Linking axionlike dark matter to neutrino masses

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dc.creatorCristian David Ruiz Carvajal
dc.creatorBruce Lehmann Sánchez Vega
dc.creatorÓscar Alberto Zapata Noreña
dc.date.accessioned2023-07-11T12:22:12Z
dc.date.accessioned2025-09-08T23:13:41Z
dc.date.available2023-07-11T12:22:12Z
dc.date.issued2017
dc.description.sponsorshipCAPES - Coordenação de Aperfeiçoamento de Pessoal de Nível Superior
dc.identifier.doihttps://doi.org/10.1103/PhysRevD.96.115035
dc.identifier.issn2470-0029
dc.identifier.urihttps://hdl.handle.net/1843/56056
dc.languageeng
dc.publisherUniversidade Federal de Minas Gerais
dc.relation.ispartofPhysical Review D
dc.rightsAcesso Restrito
dc.subjectMatéria Escura
dc.subjectNeutrinos
dc.subject.otherAxion like particles
dc.subject.otherNeutrinos
dc.titleLinking axionlike dark matter to neutrino masses
dc.typeArtigo de periódico
local.citation.epage15035-13
local.citation.issue11
local.citation.spage115035-1
local.citation.volume96
local.description.resumoWe present a framework linking axionlike particles (ALPs) to neutrino masses through the minimal inverse seesaw (ISS) mechanism in order to explain the dark matter (DM) puzzle. Specifically, we explore three minimal ISS cases where mass scales are generated through gravity-induced operators involving a scalar field hosting ALPs. In all of these cases, we find gravity-stable models that provide the observed DM relic density and, simultaneously, are consistent with the phenomenology of neutrinos and ALPs. Remarkably, in one of the ISS cases, the DM can be made of ALPs and sterile neutrinos. Furthermore, other considered ISS cases have ALPs with parameters that are within the reach of proposed ALP experiments.
local.identifier.orcidhttps://orcid.org/0000-0002-5799-2464
local.identifier.orcidhttps://orcid.org/0000-0002-6735-5813
local.identifier.orcidhttps://orcid.org/0000-0001-5533-4014
local.publisher.countryBrasil
local.publisher.departmentICX - DEPARTAMENTO DE FÍSICA
local.publisher.initialsUFMG
local.url.externahttps://journals.aps.org/prd/abstract/10.1103/PhysRevD.96.115035

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