Higgs inflation and suppression of axion isocurvature perturbation

Nakayama, Kazunori; Takimoto, Munehiro

doi:10.1016/j.physletb.2015.07.001

Cited by 23 publications

(42 citation statements)

References 64 publications

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“…In addition, several cosmological constraints on the parameter of the model are also discussed in detail. There exists related work combining double Higgs inflation with the DFSZ axion [48], and a comparison between that work and the present one will be presented in the conclusions.…”

Section: Introductionmentioning

confidence: 79%

“…[48], which corresponds to the DFSZ axion model. In the later case, the isocurvature problem is avoided in the context of several Higgs inflationary scenarios [48].…”

Section: Discussionmentioning

confidence: 99%

“…In the present work, a double Higgs inflationary mechanism [45][46][47][48] involving the ordinary Higgs and the KSVZ Peccei-Quinn field will be considered. It is argued here that the KSVZ field falls to the minima inside the inflationary period, in such a way that the topological defects are diluted away.…”

Section: Introductionmentioning

confidence: 99%

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About the isocurvature tension between axion and high scale inflationary models

Estévez

Santillán

2016

Eur. Phys. J. C

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The present work suggests that the isocurvature tension between axion and high energy inflationary scenarios may be avoided by considering a double field inflationary model involving the hidden Peccei-Quinn Higgs and the Standard Model one. Some terms in the lagrangian we propose explicitly violate the Peccei-Quinn symmetry but, at the present era, their effect is completely negligible. The resulting mechanism allows for a large value for the axion constant, of the order f a ∼ M p , thus the axion isocurvature fluctuations are suppressed even when the scale of inflation H inf is very high, of the order of H inf ∼ M gut . This numerical value is typical in Higgs inflationary models. An analysis about topological defect formation in this scenario is also performed, and it is suggested that, under certain assumptions, their effect is not catastrophic from the cosmological point of view.

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Section: Introductionmentioning

confidence: 79%

“…[48], which corresponds to the DFSZ axion model. In the later case, the isocurvature problem is avoided in the context of several Higgs inflationary scenarios [48].…”

Section: Discussionmentioning

confidence: 99%

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About the isocurvature tension between axion and high scale inflationary models

Estévez

Santillán

2016

Eur. Phys. J. C

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“…Early-and late-time accelerations of the universe expansion can be explained in the framework of scalar field models [1][2][3][4][5][6][7][29][30][31][32][33][34][35]. The consideration of f (R, T ) gravity in the case of a self-interacting scalar field φ yields f (R, T φ ) gravity [12].…”

Section: The F (R T φ ) Gravitymentioning

confidence: 99%

“…It is common to describe this phenomenon via scalar fields [1][2][3][4][5][6][7], although another reputed form to describe it comes from f (R) gravity [8][9][10][11].…”

Section: Introductionmentioning

confidence: 99%

A complete cosmological scenario from $$f(R,T^{\phi })$$ f ( R , T ϕ )

Moraes¹,

Santos²

2016

Eur. Phys. J. C

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Recent elaborated by Harko et al., the f (R, T ) theories of gravity allow one to contemplate an optimistic alternative to dark energy, for which R and T stand for the Ricci scalar and the trace of the energy-momentum tensor, respectively. Although the literature has shown that the T dependence on the gravitational part of the action -which is due to the consideration of quantum effects -may induce some novel features in the scope of late-time cosmological dynamics, in the radiation-dominated universe, when T = 0, no contributions seem to arise from such theories. Apparently, f (R, T ) contributions to a radiation-dominated universe may arise only from the f (R, T φ ) approach, which is nothing but the f (R, T ) gravity in the case of a selfinteracting scalar field whose trace of the energy-momentum tensor is T φ . We intend, in this article, to show how f (R, T φ ) theories of gravity can contribute to the study of the primordial stages of the universe. Our results predict a graceful exit from an inflationary stage to a radiation-dominated era. They also predict a late-time cosmic acceleration after a matter-dominated phase, enabling the f (R, T φ ) theories to describe, in a self-consistent way, all the different stages of the dynamics of the universe.

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Adiabatic suppression of the axion abundance and isocurvature due to coupling to hidden monopoles

Kawasaki

Takahashi

Yamada

2018

J. High Energ. Phys.

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Abstract:The string theory predicts many light fields called moduli and axions, which cause a cosmological problem due to the overproduction of their coherent oscillation after inflation. One of the prominent solutions is an adiabatic suppression mechanism, which, however, is non-trivial to achieve in the case of axions because it necessitates a large effective mass term which decreases as a function of time. The purpose of this paper is twofold. First, we provide an analytic method to calculate the cosmological abundance of coherent oscillation in a general situation under the adiabatic suppression mechanism. Secondly, we apply our method to some concrete examples, including the one where a string axion acquires a large effective mass due to the Witten effect in the presence of hidden monopoles.

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Higgs inflation and suppression of axion isocurvature perturbation

Cited by 23 publications

References 64 publications

About the isocurvature tension between axion and high scale inflationary models

About the isocurvature tension between axion and high scale inflationary models

A complete cosmological scenario from $$f(R,T^{\phi })$$ f ( R , T ϕ )

Adiabatic suppression of the axion abundance and isocurvature due to coupling to hidden monopoles

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