Investigating the magnetospheric accretion process in the young pre-transitional disk system DoAr 44 (V2062 Oph): a multiwavelength interferometric, spectropolarimetric, and photometric observing campaign
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/10.1051/0004-6361/202038892 http://hdl.handle.net/1843/56464 https://orcid.org/0000-0002-7450-6712 https://orcid.org/0000-0001-5260-7179 https://orcid.org/0000-0002-5171-8376 https://orcid.org/0000-0001-7397-8972 https://orcid.org/0000-0001-5541-2887 https://orcid.org/0000-0003-3099-757X https://orcid.org/0000-0001-7868-7031 https://orcid.org/0000-0001-6381-515X https://orcid.org/0000-0001-6660-936X https://orcid.org/0000-0001-8769-3660 https://orcid.org/0000-0001-5025-0428 https://orcid.org/0000-0002-7695-7605 https://orcid.org/0000-0002-9628-2959 |
Resumo: | Context: Young stars interact with their accretion disk through their strong magnetosphere. Aims: We aim to investigate the magnetospheric accretion/ejection process in the young stellar system DoAr 44 (V2062 Oph). Methods: We monitored the system over several rotational cycles, combining high-resolution spectropolarimetry at both optical and near-IR wavelengths with long-baseline near-IR inteferometry and multicolor photometry. Results: We derive a rotational period of 2.96 d from the system’s light curve, which is dominated by stellar spots. We fully characterize the central star’s properties from the high signal-to-noise, high-resolution optical spectra we obtained during the campaign. DoAr 44 is a young 1.2 M star, moderately accreting from its disk (M˙acc = 6.5 10−9 M yr−1), and seen at a low inclination (i ' 30◦). Several optical and near-IR line profiles probing the accretion funnel flows (Hα, Hβ, HeI 1083 nm, Paβ) and the accretion shock (HeI 587.6 nm) are modulated at the stellar rotation period. The most variable line profile is HeI 1083 nm, which exhibits modulated redshifted wings that are a signature of accretion funnel flows, as well as deep blueshifted absorptions indicative of transient outflows. The Zeeman-Doppler analysis suggests the star hosts a mainly dipolar magnetic field, inclined by about 20◦ onto the spin axis, with an intensity reaching about 800 G at the photosphere, and up to 2 ± 0.8 kG close to the accretion shock. The magnetic field appears strong enough to disrupt the inner disk close to the corotation radius, at a distance of about 4.6 R? (0.043 au), which is consistent with the 5 R? (0.047 au) upper limit we derived for the size of the magnetosphere in our Paper I from long baseline interferometry. Conclusions: DoAr 44 is a pre-transitional disk system, exhibiting a 25–30 au gap in its circumstellar disk, with the inner and outer disks being misaligned. On a scale of 0.1 au or less, our results indicate that the system is steadily accreting from its inner disk through its tilted dipolar magnetosphere. We conclude that in spite of a highly structured disk on the large scale, perhaps the signature of ongoing planetary formation, the magnetospheric accretion process proceeds unimpeded at the star-disk interaction level. |
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2023-07-17T19:13:18Z2023-07-17T19:13:18Z2020-11-09643https://doi.org/10.1051/0004-6361/2020388921432-0746http://hdl.handle.net/1843/56464https://orcid.org/0000-0002-7450-6712https://orcid.org/0000-0001-5260-7179https://orcid.org/0000-0002-5171-8376https://orcid.org/0000-0001-7397-8972https://orcid.org/0000-0001-5541-2887https://orcid.org/0000-0003-3099-757Xhttps://orcid.org/0000-0001-7868-7031https://orcid.org/0000-0001-6381-515Xhttps://orcid.org/0000-0001-6660-936Xhttps://orcid.org/0000-0001-8769-3660https://orcid.org/0000-0001-5025-0428https://orcid.org/0000-0002-7695-7605https://orcid.org/0000-0002-9628-2959Context: Young stars interact with their accretion disk through their strong magnetosphere. Aims: We aim to investigate the magnetospheric accretion/ejection process in the young stellar system DoAr 44 (V2062 Oph). Methods: We monitored the system over several rotational cycles, combining high-resolution spectropolarimetry at both optical and near-IR wavelengths with long-baseline near-IR inteferometry and multicolor photometry. Results: We derive a rotational period of 2.96 d from the system’s light curve, which is dominated by stellar spots. We fully characterize the central star’s properties from the high signal-to-noise, high-resolution optical spectra we obtained during the campaign. DoAr 44 is a young 1.2 M star, moderately accreting from its disk (M˙acc = 6.5 10−9 M yr−1), and seen at a low inclination (i ' 30◦). Several optical and near-IR line profiles probing the accretion funnel flows (Hα, Hβ, HeI 1083 nm, Paβ) and the accretion shock (HeI 587.6 nm) are modulated at the stellar rotation period. The most variable line profile is HeI 1083 nm, which exhibits modulated redshifted wings that are a signature of accretion funnel flows, as well as deep blueshifted absorptions indicative of transient outflows. The Zeeman-Doppler analysis suggests the star hosts a mainly dipolar magnetic field, inclined by about 20◦ onto the spin axis, with an intensity reaching about 800 G at the photosphere, and up to 2 ± 0.8 kG close to the accretion shock. The magnetic field appears strong enough to disrupt the inner disk close to the corotation radius, at a distance of about 4.6 R? (0.043 au), which is consistent with the 5 R? (0.047 au) upper limit we derived for the size of the magnetosphere in our Paper I from long baseline interferometry. Conclusions: DoAr 44 is a pre-transitional disk system, exhibiting a 25–30 au gap in its circumstellar disk, with the inner and outer disks being misaligned. On a scale of 0.1 au or less, our results indicate that the system is steadily accreting from its inner disk through its tilted dipolar magnetosphere. We conclude that in spite of a highly structured disk on the large scale, perhaps the signature of ongoing planetary formation, the magnetospheric accretion process proceeds unimpeded at the star-disk interaction level.Contexto: Estrelas jovens interagem com seu disco de acreção através de sua forte magnetosfera. Objetivos: Pretendemos investigar o processo de acreção/ejeção magnetosférica no sistema estelar jovem DoAr 44 (V2062 Oph). Métodos: Monitoramos o sistema ao longo de vários ciclos rotacionais, combinando espectropolarimetria de alta resolução em comprimentos de onda ópticos e infravermelho próximo com interferometria de infravermelho próximo de linha de base longa e fotometria multicolorida. Resultados: derivamos um período rotacional de 2,96 d da curva de luz do sistema, que é dominada por manchas estelares. Caracterizamos completamente as propriedades da estrela central a partir dos espectros ópticos de alta resolução e alta relação sinal-ruído que obtivemos durante a campanha. DoAr 44 é uma estrela jovem de 1,2 M, moderadamente agregada a partir de seu disco (M˙acc = 6,5 10−9 M ano–1) e vista com baixa inclinação (i ' 30◦). Vários perfis de linhas ópticas e de infravermelho próximo sondando os fluxos do funil de acreção (Hα, Hβ, HeI 1083 nm, Paβ) e o choque de acreção (HeI 587,6 nm) são modulados no período de rotação estelar. O perfil de linha mais variável é HeI 1083 nm, que exibe asas moduladas com desvio para o vermelho que são uma assinatura de fluxos de funil de acreção, bem como absorções profundas com desvio para o azul, indicativas de escoamentos transitórios. A análise Zeeman-Doppler sugere que a estrela hospeda um campo magnético principalmente dipolar, inclinado cerca de 20◦ no eixo de rotação, com uma intensidade atingindo cerca de 800 G na fotosfera, e até 2 ± 0,8 kG perto do choque de acreção. O campo magnético parece forte o suficiente para interromper o disco interno próximo ao raio de corrotação, a uma distância de cerca de 4,6 R? (0,043 au), o que é consistente com o 5 R? (0,047 au) limite superior que derivamos para o tamanho da magnetosfera em nosso Artigo I a partir de interferometria de linha de base longa. Conclusões: DoAr 44 é um sistema de disco pré-transicional, exibindo um gap de 25–30 au em seu disco circunstelar, com os discos interno e externo desalinhados. Em uma escala de 0,1 au ou menos, nossos resultados indicam que o sistema está constantemente acumulando de seu disco interno através de sua magnetosfera dipolar inclinada. Concluímos que, apesar de um disco altamente estruturado em grande escala, talvez a assinatura da formação planetária em andamento, o processo de acreção magnetosférica prossegue sem impedimentos no nível de interação estrela-disco.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 & AstrophysicsAstrofísicaEstrelas - FormaçãoAcreção - AstrofísicaEstrelas - Campos magnéticosFotometria astronômicaStarsPre-main sequence – starsVariablesT Tauri, Herbig Ae/Be – starsMagnetic field – starFormation – accretionAccretion disksInvestigating the magnetospheric accretion process in the young pre-transitional disk system DoAr 44 (V2062 Oph): a multiwavelength interferometric, spectropolarimetric, and photometric observing campaignInvestigando o processo de acreção magnetosférica no jovem sistema de disco pré-transicional DoAr 44 (V2062 Oph): uma campanha de observação interferométrica, espectropolarimétrica e fotométrica de vários comprimentos de ondainfo:eu-repo/semantics/publishedVersioninfo:eu-repo/semantics/articlehttps://www.aanda.org/articles/aa/full_html/2020/11/aa38892-20/aa38892-20.htmlJerome BouvierEvelyne AlecianSilvia Helena Paixão AlencarAlana Paixão de SousaJean-Francois DonatiKarine Rousselet-PerrautAmelia BayoLuisa M. RebullCatherine L. DougadosJean-francois DonatiGilles DuvertJean-Philippe BergerMyriam BenistyKim PouillyClaire Moutouapplication/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/1843/56464/1/License.txtfa505098d172de0bc8864fc1287ffe22MD51ORIGINALInvestigating the magnetospheric accretion process in the young pre-transitional disk system DoAr 44 (V2062 Oph) a multiwavelength interferometric, spectropolarimetric, and photometric observing campaign.pdfInvestigating the magnetospheric accretion process in the young pre-transitional disk system DoAr 44 (V2062 Oph) a multiwavelength interferometric, spectropolarimetric, and photometric observing campaign.pdfapplication/pdf7343395https://repositorio.ufmg.br/bitstream/1843/56464/2/Investigating%20the%20magnetospheric%20accretion%20process%20in%20the%20young%20pre-transitional%20disk%20system%20DoAr%2044%20%28V2062%20Oph%29%20a%20multiwavelength%20interferometric%2c%20spectropolarimetric%2c%20and%20photometric%20observing%20campaign.pdfc68fdc86d9e3504ccb56f96ecfbf7b53MD521843/564642023-07-17 16:13:18.49oai:repositorio.ufmg.br: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Repositório de PublicaçõesPUBhttps://repositorio.ufmg.br/oaiopendoar:2023-07-17T19:13:18Repositório Institucional da UFMG - Universidade Federal de Minas Gerais (UFMG)false |
dc.title.pt_BR.fl_str_mv |
Investigating the magnetospheric accretion process in the young pre-transitional disk system DoAr 44 (V2062 Oph): a multiwavelength interferometric, spectropolarimetric, and photometric observing campaign |
dc.title.alternative.pt_BR.fl_str_mv |
Investigando o processo de acreção magnetosférica no jovem sistema de disco pré-transicional DoAr 44 (V2062 Oph): uma campanha de observação interferométrica, espectropolarimétrica e fotométrica de vários comprimentos de onda |
title |
Investigating the magnetospheric accretion process in the young pre-transitional disk system DoAr 44 (V2062 Oph): a multiwavelength interferometric, spectropolarimetric, and photometric observing campaign |
spellingShingle |
Investigating the magnetospheric accretion process in the young pre-transitional disk system DoAr 44 (V2062 Oph): a multiwavelength interferometric, spectropolarimetric, and photometric observing campaign Jerome Bouvier Stars Pre-main sequence – stars Variables T Tauri, Herbig Ae/Be – stars Magnetic field – star Formation – accretion Accretion disks Astrofísica Estrelas - Formação Acreção - Astrofísica Estrelas - Campos magnéticos Fotometria astronômica |
title_short |
Investigating the magnetospheric accretion process in the young pre-transitional disk system DoAr 44 (V2062 Oph): a multiwavelength interferometric, spectropolarimetric, and photometric observing campaign |
title_full |
Investigating the magnetospheric accretion process in the young pre-transitional disk system DoAr 44 (V2062 Oph): a multiwavelength interferometric, spectropolarimetric, and photometric observing campaign |
title_fullStr |
Investigating the magnetospheric accretion process in the young pre-transitional disk system DoAr 44 (V2062 Oph): a multiwavelength interferometric, spectropolarimetric, and photometric observing campaign |
title_full_unstemmed |
Investigating the magnetospheric accretion process in the young pre-transitional disk system DoAr 44 (V2062 Oph): a multiwavelength interferometric, spectropolarimetric, and photometric observing campaign |
title_sort |
Investigating the magnetospheric accretion process in the young pre-transitional disk system DoAr 44 (V2062 Oph): a multiwavelength interferometric, spectropolarimetric, and photometric observing campaign |
author |
Jerome Bouvier |
author_facet |
Jerome Bouvier Evelyne Alecian Silvia Helena Paixão Alencar Alana Paixão de Sousa Jean-Francois Donati Karine Rousselet-Perraut Amelia Bayo Luisa M. Rebull Catherine L. Dougados Jean-francois Donati Gilles Duvert Jean-Philippe Berger Myriam Benisty Kim Pouilly Claire Moutou |
author_role |
author |
author2 |
Evelyne Alecian Silvia Helena Paixão Alencar Alana Paixão de Sousa Jean-Francois Donati Karine Rousselet-Perraut Amelia Bayo Luisa M. Rebull Catherine L. Dougados Jean-francois Donati Gilles Duvert Jean-Philippe Berger Myriam Benisty Kim Pouilly Claire Moutou |
author2_role |
author author author author author author author author author author author author author author |
dc.contributor.author.fl_str_mv |
Jerome Bouvier Evelyne Alecian Silvia Helena Paixão Alencar Alana Paixão de Sousa Jean-Francois Donati Karine Rousselet-Perraut Amelia Bayo Luisa M. Rebull Catherine L. Dougados Jean-francois Donati Gilles Duvert Jean-Philippe Berger Myriam Benisty Kim Pouilly Claire Moutou |
dc.subject.por.fl_str_mv |
Stars Pre-main sequence – stars Variables T Tauri, Herbig Ae/Be – stars Magnetic field – star Formation – accretion Accretion disks |
topic |
Stars Pre-main sequence – stars Variables T Tauri, Herbig Ae/Be – stars Magnetic field – star Formation – accretion Accretion disks Astrofísica Estrelas - Formação Acreção - Astrofísica Estrelas - Campos magnéticos Fotometria astronômica |
dc.subject.other.pt_BR.fl_str_mv |
Astrofísica Estrelas - Formação Acreção - Astrofísica Estrelas - Campos magnéticos Fotometria astronômica |
description |
Context: Young stars interact with their accretion disk through their strong magnetosphere. Aims: We aim to investigate the magnetospheric accretion/ejection process in the young stellar system DoAr 44 (V2062 Oph). Methods: We monitored the system over several rotational cycles, combining high-resolution spectropolarimetry at both optical and near-IR wavelengths with long-baseline near-IR inteferometry and multicolor photometry. Results: We derive a rotational period of 2.96 d from the system’s light curve, which is dominated by stellar spots. We fully characterize the central star’s properties from the high signal-to-noise, high-resolution optical spectra we obtained during the campaign. DoAr 44 is a young 1.2 M star, moderately accreting from its disk (M˙acc = 6.5 10−9 M yr−1), and seen at a low inclination (i ' 30◦). Several optical and near-IR line profiles probing the accretion funnel flows (Hα, Hβ, HeI 1083 nm, Paβ) and the accretion shock (HeI 587.6 nm) are modulated at the stellar rotation period. The most variable line profile is HeI 1083 nm, which exhibits modulated redshifted wings that are a signature of accretion funnel flows, as well as deep blueshifted absorptions indicative of transient outflows. The Zeeman-Doppler analysis suggests the star hosts a mainly dipolar magnetic field, inclined by about 20◦ onto the spin axis, with an intensity reaching about 800 G at the photosphere, and up to 2 ± 0.8 kG close to the accretion shock. The magnetic field appears strong enough to disrupt the inner disk close to the corotation radius, at a distance of about 4.6 R? (0.043 au), which is consistent with the 5 R? (0.047 au) upper limit we derived for the size of the magnetosphere in our Paper I from long baseline interferometry. Conclusions: DoAr 44 is a pre-transitional disk system, exhibiting a 25–30 au gap in its circumstellar disk, with the inner and outer disks being misaligned. On a scale of 0.1 au or less, our results indicate that the system is steadily accreting from its inner disk through its tilted dipolar magnetosphere. We conclude that in spite of a highly structured disk on the large scale, perhaps the signature of ongoing planetary formation, the magnetospheric accretion process proceeds unimpeded at the star-disk interaction level. |
publishDate |
2020 |
dc.date.issued.fl_str_mv |
2020-11-09 |
dc.date.accessioned.fl_str_mv |
2023-07-17T19:13:18Z |
dc.date.available.fl_str_mv |
2023-07-17T19:13:18Z |
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/1843/56464 |
dc.identifier.doi.pt_BR.fl_str_mv |
https://doi.org/10.1051/0004-6361/202038892 |
dc.identifier.issn.pt_BR.fl_str_mv |
1432-0746 |
dc.identifier.orcid.pt_BR.fl_str_mv |
https://orcid.org/0000-0002-7450-6712 https://orcid.org/0000-0001-5260-7179 https://orcid.org/0000-0002-5171-8376 https://orcid.org/0000-0001-7397-8972 https://orcid.org/0000-0001-5541-2887 https://orcid.org/0000-0003-3099-757X https://orcid.org/0000-0001-7868-7031 https://orcid.org/0000-0001-6381-515X https://orcid.org/0000-0001-6660-936X https://orcid.org/0000-0001-8769-3660 https://orcid.org/0000-0001-5025-0428 https://orcid.org/0000-0002-7695-7605 https://orcid.org/0000-0002-9628-2959 |
url |
https://doi.org/10.1051/0004-6361/202038892 http://hdl.handle.net/1843/56464 https://orcid.org/0000-0002-7450-6712 https://orcid.org/0000-0001-5260-7179 https://orcid.org/0000-0002-5171-8376 https://orcid.org/0000-0001-7397-8972 https://orcid.org/0000-0001-5541-2887 https://orcid.org/0000-0003-3099-757X https://orcid.org/0000-0001-7868-7031 https://orcid.org/0000-0001-6381-515X https://orcid.org/0000-0001-6660-936X https://orcid.org/0000-0001-8769-3660 https://orcid.org/0000-0001-5025-0428 https://orcid.org/0000-0002-7695-7605 https://orcid.org/0000-0002-9628-2959 |
identifier_str_mv |
1432-0746 |
dc.language.iso.fl_str_mv |
eng |
language |
eng |
dc.relation.ispartof.pt_BR.fl_str_mv |
Astronomy & Astrophysics |
dc.rights.driver.fl_str_mv |
info:eu-repo/semantics/openAccess |
eu_rights_str_mv |
openAccess |
dc.format.none.fl_str_mv |
application/pdf |
dc.publisher.none.fl_str_mv |
Universidade Federal de Minas Gerais |
dc.publisher.initials.fl_str_mv |
UFMG |
dc.publisher.country.fl_str_mv |
Brasil |
dc.publisher.department.fl_str_mv |
ICX - DEPARTAMENTO DE FÍSICA |
publisher.none.fl_str_mv |
Universidade Federal de Minas Gerais |
dc.source.none.fl_str_mv |
reponame:Repositório Institucional da UFMG instname:Universidade Federal de Minas Gerais (UFMG) instacron:UFMG |
instname_str |
Universidade Federal de Minas Gerais (UFMG) |
instacron_str |
UFMG |
institution |
UFMG |
reponame_str |
Repositório Institucional da UFMG |
collection |
Repositório Institucional da UFMG |
bitstream.url.fl_str_mv |
https://repositorio.ufmg.br/bitstream/1843/56464/1/License.txt https://repositorio.ufmg.br/bitstream/1843/56464/2/Investigating%20the%20magnetospheric%20accretion%20process%20in%20the%20young%20pre-transitional%20disk%20system%20DoAr%2044%20%28V2062%20Oph%29%20a%20multiwavelength%20interferometric%2c%20spectropolarimetric%2c%20and%20photometric%20observing%20campaign.pdf |
bitstream.checksum.fl_str_mv |
fa505098d172de0bc8864fc1287ffe22 c68fdc86d9e3504ccb56f96ecfbf7b53 |
bitstream.checksumAlgorithm.fl_str_mv |
MD5 MD5 |
repository.name.fl_str_mv |
Repositório Institucional da UFMG - Universidade Federal de Minas Gerais (UFMG) |
repository.mail.fl_str_mv |
|
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1793890718423449600 |