Magnetospheric accretion in the intermediate-mass T Tauri star HQ Tauri
Autor(a) principal: | |
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Data de Publicação: | 2020 |
Outros Autores: | , , , , , , , , |
Tipo de documento: | Artigo |
Idioma: | eng |
Título da fonte: | Repositório Institucional da UFMG |
Texto Completo: | https://doi.org/10.1051/0004-6361/202038086 http://hdl.handle.net/1843/56463 https://orcid.org/0000-0002-9628-2959 https://orcid.org/0000-0002-7450-6712 https://orcid.org/0000-0001-5260-7179 https://orcid.org/0000-0002-5171-8376 https://orcid.org/0000-0001-5541-2887 https://orcid.org/0000-0001-5707-8448 https://orcid.org/0000-0003-3547-3783 https://orcid.org/0000-0001-6381-515X https://orcid.org/0000-0002-9023-7890 |
Resumo: | Context: Classical T Tauri stars are pre-main sequence stars surrounded by an accretion disk. They host a strong magnetic field, and both magnetospheric accretion and ejection processes develop as the young magnetic star interacts with its disk. Studying this interaction is a major goal toward understanding the properties of young stars and their evolution. Aims: The goal of this study is to investigate the accretion process in the young stellar system HQ Tau, an intermediate-mass T Tauri star (1.9 M ). Methods: The time variability of the system is investigated both photometrically, using Kepler-K2 and complementary light curves, and from a high-resolution spectropolarimetric time series obtained with ESPaDOnS at CFHT. Results: The quasi-sinusoidal Kepler-K2 light curve exhibits a period of 2.424 d, which we ascribe to the rotational period of the star. The radial velocity of the system shows the same periodicity, as expected from the modulation of the photospheric line profiles by surface spots. A similar period is found in the red wing of several emission lines (e.g., HI, CaII, NaI), due to the appearance of inverse P Cygni components, indicative of accretion funnel flows. Signatures of outflows are also seen in the line profiles, some being periodic, others transient. The polarimetric analysis indicates a complex, moderately strong magnetic field which is possibly sufficient to truncate the inner disk close to the corotation radius, rcor ∼ 3.5 R. Additionally, we report HQ Tau to be a spectroscopic binary candidate whose orbit remains to be determined. Conclusions: The results of this study expand upon those previously reported for low-mass T Tauri stars, as they indicate that the magnetospheric accretion process may still operate in intermediate-mass pre-main sequence stars, such as HQ Tauri. |
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2023-07-17T19:12:40Z2023-07-17T19:12:40Z2020-10-08642https://doi.org/10.1051/0004-6361/2020380861432-0746http://hdl.handle.net/1843/56463https://orcid.org/0000-0002-9628-2959https://orcid.org/0000-0002-7450-6712https://orcid.org/0000-0001-5260-7179https://orcid.org/0000-0002-5171-8376https://orcid.org/0000-0001-5541-2887https://orcid.org/0000-0001-5707-8448https://orcid.org/0000-0003-3547-3783https://orcid.org/0000-0001-6381-515Xhttps://orcid.org/0000-0002-9023-7890Context: Classical T Tauri stars are pre-main sequence stars surrounded by an accretion disk. They host a strong magnetic field, and both magnetospheric accretion and ejection processes develop as the young magnetic star interacts with its disk. Studying this interaction is a major goal toward understanding the properties of young stars and their evolution. Aims: The goal of this study is to investigate the accretion process in the young stellar system HQ Tau, an intermediate-mass T Tauri star (1.9 M ). Methods: The time variability of the system is investigated both photometrically, using Kepler-K2 and complementary light curves, and from a high-resolution spectropolarimetric time series obtained with ESPaDOnS at CFHT. Results: The quasi-sinusoidal Kepler-K2 light curve exhibits a period of 2.424 d, which we ascribe to the rotational period of the star. The radial velocity of the system shows the same periodicity, as expected from the modulation of the photospheric line profiles by surface spots. A similar period is found in the red wing of several emission lines (e.g., HI, CaII, NaI), due to the appearance of inverse P Cygni components, indicative of accretion funnel flows. Signatures of outflows are also seen in the line profiles, some being periodic, others transient. The polarimetric analysis indicates a complex, moderately strong magnetic field which is possibly sufficient to truncate the inner disk close to the corotation radius, rcor ∼ 3.5 R. Additionally, we report HQ Tau to be a spectroscopic binary candidate whose orbit remains to be determined. Conclusions: The results of this study expand upon those previously reported for low-mass T Tauri stars, as they indicate that the magnetospheric accretion process may still operate in intermediate-mass pre-main sequence stars, such as HQ Tauri.Contexto: As estrelas T Tauri clássicas são estrelas pré-sequência principal rodeadas por um disco de acreção. Eles hospedam um forte campo magnético, e ambos os processos de acreção e ejeção magnetosférica se desenvolvem à medida que a jovem estrela magnética interage com seu disco. estudando isso interação é um objetivo importante para a compreensão das propriedades de estrelas jovens e sua evolução. Objetivos: O objetivo deste estudo é investigar o processo de acreção no sistema estelar jovem HQ Tau, uma estrela T Tauri de massa intermediária (1,9 M ). Métodos: A variabilidade temporal do sistema é investigada fotometricamente, usando Kepler-K2 e curvas de luz complementares, e a partir de séries temporais espectropolarimétricas de alta resolução obtidas com ESPaDOnS em CFHT. Resultados: A curva de luz quase senoidal do Kepler-K2 exibe um período de 2,424 d, que atribuímos ao período de rotação da estrela. A velocidade radial do sistema apresenta a mesma periodicidade, como esperado pela modulação dos perfis das linhas fotosféricas por manchas de superfície. Um período semelhante é encontrado na asa vermelha de várias linhas de emissão (por exemplo, HI, CaII, NaI), devido ao aparecimento de componentes inversos P Cygni, indicativos de fluxos de funil de acreção. Assinaturas de vazões também são vistas nos perfis das linhas, algumas periódicas, outras transitórias. A análise polarimétrica indica um campo magnético complexo e moderadamente forte que possivelmente é suficiente para truncar o disco interno próximo ao raio de corrotação, rcor ∼ 3,5 R. Além disso, relatamos que HQ Tau é um candidato binário espectroscópico cuja órbita ainda precisa ser determinada. Conclusões: Os resultados deste estudo expandem aqueles relatados anteriormente para estrelas T Tauri de baixa massa, pois indicam que o processo de acreção magnetosférica ainda pode operar em estrelas pré-sequência principal de massa intermediária, como HQ Tauri.CNPq - Conselho Nacional de Desenvolvimento Científico e TecnológicoFAPEMIG - Fundação de Amparo à Pesquisa do Estado de Minas GeraisCAPES - Coordenação de Aperfeiçoamento de Pessoal de Nível SuperiorOutra AgênciaengUniversidade Federal de Minas GeraisUFMGBrasilICX - DEPARTAMENTO DE FÍSICAAstronomy & AstrophysicsAstrofísicaAcreção - AstrofísicaEstrelas - FormaçãoEstrelas - MassasEstrelas variáveisEstrelas - Campos magnéticosFotometria astronômicaStarsVariablesT Tauri, Herbig Ae/Be – starsPre-main sequence – accretionAccretion disks – starsMagnetic field – starsIndividualHQ Tau – starspotsMagnetospheric accretion in the intermediate-mass T Tauri star HQ TauriAcreção magnetosférica na estrela T Tauri de massa intermediária HQ Tauriinfo:eu-repo/semantics/publishedVersioninfo:eu-repo/semantics/articlehttps://www.aanda.org/articles/aa/full_html/2020/10/aa38086-20/aa38086-20.htmlKim PouillyJerome BouvierEvelyne AlecianSilvia Helena Paixão AlencarAnn Marie CodyJean-Francois DonatiKonstantin GrankinGaitee A. J. HussainLuisa M. RebullColin Peter Folsomapplication/pdfinfo:eu-repo/semantics/openAccessreponame:Repositório Institucional da UFMGinstname:Universidade Federal de Minas Gerais (UFMG)instacron:UFMGLICENSELicense.txtLicense.txttext/plain; charset=utf-82042https://repositorio.ufmg.br/bitstream/1843/56463/1/License.txtfa505098d172de0bc8864fc1287ffe22MD51ORIGINALMagnetospheric accretion in the intermediate-mass T Tauri star HQ Tauri.pdfMagnetospheric accretion in the intermediate-mass T Tauri star HQ Tauri.pdfapplication/pdf2105559https://repositorio.ufmg.br/bitstream/1843/56463/2/Magnetospheric%20accretion%20in%20the%20intermediate-mass%20T%20Tauri%20star%20HQ%20Tauri.pdfc6dcfe59a9fcefa1031214ec993590e2MD521843/564632023-07-17 16:12:40.21oai:repositorio.ufmg.br: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Repositório de PublicaçõesPUBhttps://repositorio.ufmg.br/oaiopendoar:2023-07-17T19:12:40Repositório Institucional da UFMG - Universidade Federal de Minas Gerais (UFMG)false |
dc.title.pt_BR.fl_str_mv |
Magnetospheric accretion in the intermediate-mass T Tauri star HQ Tauri |
dc.title.alternative.pt_BR.fl_str_mv |
Acreção magnetosférica na estrela T Tauri de massa intermediária HQ Tauri |
title |
Magnetospheric accretion in the intermediate-mass T Tauri star HQ Tauri |
spellingShingle |
Magnetospheric accretion in the intermediate-mass T Tauri star HQ Tauri Kim Pouilly Stars Variables T Tauri, Herbig Ae/Be – stars Pre-main sequence – accretion Accretion disks – stars Magnetic field – stars Individual HQ Tau – starspots Astrofísica Acreção - Astrofísica Estrelas - Formação Estrelas - Massas Estrelas variáveis Estrelas - Campos magnéticos Fotometria astronômica |
title_short |
Magnetospheric accretion in the intermediate-mass T Tauri star HQ Tauri |
title_full |
Magnetospheric accretion in the intermediate-mass T Tauri star HQ Tauri |
title_fullStr |
Magnetospheric accretion in the intermediate-mass T Tauri star HQ Tauri |
title_full_unstemmed |
Magnetospheric accretion in the intermediate-mass T Tauri star HQ Tauri |
title_sort |
Magnetospheric accretion in the intermediate-mass T Tauri star HQ Tauri |
author |
Kim Pouilly |
author_facet |
Kim Pouilly Jerome Bouvier Evelyne Alecian Silvia Helena Paixão Alencar Ann Marie Cody Jean-Francois Donati Konstantin Grankin Gaitee A. J. Hussain Luisa M. Rebull Colin Peter Folsom |
author_role |
author |
author2 |
Jerome Bouvier Evelyne Alecian Silvia Helena Paixão Alencar Ann Marie Cody Jean-Francois Donati Konstantin Grankin Gaitee A. J. Hussain Luisa M. Rebull Colin Peter Folsom |
author2_role |
author author author author author author author author author |
dc.contributor.author.fl_str_mv |
Kim Pouilly Jerome Bouvier Evelyne Alecian Silvia Helena Paixão Alencar Ann Marie Cody Jean-Francois Donati Konstantin Grankin Gaitee A. J. Hussain Luisa M. Rebull Colin Peter Folsom |
dc.subject.por.fl_str_mv |
Stars Variables T Tauri, Herbig Ae/Be – stars Pre-main sequence – accretion Accretion disks – stars Magnetic field – stars Individual HQ Tau – starspots |
topic |
Stars Variables T Tauri, Herbig Ae/Be – stars Pre-main sequence – accretion Accretion disks – stars Magnetic field – stars Individual HQ Tau – starspots Astrofísica Acreção - Astrofísica Estrelas - Formação Estrelas - Massas Estrelas variáveis Estrelas - Campos magnéticos Fotometria astronômica |
dc.subject.other.pt_BR.fl_str_mv |
Astrofísica Acreção - Astrofísica Estrelas - Formação Estrelas - Massas Estrelas variáveis Estrelas - Campos magnéticos Fotometria astronômica |
description |
Context: Classical T Tauri stars are pre-main sequence stars surrounded by an accretion disk. They host a strong magnetic field, and both magnetospheric accretion and ejection processes develop as the young magnetic star interacts with its disk. Studying this interaction is a major goal toward understanding the properties of young stars and their evolution. Aims: The goal of this study is to investigate the accretion process in the young stellar system HQ Tau, an intermediate-mass T Tauri star (1.9 M ). Methods: The time variability of the system is investigated both photometrically, using Kepler-K2 and complementary light curves, and from a high-resolution spectropolarimetric time series obtained with ESPaDOnS at CFHT. Results: The quasi-sinusoidal Kepler-K2 light curve exhibits a period of 2.424 d, which we ascribe to the rotational period of the star. The radial velocity of the system shows the same periodicity, as expected from the modulation of the photospheric line profiles by surface spots. A similar period is found in the red wing of several emission lines (e.g., HI, CaII, NaI), due to the appearance of inverse P Cygni components, indicative of accretion funnel flows. Signatures of outflows are also seen in the line profiles, some being periodic, others transient. The polarimetric analysis indicates a complex, moderately strong magnetic field which is possibly sufficient to truncate the inner disk close to the corotation radius, rcor ∼ 3.5 R. Additionally, we report HQ Tau to be a spectroscopic binary candidate whose orbit remains to be determined. Conclusions: The results of this study expand upon those previously reported for low-mass T Tauri stars, as they indicate that the magnetospheric accretion process may still operate in intermediate-mass pre-main sequence stars, such as HQ Tauri. |
publishDate |
2020 |
dc.date.issued.fl_str_mv |
2020-10-08 |
dc.date.accessioned.fl_str_mv |
2023-07-17T19:12:40Z |
dc.date.available.fl_str_mv |
2023-07-17T19:12:40Z |
dc.type.status.fl_str_mv |
info:eu-repo/semantics/publishedVersion |
dc.type.driver.fl_str_mv |
info:eu-repo/semantics/article |
format |
article |
status_str |
publishedVersion |
dc.identifier.uri.fl_str_mv |
http://hdl.handle.net/1843/56463 |
dc.identifier.doi.pt_BR.fl_str_mv |
https://doi.org/10.1051/0004-6361/202038086 |
dc.identifier.issn.pt_BR.fl_str_mv |
1432-0746 |
dc.identifier.orcid.pt_BR.fl_str_mv |
https://orcid.org/0000-0002-9628-2959 https://orcid.org/0000-0002-7450-6712 https://orcid.org/0000-0001-5260-7179 https://orcid.org/0000-0002-5171-8376 https://orcid.org/0000-0001-5541-2887 https://orcid.org/0000-0001-5707-8448 https://orcid.org/0000-0003-3547-3783 https://orcid.org/0000-0001-6381-515X https://orcid.org/0000-0002-9023-7890 |
url |
https://doi.org/10.1051/0004-6361/202038086 http://hdl.handle.net/1843/56463 https://orcid.org/0000-0002-9628-2959 https://orcid.org/0000-0002-7450-6712 https://orcid.org/0000-0001-5260-7179 https://orcid.org/0000-0002-5171-8376 https://orcid.org/0000-0001-5541-2887 https://orcid.org/0000-0001-5707-8448 https://orcid.org/0000-0003-3547-3783 https://orcid.org/0000-0001-6381-515X https://orcid.org/0000-0002-9023-7890 |
identifier_str_mv |
1432-0746 |
dc.language.iso.fl_str_mv |
eng |
language |
eng |
dc.relation.ispartof.pt_BR.fl_str_mv |
Astronomy & Astrophysics |
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info:eu-repo/semantics/openAccess |
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openAccess |
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application/pdf |
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Universidade Federal de Minas Gerais |
dc.publisher.initials.fl_str_mv |
UFMG |
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Brasil |
dc.publisher.department.fl_str_mv |
ICX - DEPARTAMENTO DE FÍSICA |
publisher.none.fl_str_mv |
Universidade Federal de Minas Gerais |
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