stage finishing many e-foldings before cosmological scales exit the horizon), (ii) their inflationary fluctuations and (iii) their coupling to other degrees of freedom. Our case of interest is when these fields (interpreted as the precursors of large-angle anomalies) leave an observable imprint only in isolated patches of the Universe. When the latter intersect the last scattering surface, such imprints arise in the CMB. Nevertheless, due to their statistically inhomogeneous nature, these imprints are difficult to detect, for they become hidden in the background similarly to the Cold Spot. We then compute the probability that a single isocurvature field becomes inhomogeneous at the end of inflation and find that, if the appropriate conditions are given (which depend exclusively on the preexisting fast-roll stage), this probability is at the percent level. Finally, we discuss several mechanisms (including the curvaton and the inhomogeneous reheating) to investigate whether an initial statistically inhomogeneous isocurvature field fluctuation might give rise to some of the observed anomalies. In particular, we focus on the Cold Spot, the power deficit at low multipoles and the breaking of statistical isotropy.

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Beauty is more attractive: particle production andmoduli trapping with higher dimensional interaction

Cited by 19 publications

References 35 publications

Higgs relaxation after inflation

Higgs relaxation after inflation

Asymmetric preheating

Hidden in the background: a local approach to CMB anomalies

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