The connection between stellar activity cycles and magnetic field topology
Autor(a) principal: | |
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Data de Publicação: | 2016 |
Outros Autores: | , , , , , , , , , , , , , , , |
Tipo de documento: | Artigo |
Idioma: | por |
Título da fonte: | Repositório Institucional da UFRN |
Texto Completo: | https://repositorio.ufrn.br/jspui/handle/123456789/29046 |
Resumo: | Zeeman–Doppler imaging (ZDI) has successfully mapped the large-scale magnetic fields of stars over a large range of spectral types, rotation periods and ages. When observed over multiple epochs, some stars show polarity reversals in their global magnetic fields. On the Sun, polarity reversals are a feature of its activity cycle. In this paper, we examine the magnetic properties of stars with existing chromospherically determined cycle periods. Previous authors have suggested that cycle periods lie on multiple branches, either in the cycle period–Rossby number plane or the cycle period–rotation period plane.We find some evidence that stars along the active branch show significant average toroidal fields that exhibit large temporal variations while stars exclusively on the inactive branch remain dominantly poloidal throughout their entire cycle. This lends credence to the idea that different shear layers are in operation along each branch. There is also evidence that the short magnetic polarity switches observed on some stars are characteristic of the inactive branch while the longer chromospherically determined periods are characteristic of the active branch. This may explain the discrepancy between the magnetic and chromospheric cycle periods found on some stars. These results represent a first attempt at linking global magnetic field properties obtained from ZDI and activity cycles |
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See, V.Jardine, M.Vidotto, A. A.Donati, J. F.Saikia, S. BoroBouvier, J.Fares, R.Folsom, C. P.Gregory, S. G.Hussain, G.Jeffers, S. V.Marsden, S. C.Morin, J.Moutou, C.Nascimento Júnior, José Dias doPetit, P.Waite, I. A.2020-05-21T17:51:15Z2020-05-21T17:51:15Z2016-08-12SEE, V.; JARDINE, M.; VIDOTTO, A. A.; DONATI, J.-f.; SAIKIA, S. Boro; BOUVIER, J.; FARES, R.; FOLSOM, C. P.; GREGORY, S. G.; HUSSAIN, G.; NASCIMENTO JUNIOR, J.D.. The connection between stellar activity cycles and magnetic field topology. Monthly Notices Of The Royal Astronomical Society, [s.l.], v. 462, n. 4, p. 4442-4450, 12 ago. 2016. Disponível em: http://dx.doi.org/10.1093/mnras/stw2010. Acesso em: 13 mai. 2020.1678-765X10.1093/mnras/stw2010https://repositorio.ufrn.br/jspui/handle/123456789/29046Zeeman–Doppler imaging (ZDI) has successfully mapped the large-scale magnetic fields of stars over a large range of spectral types, rotation periods and ages. When observed over multiple epochs, some stars show polarity reversals in their global magnetic fields. On the Sun, polarity reversals are a feature of its activity cycle. In this paper, we examine the magnetic properties of stars with existing chromospherically determined cycle periods. Previous authors have suggested that cycle periods lie on multiple branches, either in the cycle period–Rossby number plane or the cycle period–rotation period plane.We find some evidence that stars along the active branch show significant average toroidal fields that exhibit large temporal variations while stars exclusively on the inactive branch remain dominantly poloidal throughout their entire cycle. This lends credence to the idea that different shear layers are in operation along each branch. There is also evidence that the short magnetic polarity switches observed on some stars are characteristic of the inactive branch while the longer chromospherically determined periods are characteristic of the active branch. This may explain the discrepancy between the magnetic and chromospheric cycle periods found on some stars. These results represent a first attempt at linking global magnetic field properties obtained from ZDI and activity cyclesZeeman–Doppler imaging (ZDI) has successfully mapped the large-scale magnetic fields of stars over a large range of spectral types, rotation periods and ages. When observed over multiple epochs, some stars show polarity reversals in their global magnetic fields. On the Sun, polarity reversals are a feature of its activity cycle. In this paper, we examine the magnetic properties of stars with existing chromospherically determined cycle periods. Previous authors have suggested that cycle periods lie on multiple branches, either in the cycle period–Rossby number plane or the cycle period–rotation period plane.We find some evidence that stars along the active branch show significant average toroidal fields that exhibit large temporal variations while stars exclusively on the inactive branch remain dominantly poloidal throughout their entire cycle. This lends credence to the idea that different shear layers are in operation along each branch. There is also evidence that the short magnetic polarity switches observed on some stars are characteristic of the inactive branch while the longer chromospherically determined periods are characteristic of the active branch. This may explain the discrepancy between the magnetic and chromospheric cycle periods found on some stars. These results represent a first attempt at linking global magnetic field properties obtained from ZDI and activity cyclesRoyal Astronomical SocietyTechniques - polarimetricStars - activityStars - evolutionStars - magnetic fieldStars - rotationThe connection between stellar activity cycles and magnetic field topologyinfo:eu-repo/semantics/publishedVersioninfo:eu-repo/semantics/articleporreponame:Repositório Institucional da UFRNinstname:Universidade Federal do Rio Grande do Norte (UFRN)instacron:UFRNinfo:eu-repo/semantics/openAccessORIGINALTheConnectionBetweenStellarActivityCyclesAndMagneticFieldTopology_2016.pdfTheConnectionBetweenStellarActivityCyclesAndMagneticFieldTopology_2016.pdfArtigoapplication/pdf392508https://repositorio.ufrn.br/bitstream/123456789/29046/1/TheConnectionBetweenStellarActivityCyclesAndMagneticFieldTopology_2016.pdf57145b914f00ecb986724a9c57df8496MD51LICENSElicense.txtlicense.txttext/plain; charset=utf-81484https://repositorio.ufrn.br/bitstream/123456789/29046/2/license.txte9597aa2854d128fd968be5edc8a28d9MD52TEXTTheConnectionBetweenStellarActivityCyclesAndMagneticFieldTopology_2016.pdf.txtTheConnectionBetweenStellarActivityCyclesAndMagneticFieldTopology_2016.pdf.txtExtracted texttext/plain56667https://repositorio.ufrn.br/bitstream/123456789/29046/3/TheConnectionBetweenStellarActivityCyclesAndMagneticFieldTopology_2016.pdf.txt0006540b2a345e51bf45933742ca3f0cMD53THUMBNAILTheConnectionBetweenStellarActivityCyclesAndMagneticFieldTopology_2016.pdf.jpgTheConnectionBetweenStellarActivityCyclesAndMagneticFieldTopology_2016.pdf.jpgGenerated Thumbnailimage/jpeg1699https://repositorio.ufrn.br/bitstream/123456789/29046/4/TheConnectionBetweenStellarActivityCyclesAndMagneticFieldTopology_2016.pdf.jpga2d2c128f984c52ecf51885155ca8c20MD54123456789/290462020-05-24 06:21:28.029oai:https://repositorio.ufrn.br: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Repositório de PublicaçõesPUBhttp://repositorio.ufrn.br/oai/opendoar:2020-05-24T09:21:28Repositório Institucional da UFRN - Universidade Federal do Rio Grande do Norte (UFRN)false |
dc.title.pt_BR.fl_str_mv |
The connection between stellar activity cycles and magnetic field topology |
title |
The connection between stellar activity cycles and magnetic field topology |
spellingShingle |
The connection between stellar activity cycles and magnetic field topology See, V. Techniques - polarimetric Stars - activity Stars - evolution Stars - magnetic field Stars - rotation |
title_short |
The connection between stellar activity cycles and magnetic field topology |
title_full |
The connection between stellar activity cycles and magnetic field topology |
title_fullStr |
The connection between stellar activity cycles and magnetic field topology |
title_full_unstemmed |
The connection between stellar activity cycles and magnetic field topology |
title_sort |
The connection between stellar activity cycles and magnetic field topology |
author |
See, V. |
author_facet |
See, V. Jardine, M. Vidotto, A. A. Donati, J. F. Saikia, S. Boro Bouvier, J. Fares, R. Folsom, C. P. Gregory, S. G. Hussain, G. Jeffers, S. V. Marsden, S. C. Morin, J. Moutou, C. Nascimento Júnior, José Dias do Petit, P. Waite, I. A. |
author_role |
author |
author2 |
Jardine, M. Vidotto, A. A. Donati, J. F. Saikia, S. Boro Bouvier, J. Fares, R. Folsom, C. P. Gregory, S. G. Hussain, G. Jeffers, S. V. Marsden, S. C. Morin, J. Moutou, C. Nascimento Júnior, José Dias do Petit, P. Waite, I. A. |
author2_role |
author author author author author author author author author author author author author author author author |
dc.contributor.author.fl_str_mv |
See, V. Jardine, M. Vidotto, A. A. Donati, J. F. Saikia, S. Boro Bouvier, J. Fares, R. Folsom, C. P. Gregory, S. G. Hussain, G. Jeffers, S. V. Marsden, S. C. Morin, J. Moutou, C. Nascimento Júnior, José Dias do Petit, P. Waite, I. A. |
dc.subject.por.fl_str_mv |
Techniques - polarimetric Stars - activity Stars - evolution Stars - magnetic field Stars - rotation |
topic |
Techniques - polarimetric Stars - activity Stars - evolution Stars - magnetic field Stars - rotation |
description |
Zeeman–Doppler imaging (ZDI) has successfully mapped the large-scale magnetic fields of stars over a large range of spectral types, rotation periods and ages. When observed over multiple epochs, some stars show polarity reversals in their global magnetic fields. On the Sun, polarity reversals are a feature of its activity cycle. In this paper, we examine the magnetic properties of stars with existing chromospherically determined cycle periods. Previous authors have suggested that cycle periods lie on multiple branches, either in the cycle period–Rossby number plane or the cycle period–rotation period plane.We find some evidence that stars along the active branch show significant average toroidal fields that exhibit large temporal variations while stars exclusively on the inactive branch remain dominantly poloidal throughout their entire cycle. This lends credence to the idea that different shear layers are in operation along each branch. There is also evidence that the short magnetic polarity switches observed on some stars are characteristic of the inactive branch while the longer chromospherically determined periods are characteristic of the active branch. This may explain the discrepancy between the magnetic and chromospheric cycle periods found on some stars. These results represent a first attempt at linking global magnetic field properties obtained from ZDI and activity cycles |
publishDate |
2016 |
dc.date.issued.fl_str_mv |
2016-08-12 |
dc.date.accessioned.fl_str_mv |
2020-05-21T17:51:15Z |
dc.date.available.fl_str_mv |
2020-05-21T17:51:15Z |
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.citation.fl_str_mv |
SEE, V.; JARDINE, M.; VIDOTTO, A. A.; DONATI, J.-f.; SAIKIA, S. Boro; BOUVIER, J.; FARES, R.; FOLSOM, C. P.; GREGORY, S. G.; HUSSAIN, G.; NASCIMENTO JUNIOR, J.D.. The connection between stellar activity cycles and magnetic field topology. Monthly Notices Of The Royal Astronomical Society, [s.l.], v. 462, n. 4, p. 4442-4450, 12 ago. 2016. Disponível em: http://dx.doi.org/10.1093/mnras/stw2010. Acesso em: 13 mai. 2020. |
dc.identifier.uri.fl_str_mv |
https://repositorio.ufrn.br/jspui/handle/123456789/29046 |
dc.identifier.issn.none.fl_str_mv |
1678-765X 10.1093/mnras/stw2010 |
identifier_str_mv |
SEE, V.; JARDINE, M.; VIDOTTO, A. A.; DONATI, J.-f.; SAIKIA, S. Boro; BOUVIER, J.; FARES, R.; FOLSOM, C. P.; GREGORY, S. G.; HUSSAIN, G.; NASCIMENTO JUNIOR, J.D.. The connection between stellar activity cycles and magnetic field topology. Monthly Notices Of The Royal Astronomical Society, [s.l.], v. 462, n. 4, p. 4442-4450, 12 ago. 2016. Disponível em: http://dx.doi.org/10.1093/mnras/stw2010. Acesso em: 13 mai. 2020. 1678-765X 10.1093/mnras/stw2010 |
url |
https://repositorio.ufrn.br/jspui/handle/123456789/29046 |
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por |
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por |
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info:eu-repo/semantics/openAccess |
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openAccess |
dc.publisher.none.fl_str_mv |
Royal Astronomical Society |
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Royal Astronomical Society |
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