Is the primary CoRoT target HD 43587 under a Maunder minimum phase?

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dc.creatorRafael Ramon Ferreira
dc.creatorRafaella Barbosa
dc.creatorMatthieu Sébastien Castro
dc.creatorGustavo Andres Guerrero Eraso
dc.creatorLeandro de Almeida
dc.creatorPatrick Boumier
dc.creatorJosé Dias do Nascimento Júnior
dc.date.accessioned2023-10-31T17:27:43Z
dc.date.accessioned2025-09-08T23:15:25Z
dc.date.available2023-10-31T17:27:43Z
dc.date.issued2020
dc.description.sponsorshipCNPq - Conselho Nacional de Desenvolvimento Científico e Tecnológico
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/10.1051/0004-6361/201937219
dc.identifier.issn1432-0746
dc.identifier.urihttps://hdl.handle.net/1843/60352
dc.languageeng
dc.publisherUniversidade Federal de Minas Gerais
dc.relation.ispartofAstronomy & Astrophysics
dc.rightsAcesso Aberto
dc.subjectEstrelas
dc.subjectCampos magnéticos
dc.subject.otherStars
dc.subject.otherRotation
dc.subject.otherMagnetic field
dc.titleIs the primary CoRoT target HD 43587 under a Maunder minimum phase?
dc.typeArtigo de periódico
local.citation.epage12
local.citation.spage1
local.citation.volume640
local.description.resumoCONTEXT. One of the most enigmatic phenomena related to solar activity is the so-called Maunder minimum phase. It consists in the lowest sunspot count ever registered for the Sun and has not been confirmed for other stars to date. Since the spectroscopic observations of stellar activity at the Mount Wilson Observatory, the solar analog HD 43587 has shown a very low and apparently invariant activity level, which makes it a Maunder minimum candidate. AIMS. We aim to analyze the chromospheric activity evolution of HD 43587 and its evolutive status, with the intention of unraveling the reasons for this low and flat activity. METHODS. We used an activity measurements dataset available in the literature, and computed the S -index from HARPS and NARVAL spectra to infer a cycle period. Additionally, we analyzed the CoRoT light curve of HD 43587, and applied gyrochronology and activity calibrations to determine its rotation period. Finally, based on an evolutionary model and the inferred rotation period, we used the EULAG-MHD code to perform global MHD simulations of HD 43587 to get some insight into its dynamo process. RESULTS. We confirm the almost flat activity profile, with a cycle period Pcyc = 10.44 ± 3.03 yr deduced from the S -index time series, and a long-term trend that might be a period of more than 50 yr. It was impossible to define a rotation period from the light curve, however gyrochronology and activity calibrations allow us to infer an indirect estimate of Prot = 22.6 ± 1.9 d. Furthermore, the MHD simulations confirm an oscillatory dynamo with a cycle period in good agreement with the observations and a low level of surface magnetic activity. CONCLUSIONS. We conclude that this object might be experiencing a “natural” decrease in magnetic activity as a consequence of its age. Nevertheless, the possibility that HD 43587 is in a Maunder minimum phase cannot be ruled out.
local.identifier.orcidhttp://orcid.org/0000-0001-7255-3489
local.identifier.orcidhttps://orcid.org/0000-0002-1332-2477
local.identifier.orcidhttps://orcid.org/0000-0002-2671-8796
local.identifier.orcidhttps://orcid.org/0000-0001-8179-1147
local.identifier.orcidhttps://orcid.org/0000-0001-7804-2145
local.publisher.countryBrasil
local.publisher.departmentICX - DEPARTAMENTO DE FÍSICA
local.publisher.initialsUFMG
local.url.externahttps://www.aanda.org/articles/aa/abs/2020/08/aa37219-19/aa37219-19.html

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