MeV-scale reheating temperature and thermalization of oscillating neutrinos by radiative and hadronic decays of massive particles

Hasegawa, T.; Hiroshima, Nagisa; Kohri, Kazunori; Hansen, Rasmus S. L.; Tram, Thomas; Hannestad, Steen

doi:10.1088/1475-7516/2019/12/012

Cited by 243 publications

(210 citation statements)

References 36 publications

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“…Therefore, there is a range of m outside of which agreement with A s data can not be obtained, for any value of the equation of state parameter, in the interval −1/3 ≤ w ≤ 1. This range is actually very tight and falls within the suggested range given by (73). Within this range there are fine-tuned values for which reheating can be instantaneous.…”

Section: Model Isupporting

confidence: 75%

“…The reheating temperature should be larger than M eV so that Big Bang Nucleosynthesis (BBN) is not upset. Lower values on T reh have been established in [72] and recently in [73] .…”

Section: Cosmological Observablesmentioning

confidence: 95%

“…As we shall see this estimate is not far from the one we get in our numerical treatment. What is more important, perhaps, is the fact that in the regime of small c the power spectrum amplitude, which forces m to be within the limits suggested by (73), also determines the maximum reheating temperature.…”

Section: Model Imentioning

confidence: 97%

“…It is worth mentioning that given a fixed value for the parameter a there is a fine-tuned value of m, in the range suggested by (73), for which the case w = 1/3 falls within the allowed region by A s observations 6 . In this case the instantaneous reheating temperature is attained for any value of w in the range −1/3 ≤ w ≤ 1.…”

Section: Model Imentioning

confidence: 97%

“…These have not been randomly chosen. In fact, for the case A the parameter a touches its lower bound, discussed before, and c has been taken so that m falls well within the range suggested by (73). In fact we choose m 6.32 × 10 −6 .…”

Section: Model Imentioning

confidence: 99%

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Reheating in R2 Palatini inflationary models

Gialamas

Lahanas

2020

Phys. Rev. D

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We consider R 2 inflation in the Palatini gravity assuming the existence of scalar fields, coupled to gravity in the most general manner. These theories, in the Einstein frame, and for one scalar field h, share common features with K -inflation models. We apply this formalism for the study of popular inflationary models, whose potentials are monomials, V ∼ h n , with n a positive even integer. We also study the Higgs model non-minimally coupled to gravity. Although these have been recently studied, in the framework of the Palatini approach, we show that the scalar power spectrum severely constrains these models. Although we do not propose a particular reheating mechanism, we show that the quadratic ∼ h 2 and the Higgs model can survive these constraints with a maximum reheating temperature as large as ∼ 10 15 GeV , when reheating is instantaneous. However, this can be only attained at the cost of a delicate fine-tuning of couplings. Deviations from this fine-tuned values can still yield predictions compatible with the cosmological data, for couplings that lie in very tight range, giving lower reheating temperatures.

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Section: Model Isupporting

confidence: 75%

“…The reheating temperature should be larger than M eV so that Big Bang Nucleosynthesis (BBN) is not upset. Lower values on T reh have been established in [72] and recently in [73] .…”

Section: Cosmological Observablesmentioning

confidence: 95%

Section: Model Imentioning

confidence: 97%

Section: Model Imentioning

confidence: 97%

Section: Model Imentioning

confidence: 99%

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Reheating in R2 Palatini inflationary models

Gialamas

Lahanas

2020

Phys. Rev. D

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f(R)$f(R)$‐Gravity Generated Post‐Inflationary Eras and Their Effect on Primordial Gravitational Waves

Oikonomou

2022

Annalen der Physik

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In this work the effects of a geometrically generated post-inflationary era on the energy spectrum of the primordial gravitational waves are considered. Specifically, a post-inflationary constant equation of state era, generated by the synergistic effect of f (R) gravity and of radiation and matter perfect fluids shall be considered. Two cases of interest shall be studied, one with equation of state parameter w = −1∕3, in which case the Universe neither accelerates nor decelerates, and one with w = 0 so an early matter domination era. For the evaluation of the inflationary observational indices which is relevant for the calculation of the gravitational waves energy spectrum, the effects of the constant equation of state parameter era, on the e-foldings number is also taken into account. In both the w = −1∕3 and w = 0 cases, the energy spectrum of the primordial gravitational waves is amplified, but for the w = 0 case, the effect is stronger.

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Sterile neutrino dark matter and leptogenesis in Left-Right Higgs Parity

Dunsky

Hall

Harigaya

2021

J. High Energ. Phys.

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The standard model Higgs quartic coupling vanishes at (109 − 1013) GeV. We study SU(2)L× SU(2)R× U(1)B−L theories that incorporate the Higgs Parity mechanism, where this becomes the scale of Left-Right symmetry breaking, vR. Furthermore, these theories solve the strong CP problem and predict three right-handed neutrinos. We introduce cosmologies where SU(2)R× U(1)B−L gauge interactions produce right-handed neutrinos via the freeze-out or freeze-in mechanisms. In both cases, we find the parameter space where the lightest right-handed neutrino is dark matter and the decay of a heavier one creates the baryon asymmetry of the universe via leptogenesis. A theory of flavor is constructed that naturally accounts for the lightness and stability of the right-handed neutrino dark matter, while maintaining sufficient baryon asymmetry. The dark matter abundance and successful natural leptogenesis require vR to be in the range (1010− 1013) GeV for freeze-out, in remarkable agreement with the scale where the Higgs quartic coupling vanishes, whereas freeze-in requires vR ≳ 109 GeV. The allowed parameter space can be probed by the warmness of dark matter, precise determinations of the top quark mass and QCD coupling by future colliders and lattice computations, and measurement of the neutrino mass hierarchy.

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MeV-scale reheating temperature and thermalization of oscillating neutrinos by radiative and hadronic decays of massive particles

Cited by 243 publications

References 36 publications

Reheating in R2 Palatini inflationary models

Reheating in R2 Palatini inflationary models

f(R)$f(R)$‐Gravity Generated Post‐Inflationary Eras and Their Effect on Primordial Gravitational Waves

Sterile neutrino dark matter and leptogenesis in Left-Right Higgs Parity

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