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Baryogenesis and gravitational waves in the Zee–Babu model

The European physical journal. C, Particles and fields, 2022-11, Vol.82 (11), p.1005-16, Article 1005 [Peer Reviewed Journal]

The Author(s) 2022 ;COPYRIGHT 2022 Springer ;The Author(s) 2022. This work is published under http://creativecommons.org/licenses/by/4.0/ (the “License”). Notwithstanding the ProQuest Terms and Conditions, you may use this content in accordance with the terms of the License. ;ISSN: 1434-6052 ;ISSN: 1434-6044 ;EISSN: 1434-6052 ;DOI: 10.1140/epjc/s10052-022-10961-2

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  • Title:
    Baryogenesis and gravitational waves in the Zee–Babu model
  • Author: Phong, Vo Quoc ; Thao, Nguyen Chi ; Long, Hoang Ngoc
  • Subjects: Antimatter ; Astronomy ; Astrophysics and Cosmology ; Bosons ; Cosmology ; Density ; Elementary Particles ; Gravitational waves ; Hadrons ; Heavy Ions ; Mathematical models ; Measurement Science and Instrumentation ; Nuclear Energy ; Nuclear Physics ; Parameters ; Phase transitions ; Physics ; Physics and Astronomy ; Quantum Field Theories ; Quantum Field Theory ; Regular Article - Theoretical Physics ; Scaling laws ; String Theory
  • Is Part Of: The European physical journal. C, Particles and fields, 2022-11, Vol.82 (11), p.1005-16, Article 1005
  • Description: To explain the matter-antimatter asymmetry in the Zee–Babu (ZB) model, the sphaleron process in the baryogenesis scenario is calculated. It always satisfies the de-coupling condition and the strength of phase transition ( S ) is always greater than 1 in the presence of triggers other than that in the Standard Model, which are singly ( h ± ) and doubly ( k ± ± ) charged scalar bosons. Sphaleron energies are in the range of 5-10 TeV, in calculation with bubble profiles containing free parameters and assuming nuclear bubbles of h ± and k ± ± are very small. We tested the scaling law of sphaleron again with an average error of 10 % . When the temperature is close to the critical one ( T c ), the density of nuclear bubble is produced very large and decreases as the temperature decreases. The key parameter is α which results in the gravitational wave density parameter ( Ω h 2 ) in the range of 10 - 14 to 10 - 12 when β / H ∗ = 22.5 , this is not enough to detect gravitational waves from electroweak phase transition (EWPT) according to the present LISA data but may be detected in the future. As the larger strength of phase transition is, the more α increases (this increase is almost linear with S ), the larger the gravitational wave density parameter is. Also in the context of considering the generation of gravitational waves, in the ZB model we calculated α ∼ a few × 10 - 2 ≪ 1 , so rigorously conclude that the EWPT is not strong even though S > 1 . We also suggest that, for a model with a lot of extra scalar particles and particles which play a role in mass generation, the stronger the EWPT process and the larger Ω h 2 can be.
  • Publisher: Berlin/Heidelberg: Springer Berlin Heidelberg
  • Language: English
  • Identifier: ISSN: 1434-6052
    ISSN: 1434-6044
    EISSN: 1434-6052
    DOI: 10.1140/epjc/s10052-022-10961-2
  • Source: SpringerOpen website
    ProQuest Central
    DOAJ Directory of Open Access Journals
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