Magnetic field generation in PMS stars with and without radiative core

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dc.creatorBonnie Romano Zaire
dc.creatorGustavo Andres Guerrero Eraso
dc.creatorAlexander G. Kosovichev
dc.creatorPiotr Krzysztof Smolarkiewicz
dc.creatorNatalia Rezende Landin
dc.date.accessioned2023-10-31T13:32:35Z
dc.date.accessioned2025-09-08T23:17:44Z
dc.date.available2023-10-31T13:32:35Z
dc.date.issued2016
dc.description.sponsorshipFAPEMIG - Fundação de Amparo à Pesquisa do Estado de Minas Gerais
dc.format.mimetypepdf
dc.identifier.doihttps://doi.org/10.1017/S1743921317003970
dc.identifier.issn1743-9221
dc.identifier.urihttps://hdl.handle.net/1843/60316
dc.languageeng
dc.publisherUniversidade Federal de Minas Gerais
dc.relation.ispartofProceedings of the International Astronomical Union
dc.rightsAcesso Aberto
dc.subjectEstrelas
dc.subjectEstrelas T Tauri
dc.subjectCampo magnético
dc.subject.otherStar
dc.subject.otherT Tauri
dc.titleMagnetic field generation in PMS stars with and without radiative core
dc.typeArtigo de periódico
local.citation.epage37
local.citation.issue328
local.citation.spage30
local.citation.volume12
local.description.resumoRecent observations of the magnetic field in pre-main sequence stars suggest that the magnetic field topology changes as a function of age. The presence of a tachocline could be an important factor in the development of magnetic field with higher multipolar modes. In this work we performed MHD simulations using the EULAG-MHD code to study the magnetic field generation and evolution in models that mimic stars at two evolutionary stages. The stratification for both stellar phases was computed by fitting stellar structure profiles obtained with the ATON stellar evolution code. The first stage is at 1.1Myr, when the star is completely convective. The second stage is at 14Myrs, when the star is partly convective, with a radiative core developed up to 30% of the stellar radius. In this proceedings we present a preliminary analysis of the resulting mean-flows and magnetic field. The mean-flow analysis shown that the star rotate almost rigidly on the fully convective phase, whereas at the partially convective phase there is differential rotation with conical contours of iso-rotation. As for the mean magnetic field both simulations show similarities with respect to the field evolution. However, the topology of the magnetic field is different.
local.identifier.orcidhttps://orcid.org/0000-0002-9328-9530
local.identifier.orcidhttps://orcid.org/0000-0002-2671-8796
local.identifier.orcidhttps://orcid.org/0000-0003-0364-4883
local.identifier.orcidhttps://orcid.org/0000-0001-7077-3285
local.identifier.orcidhttps://orcid.org/0000-0002-2045-8401
local.publisher.countryBrasil
local.publisher.departmentICX - DEPARTAMENTO DE FÍSICA
local.publisher.initialsUFMG
local.url.externahttps://www.cambridge.org/core/journals/proceedings-of-the-international-astronomical-union/article/magnetic-field-generation-in-pms-stars-with-and-without-radiative-core/DB18793F7209FC40487F89B18B4EF218

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