Editorial

Nardi, Henrique Caetano; Machado, Paula Sandrine

doi:10.22456/2238-152x.31523

Cited by 5 publications

(10 citation statements)

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“…The baryon number of the universe in the leptogenesis scenario depends on the decay of the lightest right-handed neutrinos, [29][30][31][32][33][34][35][36][37][38] where we assume that M 1 ≪ M 2 , M 3 . The CP asymmetry parameter from the decay of the lightest right-handed neutrino N 1 is obtained from…”

Section: Summary and Discussionmentioning

confidence: 99%

“…20 In the future experiments, more sensitivity |M ee | ≃ a few meV will be reached. 20 We use one flavor dominant approximation [35][36][37][38] for M 1 = 10 10 − 10 14 GeV for the sake of simplicity. More general analysis will be found in our future study.…”

Section: Summary and Discussionmentioning

confidence: 99%

“…for 10 12 GeV ≤ M 1 (one flavor dominant case [35][36][37][38] ) where washout effect on ǫ i in the expanding universe is controlled by…”

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confidence: 99%

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Seesaw model and two zero flavor neutrino texture

Kitabayashi

Yasuè

2017

Int. J. Mod. Phys. A

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In the two zero flavor neutrino mass matrix scheme with nonvanishing Majorana effective mass Mee for the neutrinoless double beta decay, four textures are compatible with observed data. We obtain the complete list of the possible textures of four zero Dirac neutrino mass matrix m D in the seesaw mechanism providing these four flavor neutrino textures. Explicit analytical analysis of m D turns out to provide the relation of m D ∝ √ Mee.

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Section: Summary and Discussionmentioning

confidence: 99%

Section: Summary and Discussionmentioning

confidence: 99%

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Seesaw model and two zero flavor neutrino texture

Kitabayashi

Yasuè

2017

Int. J. Mod. Phys. A

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“…The prediction for the baryon asymmetry in the Universe requires to compute the CP asymmetry parameter ε and to take into consideration its evolution during the expansion of the Universe, which depends on the interactions that are in thermal equilibrium at different temperatures. With this respect, the value of the RH neutrino mass scale µ L is a fundamental parameter as it identifies different flavour regimes [141][142][143][144][145][146][147]: the lower µ L is, the more relevant the flavour composition of the charged leptons produced in the RH neutrino decays is. For the SU (3) V MLFV framework, µ L 10 14 GeV and it corresponds to the so-called unflavoured regime, where the charged lepton flavour does not play any role.…”

Section: Baryogenesis Trough Leptogenesismentioning

confidence: 99%

Predictive leptogenesis from minimal lepton flavour violation

Merlo

Rosauro-Alcaraz

2018

J. High Energ. Phys.

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A predictive Leptogenesis scenario is presented based on the Minimal Lepton Flavour Violation symmetry. In the realisation with three right-handed neutrinos transforming under the same flavour symmetry of the lepton electroweak doublets, lepton masses and PMNS mixing parameters can be described according to the current data, including a large Dirac CP phase. The observed matter-antimatter asymmetry of the Universe can be achieved through Leptogenesis, with the CP asymmetry parameter ε described in terms of only lepton masses, mixings and phases, plus two real parameters of the low-energy effective description. This is in contrast with the large majority of models present in the literature, where ε depends on several high-energy parameters, preventing a direct connection between low-energy observables and the baryon to photon ratio today. Recovering the correct amount of baryon asymmetry in the Universe constrains the Majorana phases of the PMNS matrix within specific ranges of values: clear predictions for the neutrinoless double beta decay emerge, representing a potential smoking gun for this framework.4 In Ref.[71], considering the SO(3) × CP version of MLFV, the equivalent of the coefficients c 1,2 have been shown to be generated by radiative corrections during the evolution of the Lagrangian parameters. Experiment Isotope |mee| [ eV] CUORE [188] 130 Te 0.073 ± 0.008 GERDA-II [189] 76 Ge 0.11 ± 0.01 LUCIFER [190] 82 Se 0.20 ± 0.02 MAJORANA D. [191] 76 Ge 0.13 ± 0.01 NEXT [192] 136 Xe 0.12 ± 0.01 AMoRE [193] 100 Mo 0.084 ± 0.008 nEXO [194] 136 Xe 0.011 ± 0.001 PandaX-III [195] 136 Xe 0.082 ± 0.009 SNO+ [196] 130 Te 0.076 ± 0.007 SuperNEMO [197] 82 Se 0.084 ± 0.008

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“…Depending on the nature of the decaying particle, the decay products may include γ-photons, electrons, positrons and other more exotic particles. For example, detection of positrons of tens of GeV by the PAMELA (Adriani et al 2009) can be explained by the injection from annihilation and/or decay of dark matter (He 2009;Nardi et al 2009). It is clear however that through formation of particle showers the decays end when weakly interacting stable particles escape, while the other couple to baryons via electromagnetic interactions, ionize them and deposit energy.…”

Section: Ionization and Heatingmentioning

confidence: 99%

THE SIGNATURES OF PARTICLE DECAY IN 21 cm ABSORPTION FROM THE FIRST MINIHALOS

Vasiliev

Shchekinov

2013

ApJ

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The imprint of decaying dark matter (DM) particles in characteristics of the "21 cm forest"absorptions in 21 cm from minihalos in spectra of distant radio-loud sources -is considered within a 1D self-consistent hydrodynamic description of minihalos from their turnaround point to virialization. The most pronounced influence of decaying DM on evolution of minihalos is found in the mass range M = 10 5 − 10 6 M ⊙ , for which unstable DM with the current upper limit of the ionization rate ξ L = 0.59 × 10 −25 s −1 depresses 21 cm optical depth by an order of magnitude compared to the standard recombination scenario. Even rather a modest ionization ξ ∼ 0.3ξ L practically "erases" absorption features and results in a considerable decrease (by factor of more than 2.5) of the number of strong (W obs ν > ∼ 0.3 kHz at z ≃ 10) absorptions. At such circumstances broad-band observations are to be more suitable for inferring physical conditions of the absorbing gas. X-ray photons from stellar activity of initial episodes of star formation can compete the contribution from decaying DM only at z < 10. Therefore, when observed the 21 cm signal will allow to follow evolution of decaying DM particles in the redshift range z = 10 − 15. Contrary, in case of non-detection of the 21 cm signal in the frequency range ν < 140 MHz a lower limit on the ionization rate from decaying dark matter can be established.

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Editorial

Cited by 5 publications

References 0 publications

Seesaw model and two zero flavor neutrino texture

Seesaw model and two zero flavor neutrino texture

Predictive leptogenesis from minimal lepton flavour violation

THE SIGNATURES OF PARTICLE DECAY IN 21 cm ABSORPTION FROM THE FIRST MINIHALOS

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