Axion dark matter in a 3−3−1 model

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dc.creatorJuan Carlos Montero Garcia
dc.creatorAna Rubiela Romero Castellanos
dc.creatorBruce Lehmann Sánchez Vega
dc.date.accessioned2023-07-17T19:30:02Z
dc.date.accessioned2025-09-09T01:23:53Z
dc.date.available2023-07-17T19:30:02Z
dc.date.issued2018
dc.description.sponsorshipCAPES - Coordenação de Aperfeiçoamento de Pessoal de Nível Superior
dc.description.sponsorshipFAPESP - Fundação de Amparo à Pesquisa do Estado de São Paulo
dc.format.mimetypepdf
dc.identifier.doihttps://doi.org/10.1103/PhysRevD.97.063015
dc.identifier.issn2470-0029
dc.identifier.urihttps://hdl.handle.net/1843/56473
dc.languageeng
dc.publisherUniversidade Federal de Minas Gerais
dc.relation.ispartofPhysical Review D
dc.rightsAcesso Aberto
dc.subjectMatéria escura
dc.subject.otherAxion
dc.subject.otherDark matter
dc.subject.other3−3−1 model
dc.titleAxion dark matter in a 3−3−1 model
dc.typeArtigo de periódico
local.citation.epage063015-12
local.citation.issue6
local.citation.spage063015-1
local.citation.volume97
local.description.resumoSlightly extending a right-handed neutrino version of the 3−3−1 model, we show that it is not only possible to solve the strong CP problem but also to give the total dark matter abundance reported by the Planck collaboration. Specifically, we consider the possibility of introducing a 3−3−1 scalar singlet to implement a gravity stable Peccei-Quinn mechanism in this model. Remarkably, for allowed regions of the parameter space, the arising axions with masses ma≈meV can both make up the total dark matter relic density through nonthermal production mechanisms and be very close to the region to be explored by the IAXO helioscope.
local.identifier.orcidhttps://orcid.org/0000-0002-5457-9359
local.identifier.orcidhttps://orcid.org/0000-0002-6115-229X
local.identifier.orcidhttps://orcid.org/0000-0002-6735-5813
local.publisher.countryBrasil
local.publisher.departmentICX - DEPARTAMENTO DE FÍSICA
local.publisher.initialsUFMG
local.url.externahttps://journals.aps.org/prd/abstract/10.1103/PhysRevD.97.063015

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