Star-disk interactions in the strongly accreting T Tauri star S CrA N
Context. Classical T Tauri stars are thought to accrete material from their surrounding protoplanetary disks through funnel flows along their magnetic field lines. The classical T Tauri stars with high accretion rates (∼10−7 M⊙ yr−1) are ideal targets for testing this magnetospheric accretion scenar...
| Autores: | , , , , , , , , , , , , , |
|---|---|
| Tipo de recurso: | artículo |
| Estado: | Versión publicada |
| Fecha de publicación: | 2023 |
| País: | Brasil |
| Institución: | Universidade Federal de Minas Gerais (UFMG) |
| Repositorio: | Repositório Institucional da UFMG |
| Idioma: | inglés |
| OAI Identifier: | oai:repositorio.ufmg.br:1843/79457 |
| Acceso en línea: | https://doi.org/10.1051/0004-6361/202347145 http://hdl.handle.net/1843/79457 https://orcid.org/0000-0002-5762-0249 https://orcid.org/0000-0001-5260-7179 https://orcid.org/0000-0003-3099-757X https://orcid.org/0000-0002-9328-9530 https://orcid.org/0000-0002-9023-7890 https://orcid.org/0000-0002-9628-2959 https://orcid.org/0000-0002-7450-6712 https://orcid.org/0000-0001-7633-7038 https://orcid.org/0000-0001-7788-3727 https://orcid.org/0000-0001-7397-8972 https://orcid.org/0000-0001-6660-936X https://orcid.org/0000-0003-3547-3783 https://orcid.org/0000-0002-0493-4674 |
| Access Level: | acceso abierto |
| Palabra clave: | Stars: variables: T Tauri Stars: individual: S CrA N Herbig Ae/Be Stars: magnetic field Techniques: spectroscopic Techniques: polarimetric Accretion Accretion disks Estrelas - Campos magnéticos Estrelas T Tauri Astronomia |
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oai:repositorio.ufmg.br:1843/79457 |
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BR |
| network_name_str |
Brasil |
| repository_id_str |
|
| dc.title.none.fl_str_mv |
Star-disk interactions in the strongly accreting T Tauri star S CrA N |
| title |
Star-disk interactions in the strongly accreting T Tauri star S CrA N |
| spellingShingle |
Star-disk interactions in the strongly accreting T Tauri star S CrA N Hugo Nowacki Stars: variables: T Tauri Stars: individual: S CrA N Herbig Ae/Be Stars: magnetic field Techniques: spectroscopic Techniques: polarimetric Accretion Accretion disks Estrelas - Campos magnéticos Estrelas T Tauri Astronomia |
| title_short |
Star-disk interactions in the strongly accreting T Tauri star S CrA N |
| title_full |
Star-disk interactions in the strongly accreting T Tauri star S CrA N |
| title_fullStr |
Star-disk interactions in the strongly accreting T Tauri star S CrA N |
| title_full_unstemmed |
Star-disk interactions in the strongly accreting T Tauri star S CrA N |
| title_sort |
Star-disk interactions in the strongly accreting T Tauri star S CrA N |
| dc.creator.none.fl_str_mv |
Hugo Nowacki Evelyne Alecian Karine Perraut Bonnie Zaire Colin Folsom Kim Pouilly Jerome Bouvier Rajeev Manick George Pantolmos Alana Sousa Catherine Dougados Jerome Bouvier Gaitee Hussain Silvia Helena Paixao Alencar Jean-Baptiste Le Bouquin |
| author |
Hugo Nowacki |
| author_facet |
Hugo Nowacki Evelyne Alecian Karine Perraut Bonnie Zaire Colin Folsom Kim Pouilly Jerome Bouvier Rajeev Manick George Pantolmos Alana Sousa Catherine Dougados Gaitee Hussain Silvia Helena Paixao Alencar Jean-Baptiste Le Bouquin |
| author_role |
author |
| author2 |
Evelyne Alecian Karine Perraut Bonnie Zaire Colin Folsom Kim Pouilly Jerome Bouvier Rajeev Manick George Pantolmos Alana Sousa Catherine Dougados Gaitee Hussain Silvia Helena Paixao Alencar Jean-Baptiste Le Bouquin |
| author2_role |
author author author author author author author author author author author author author |
| dc.subject.por.fl_str_mv |
Stars: variables: T Tauri Stars: individual: S CrA N Herbig Ae/Be Stars: magnetic field Techniques: spectroscopic Techniques: polarimetric Accretion Accretion disks Estrelas - Campos magnéticos Estrelas T Tauri Astronomia |
| topic |
Stars: variables: T Tauri Stars: individual: S CrA N Herbig Ae/Be Stars: magnetic field Techniques: spectroscopic Techniques: polarimetric Accretion Accretion disks Estrelas - Campos magnéticos Estrelas T Tauri Astronomia |
| description |
Context. Classical T Tauri stars are thought to accrete material from their surrounding protoplanetary disks through funnel flows along their magnetic field lines. The classical T Tauri stars with high accretion rates (∼10−7 M⊙ yr−1) are ideal targets for testing this magnetospheric accretion scenario in a sustained regime. Aims. We constrained the accretion-ejection phenomena around the strongly accreting northern component of the S CrA young binary system (S CrA N) by deriving its magnetic field topology and its magnetospheric properties, and by detecting ejection signatures, if any. Methods. We led a two-week observing campaign on S CrA N with the ESPaDOnS optical spectropolarimeter at the Canada-France-Hawaii Telescope. We recorded 12 Stokes I and V spectra over 14 nights. We computed the corresponding least-squares deconvolution (LSD) profiles of the photospheric lines and performed Zeeman-Doppler imaging (ZDI). We analyzed the kinematics of noticeable emission lines, namely He I λ5876 and the first four lines of the Balmer series, which are known to trace the accretion process. Results. We found that S CrA N is a low-mass (0.8 M⊙) young (∼1 Myr) and fully convective object exhibiting strong and variable veiling (with a mean value of 7 ± 2), which suggests that the star is in a strong accretion regime. These findings could indicate a stellar evolutionary stage between Class I and Class II for S CrA N. We reconstructed an axisymmetric large-scale magnetic field (∼70% of the total energy) that is primarily located in the dipolar component, but has significant higher poloidal orders. From the narrow emission component radial velocity curve of He I λ5876, we derived a stellar rotation period of P* = 7.3 ± 0.2 days. We found a magnetic truncation radius of ∼2 R* which is significantly closer to the star than the corotation radius of ∼6 R*, suggesting that S CrA N is in an unstable accretion regime. That the truncation radius is quite smaller than the size of the Brγ line emitting region, as measured with the GRAVITY interferometer (∼8 R*), supports the presence of outflows, which is nicely corroborated by the line profiles presented in this work. Conclusions. The findings from spectropolarimetry are complementary to those provided by optical long-baseline interferometry, allowing us to construct a coherent view of the innermost regions of a young, strongly accreting star. The strong and complex magnetic field reconstructed for S CrA N is inconsistent with the observed magnetic signatures of the emission lines associated with the postshock region, however. We recommend a multitechnique synchronized campaign of several days to place more constrains on a system that varies on a timescale of about one day. |
| publishDate |
2023 |
| dc.date.none.fl_str_mv |
2023-10-10 2025-01-23T23:56:34Z 2025-01-23T23:56:34Z |
| 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 |
https://doi.org/10.1051/0004-6361/202347145 0004-6361 http://hdl.handle.net/1843/79457 https://orcid.org/0000-0002-5762-0249 https://orcid.org/0000-0001-5260-7179 https://orcid.org/0000-0003-3099-757X https://orcid.org/0000-0002-9328-9530 https://orcid.org/0000-0002-9023-7890 https://orcid.org/0000-0002-9023-7890 https://orcid.org/0000-0002-9628-2959 https://orcid.org/0000-0002-7450-6712 https://orcid.org/0000-0001-7633-7038 https://orcid.org/0000-0001-7788-3727 https://orcid.org/0000-0001-7397-8972 https://orcid.org/0000-0001-6660-936X https://orcid.org/0000-0003-3547-3783 https://orcid.org/0000-0002-0493-4674 |
| url |
https://doi.org/10.1051/0004-6361/202347145 http://hdl.handle.net/1843/79457 https://orcid.org/0000-0002-5762-0249 https://orcid.org/0000-0001-5260-7179 https://orcid.org/0000-0003-3099-757X https://orcid.org/0000-0002-9328-9530 https://orcid.org/0000-0002-9023-7890 https://orcid.org/0000-0002-9628-2959 https://orcid.org/0000-0002-7450-6712 https://orcid.org/0000-0001-7633-7038 https://orcid.org/0000-0001-7788-3727 https://orcid.org/0000-0001-7397-8972 https://orcid.org/0000-0001-6660-936X https://orcid.org/0000-0003-3547-3783 https://orcid.org/0000-0002-0493-4674 |
| identifier_str_mv |
0004-6361 |
| dc.language.iso.fl_str_mv |
eng |
| language |
eng |
| dc.relation.none.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 |
pdf application/pdf |
| dc.publisher.none.fl_str_mv |
Universidade Federal de Minas Gerais Brasil ICX - DEPARTAMENTO DE FÍSICA UFMG |
| publisher.none.fl_str_mv |
Universidade Federal de Minas Gerais Brasil ICX - DEPARTAMENTO DE FÍSICA UFMG |
| 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 |
| repository.name.fl_str_mv |
Repositório Institucional da UFMG - Universidade Federal de Minas Gerais (UFMG) |
| repository.mail.fl_str_mv |
repositorio@ufmg.br |
| _version_ |
1853663266966863872 |
| spelling |
Star-disk interactions in the strongly accreting T Tauri star S CrA NStars: variables: T TauriStars: individual: S CrA NHerbig Ae/BeStars: magnetic fieldTechniques: spectroscopicTechniques: polarimetricAccretionAccretion disksEstrelas - Campos magnéticosEstrelas T TauriAstronomiaContext. Classical T Tauri stars are thought to accrete material from their surrounding protoplanetary disks through funnel flows along their magnetic field lines. The classical T Tauri stars with high accretion rates (∼10−7 M⊙ yr−1) are ideal targets for testing this magnetospheric accretion scenario in a sustained regime. Aims. We constrained the accretion-ejection phenomena around the strongly accreting northern component of the S CrA young binary system (S CrA N) by deriving its magnetic field topology and its magnetospheric properties, and by detecting ejection signatures, if any. Methods. We led a two-week observing campaign on S CrA N with the ESPaDOnS optical spectropolarimeter at the Canada-France-Hawaii Telescope. We recorded 12 Stokes I and V spectra over 14 nights. We computed the corresponding least-squares deconvolution (LSD) profiles of the photospheric lines and performed Zeeman-Doppler imaging (ZDI). We analyzed the kinematics of noticeable emission lines, namely He I λ5876 and the first four lines of the Balmer series, which are known to trace the accretion process. Results. We found that S CrA N is a low-mass (0.8 M⊙) young (∼1 Myr) and fully convective object exhibiting strong and variable veiling (with a mean value of 7 ± 2), which suggests that the star is in a strong accretion regime. These findings could indicate a stellar evolutionary stage between Class I and Class II for S CrA N. We reconstructed an axisymmetric large-scale magnetic field (∼70% of the total energy) that is primarily located in the dipolar component, but has significant higher poloidal orders. From the narrow emission component radial velocity curve of He I λ5876, we derived a stellar rotation period of P* = 7.3 ± 0.2 days. We found a magnetic truncation radius of ∼2 R* which is significantly closer to the star than the corotation radius of ∼6 R*, suggesting that S CrA N is in an unstable accretion regime. That the truncation radius is quite smaller than the size of the Brγ line emitting region, as measured with the GRAVITY interferometer (∼8 R*), supports the presence of outflows, which is nicely corroborated by the line profiles presented in this work. Conclusions. The findings from spectropolarimetry are complementary to those provided by optical long-baseline interferometry, allowing us to construct a coherent view of the innermost regions of a young, strongly accreting star. The strong and complex magnetic field reconstructed for S CrA N is inconsistent with the observed magnetic signatures of the emission lines associated with the postshock region, however. We recommend a multitechnique synchronized campaign of several days to place more constrains on a system that varies on a timescale of about one day.Universidade Federal de Minas GeraisBrasilICX - DEPARTAMENTO DE FÍSICAUFMG2025-01-23T23:56:34Z2025-01-23T23:56:34Z2023-10-10info:eu-repo/semantics/publishedVersioninfo:eu-repo/semantics/articlepdfapplication/pdfhttps://doi.org/10.1051/0004-6361/2023471450004-6361http://hdl.handle.net/1843/79457https://orcid.org/0000-0002-5762-0249https://orcid.org/0000-0001-5260-7179https://orcid.org/0000-0003-3099-757Xhttps://orcid.org/0000-0002-9328-9530https://orcid.org/0000-0002-9023-7890https://orcid.org/0000-0002-9023-7890https://orcid.org/0000-0002-9628-2959https://orcid.org/0000-0002-7450-6712https://orcid.org/0000-0001-7633-7038https://orcid.org/0000-0001-7788-3727https://orcid.org/0000-0001-7397-8972https://orcid.org/0000-0001-6660-936Xhttps://orcid.org/0000-0003-3547-3783https://orcid.org/0000-0002-0493-4674engAstronomy & astrophysicsinfo:eu-repo/semantics/openAccessreponame:Repositório Institucional da UFMGinstname:Universidade Federal de Minas Gerais (UFMG)instacron:UFMGHugo NowackiEvelyne AlecianKarine PerrautBonnie ZaireColin FolsomKim PouillyJerome BouvierRajeev ManickGeorge PantolmosAlana SousaCatherine DougadosJerome BouvierGaitee HussainSilvia Helena Paixao AlencarJean-Baptiste Le Bouquin2025-01-23T23:56:35Zoai:repositorio.ufmg.br:1843/79457Repositório InstitucionalPUBhttps://repositorio.ufmg.br/oairepositorio@ufmg.bropendoar:2025-01-23T23:56:35Repositório Institucional da UFMG - Universidade Federal de Minas Gerais (UFMG)false |
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15,228081 |