Baryogenesis from axion inflation

Domcke, Valerie; Harling, Benedict von; Morgante, Enrico; Mukaida, Kyohei

doi:10.1088/1475-7516/2019/10/032

Cited by 88 publications

(146 citation statements)

References 75 publications

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“…On the other hand, expanding in the infrared (IR) limit (−kτ 1) the integrand of Eq. (15) has no IR divergences.…”

Section: Energy-momentum Tensor and Helicitymentioning

confidence: 99%

“…Considering the energy density and the helicity, the bare expectation values are those computed in the previous section for µ = 0 (see Eqs. (15) and (18)) or their extensions to µ = 0 given in Appendix B. Their adiabatic counterpart is instead given by their corresponding integrals expressed in terms of the WKB mode functions of a given adiabatic order n. Namely, these are given by Eqs.…”

Section: Adiabatic Expansion and Regularizationmentioning

confidence: 99%

“…In this appendix we give the analytical expressions of the bare integrals in Eqs. (15) and (18). We carefully show the calculation of the energy density of Eq.…”

Section: A Calculation Of the Energy Density And Its Backreactionmentioning

confidence: 99%

“…where g is a coupling constant with a physical dimension of length, or inverse energy (we put = c = 1), leads to decay of the pseudo-scalar field into gauge fields modifying its background dynamics [1] and to a wide range of potentially observable signatures including primordial magnetic fields [2][3][4][5][6][7][8][9][10], preheating at the end of * mario.ballardini@gmail.com † matteo.braglia2@unibo.it ‡ fabio.finelli@inaf.it § giovanni.marozzi@unipi.it ¶ alstar@landau.ac.ru inflation [4,11,12] , baryogenesis and leptogenesis [13][14][15], equilateral non-Gaussianites [16][17][18], chiral gravitational waves in the range of direct detection by gravitational wave antennas [19][20][21][22], and primordial black holes (PBHs) [18,[23][24][25][26]. The decay of the inflaton into gauge fields due to the coupling in Eq.…”

Section: Introductionmentioning

confidence: 99%

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Energy-momentum tensor and helicity for gauge fields coupled to a pseudoscalar inflaton

et al. 2019

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We study the energy-momentum tensor and helicity of gauge fields coupled through gφFF /4 to a pseudo-scalar field φ driving inflation. Under the assumption of a constant time derivative of the background inflaton, we compute analitically divergent and finite terms of the energy density and helicity of gauge fields for any value of the coupling g. We introduce a suitable adiabatic expansion for mode functions of physical states of the gauge fields which correctly reproduces ultraviolet divergences in average quantities and identify corresponding counterterms. Our calculations shed light on the accuracy and the range of validity of approximated analytic estimates of the energy density and helicity terms previously existed in the literature in the strongly coupled regime only, i.e. for gφ/(2H)1. We discuss the implications of our analytic calculations for the backreaction of quantum fluctuations onto the inflaton evolution.

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“…On the other hand, expanding in the infrared (IR) limit (−kτ 1) the integrand of Eq. (15) has no IR divergences.…”

Section: Energy-momentum Tensor and Helicitymentioning

confidence: 99%

Section: Adiabatic Expansion and Regularizationmentioning

confidence: 99%

“…In this appendix we give the analytical expressions of the bare integrals in Eqs. (15) and (18). We carefully show the calculation of the energy density of Eq.…”

Section: A Calculation Of the Energy Density And Its Backreactionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Energy-momentum tensor and helicity for gauge fields coupled to a pseudoscalar inflaton

et al. 2019

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“…Interestingly, they can be used to solve open problems of the SM as they are well-motivated candidates to explain e.g. dark matter [3][4][5], inflation [6,7], and baryogenesis [8,9]. They were originally introduced to solve the Strong CP problem [10,11] and still remain the most popular explanation to this puzzle.…”

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confidence: 99%

Axion fragmentation

Fonseca

Morgante

Sato

et al. 2020

J. High Energ. Phys.

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137

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We investigate the production of axion quanta during the early universe evolution of an axion-like field rolling down a wiggly potential. We compute the growth of quantum fluctuations and their back-reaction on the homogeneous zeromode. We evaluate the transfer of kinetic energy from the zero mode to the quantum fluctuations and the conditions to decelerate the axion zero-mode as a function of the Hubble rate, the slope of the potential, the size of the barriers and the initial field velocity. We discuss how these effects impact the relaxion mechanism. arXiv:1911.08472v1 [hep-ph] 19 Nov 2019 1 As this work was being completed, Ref.[15] appeared, which considers the production of axion quantum fluctuations during oscillations about the minimum of the potential, as in [14]. This effect is important only if the initial position of the axion field is tuned very close to the top of the barrier of the axion potential, at the level of ∼ 10 −7 . Such peculiar initial position was recently motivated by some inflation dynamics in [16] and by anthropic arguments in [17].

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Standard Model of Cosmology

Gouttenoire

2022

Beyond the Standard Model Cocktail

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Baryogenesis from axion inflation

Abstract: 1 Here we assume that the sphaleron and Yukawa interactions are not efficient during inflation. 2 We have expanded in µ α /T for µ α /T 1 which will always be fulfilled in the cases of interest.

Cited by 88 publications

References 75 publications

Energy-momentum tensor and helicity for gauge fields coupled to a pseudoscalar inflaton

Energy-momentum tensor and helicity for gauge fields coupled to a pseudoscalar inflaton

Axion fragmentation

Standard Model of Cosmology

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