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Please use this identifier to cite or link to this item: http://hdl.handle.net/1843/60867
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dc.creatorGustavo Andres Guerrero Erasopt_BR
dc.creatorFabio Del Sordopt_BR
dc.creatorAlfio Maurizio Bonannopt_BR
dc.creatorPiotr Krzysztof Smolarkiewiczpt_BR
dc.date.accessioned2023-11-13T16:02:38Z-
dc.date.available2023-11-13T16:02:38Z-
dc.date.issued2019-
dc.citation.volume490pt_BR
dc.citation.issue3pt_BR
dc.citation.spage4281pt_BR
dc.citation.epage4291pt_BR
dc.identifier.doihttps://doi.org/10.1093/mnras/stz2849pt_BR
dc.identifier.issn1365-2966pt_BR
dc.identifier.urihttp://hdl.handle.net/1843/60867-
dc.description.resumoUnveiling the evolution of toroidal field instability, known as Tayler instability, is essential to understand the strength and topology of the magnetic fields observed in early-type stars, in the core of the red giants, or in any stellar radiative zone. We want to study the non-linear evolution of the instability of a toroidal field stored in a stably stratified layer, in spherical symmetry and in the absence of rotation. In particular, we intend to quantify the suppression of the instability as a function of the Brunt–V¨ais¨ala (ωBV ) and the Alfv´en (ωA ) frequencies. We use the magnetohydrodynamic (MHD) equations as implemented in the anelastic approximation in the EULAG–MHD code and perform a large series of numerical simulations of the instability exploring the parameter space for the ωBV and ωA . We show that beyond a critical value gravity strongly suppress the instability, in agreement with the linear analysis. The intensity of the initial field also plays an important role: weaker fields show much slower growth rates. Moreover, in the case of very low gravity, the fastest growing modes have a large characteristic radial scale, at variance with the case of strong gravity, where the instability is characterized by horizontal displacements. Our results illustrate that the anelastic approximation can efficiently describe the evolution of toroidal field instability in stellar interiors. The suppression of the instability as a consequence of increasing values of ωBV might play a role to explain the magnetic desert in Ap/Bp stars, since weak fields are only marginally unstable in the case of strong gravity.pt_BR
dc.format.mimetypepdfpt_BR
dc.languageengpt_BR
dc.publisherUniversidade Federal de Minas Geraispt_BR
dc.publisher.countryBrasilpt_BR
dc.publisher.departmentICX - DEPARTAMENTO DE FÍSICApt_BR
dc.publisher.initialsUFMGpt_BR
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society-
dc.rightsAcesso Abertopt_BR
dc.subjectStarspt_BR
dc.subjectMagnetic fieldpt_BR
dc.subjectGravitypt_BR
dc.subject.otherEstrelaspt_BR
dc.subject.otherCampos magnéticospt_BR
dc.subject.otherGravidadept_BR
dc.titleGlobal simulations of Tayler instability in stellar interiors: the stabilizing effect of gravitypt_BR
dc.typeArtigo de Periódicopt_BR
dc.url.externahttps://academic.oup.com/mnras/article/490/3/4281/5586574pt_BR
dc.identifier.orcidhttps://orcid.org/0000-0002-2671-8796pt_BR
dc.identifier.orcidhttps://orcid.org/0000-0001-9268-4849pt_BR
dc.identifier.orcidhttps://orcid.org/0000-0003-3175-9776pt_BR
dc.identifier.orcidhttps://orcid.org/0000-0001-7077-3285pt_BR
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