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Authordc.contributor.authorBecerra, Laura
Authordc.contributor.authorReisenegger, Andreas
Authordc.contributor.authorValdivia Hepp, Juan Alejandro
Authordc.contributor.authorGusakov, Mikhail E.
Admission datedc.date.accessioned2022-06-30T21:48:00Z
Available datedc.date.available2022-06-30T21:48:00Z
Publication datedc.date.issued2022
Cita de ítemdc.identifier.citationMNRAS 000, 1–14 (2021)es_ES
Identifierdc.identifier.other10.1093/mnras/stac102
Identifierdc.identifier.urihttps://repositorio.uchile.cl/handle/2250/186381
Abstractdc.description.abstractLong-lived magnetic fields are known to exist in upper main-sequence stars, white dwarfs, and neutron stars. In order to explore possible equilibrium configurations of the magnetic field inside these stars, we have performed 3D-magnetohydrodynamic simulations of the evolution of initially random magnetic fields in stably stratified and barotropic stars with an ideal-gas equation of state using the Pencil Code, a high-order finite-difference code for compressible hydrodynamic flows in the presence of magnetic fields. In barotropic (isentropic) stars, we confirm previous results in the sense that all initial magnetic fields we tried decay away, unable to reach a stable equilibrium. In the case of stably stratified stars (with radially increasing specific entropy), initially random magnetic fields appear to always evolve to a stable equilibrium. However, the nature of this equilibrium depends on the dissipation mechanisms considered. If magnetic diffusivity (or hyperdiffusivity) is included, the final state is more axially symmetric and dominated by large wavelengths than the initial state, whereas this is not the case if only viscosity (or hyperviscosity) is present. In real stars, the main mechanism allowing them to relax to an equilibrium is likely to be phase mixing, which we argue is more closely mimicked by viscosity. Therefore, we conclude that, depending on its formation mechanism, the equilibrium magnetic field in these stars could in principle be very asymmetric.es_ES
Patrocinadordc.description.sponsorshipComision Nacional de Investigacion Cientifica y Tecnologica (CONICYT) CONICYT FONDECYT 3190172 1201582 1190703 CEDENNA under CONICYT grant AFB180001 Russian Foundation for Basic Research (RFBR) 19-52-12013 Comision Nacional de Investigacion Cientifica y Tecnologica (CONICYT) CONICYT PIA/BASAL PFB-06 FONDEQUIP AIC-57 QUIMAL 130008es_ES
Lenguagedc.language.isoenes_ES
Publisherdc.publisherOxfordes_ES
Type of licensedc.rightsAttribution-NonCommercial-NoDerivs 3.0 United States*
Link to Licensedc.rights.urihttp://creativecommons.org/licenses/by-nc-nd/3.0/us/*
Sourcedc.sourceMonthly Notices of The Royal Astronomical Societyes_ES
Keywordsdc.subjectMHDes_ES
Keywordsdc.subjectStars: magnetic fieldes_ES
Keywordsdc.subjectStars: massivees_ES
Keywordsdc.subjectStars: neutrones_ES
Keywordsdc.subjectStars: white dwarfses_ES
Keywordsdc.subjectSoftware: simulationses_ES
Títulodc.titleEvolution of random initial magnetic fields in stably stratified and barotropic starses_ES
Document typedc.typeArtículo de revistaes_ES
dc.description.versiondc.description.versionVersión sometida a revisión - Preprintes_ES
dcterms.accessRightsdcterms.accessRightsAcceso abiertoes_ES
Catalogueruchile.catalogadorcrbes_ES
Indexationuchile.indexArtículo de publícación WoSes_ES


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Attribution-NonCommercial-NoDerivs 3.0 United States
Except where otherwise noted, this item's license is described as Attribution-NonCommercial-NoDerivs 3.0 United States