The history of a quiet-sun magnetic element revealed by IMaX/Sunrise

Isolated flux tubes are considered to be fundamental magnetic building blocks of the solar photosphere. Their formation is usually attributed to the concentration of magnetic field to kG strengths by the convective collapse mechanism. However, the small size of the magnetic elements in quiet-Sun are...

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Autores: Requerey, Iker S., Toro, José Carlos del, Bellot Rubio, Luis R., Bonet, José A., Martínez Pillet, Valentín, Solanki, S. K., Schmidt, W.
Tipo de recurso: artículo
Estado:Versión aceptada para publicación
Fecha de publicación:2014
País:España
Institución:Consejo Superior de Investigaciones Científicas (CSIC)
Repositorio:DIGITAL.CSIC. Repositorio Institucional del CSIC
OAI Identifier:oai:digital.csic.es:10261/399651
Acceso en línea:http://hdl.handle.net/10261/399651
Access Level:acceso abierto
Palabra clave:Convection
Magnetic fields
Sun: granulation
Sun: photosphere
Techniques: polarimetric
Techniques: spectroscopic
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spelling The history of a quiet-sun magnetic element revealed by IMaX/SunriseRequerey, Iker S.Toro, José Carlos delBellot Rubio, Luis R.Bonet, José A.Martínez Pillet, ValentínSolanki, S. K.Schmidt, W.ConvectionMagnetic fieldsSun: granulationSun: photosphereTechniques: polarimetricTechniques: spectroscopicIsolated flux tubes are considered to be fundamental magnetic building blocks of the solar photosphere. Their formation is usually attributed to the concentration of magnetic field to kG strengths by the convective collapse mechanism. However, the small size of the magnetic elements in quiet-Sun areas has prevented this scenario from being studied in fully resolved structures. Here, we report on the formation and subsequent evolution of one such photospheric magnetic flux tube, observed in the quiet Sun with unprecedented spatial resolution (0.''15-0.''18) and high temporal cadence (33 s). The observations were acquired by the Imaging Magnetograph eXperiment on board the SUNRISE balloon-borne solar observatory. The equipartition field strength magnetic element is the result of the merging of several same polarity magnetic flux patches, including a footpoint of a previously emerged loop. The magnetic structure is then further intensified to kG field strengths by convective collapse. The fine structure found within the flux concentration reveals that the scenario is more complex than can be described by a thin flux tube model with bright points and downflow plumes being established near the edges of the kG magnetic feature. We also observe a daisy-like alignment of surrounding granules and a long-lived inflow toward the magnetic feature. After a subsequent weakening process, the field is again intensified to kG strengths. The area of the magnetic feature is seen to change in anti-phase with the field strength, while the brightness of the bright points and the speed of the downflows varies in phase. We also find a relation between the brightness of the bright point and the presence of upflows within it. © 2014. The American Astronomical SocietyThe work by I.S.R. has been funded by the Basque Government under a grant from Programa de Formacion de Personal In- ´ vestigador del Departamento de Educacion, Universidades e In- ´ vestigacion. This work has been partially funded by the Spanish ´ Ministerio de Econom´ıa y Competitividad, through Project No. AYA2012-39636-C06, including a percentage from European FEDER funds. The German contribution has been funded by the Bundesministerium fur Wirtschaft und Technologie through ¨ Deutsches Zentrum fur Luft- und Raumfahrt e.V. (DLR), grant ¨ No. 50 OU 0401, and by the Innovationsfond of the President of the Max Planck Society (MPG). This work was partly supported by the BK21 plus program through the National Research Foundation (NRF) funded by the Ministry of Education of Korea.Peer reviewedAmerican Astronomical SocietyMinisterio de Economía y Competitividad (España)European CommissionGerman Research FoundationMax Planck SocietyNational Research Foundation of KoreaConsejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]202520252014info:eu-repo/semantics/articlehttp://purl.org/coar/resource_type/c_6501Postprintinfo:eu-repo/semantics/acceptedVersionhttp://hdl.handle.net/10261/399651reponame:DIGITAL.CSIC. Repositorio Institucional del CSICinstname:Consejo Superior de Investigaciones Científicas (CSIC)Inglés#PLACEHOLDER_PARENT_METADATA_VALUE#info:eu-repo/grantAgreement/AEI//AYA2012-39636-C06http://dx.doi.org/10.1088/0004-637X/789/1/6Síinfo:eu-repo/semantics/openAccessoai:digital.csic.es:10261/3996512026-05-22T06:33:51Z
dc.title.none.fl_str_mv The history of a quiet-sun magnetic element revealed by IMaX/Sunrise
title The history of a quiet-sun magnetic element revealed by IMaX/Sunrise
spellingShingle The history of a quiet-sun magnetic element revealed by IMaX/Sunrise
Requerey, Iker S.
Convection
Magnetic fields
Sun: granulation
Sun: photosphere
Techniques: polarimetric
Techniques: spectroscopic
title_short The history of a quiet-sun magnetic element revealed by IMaX/Sunrise
title_full The history of a quiet-sun magnetic element revealed by IMaX/Sunrise
title_fullStr The history of a quiet-sun magnetic element revealed by IMaX/Sunrise
title_full_unstemmed The history of a quiet-sun magnetic element revealed by IMaX/Sunrise
title_sort The history of a quiet-sun magnetic element revealed by IMaX/Sunrise
dc.creator.none.fl_str_mv Requerey, Iker S.
Toro, José Carlos del
Bellot Rubio, Luis R.
Bonet, José A.
Martínez Pillet, Valentín
Solanki, S. K.
Schmidt, W.
author Requerey, Iker S.
author_facet Requerey, Iker S.
Toro, José Carlos del
Bellot Rubio, Luis R.
Bonet, José A.
Martínez Pillet, Valentín
Solanki, S. K.
Schmidt, W.
author_role author
author2 Toro, José Carlos del
Bellot Rubio, Luis R.
Bonet, José A.
Martínez Pillet, Valentín
Solanki, S. K.
Schmidt, W.
author2_role author
author
author
author
author
author
dc.contributor.none.fl_str_mv Ministerio de Economía y Competitividad (España)
European Commission
German Research Foundation
Max Planck Society
National Research Foundation of Korea
Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]
dc.subject.none.fl_str_mv Convection
Magnetic fields
Sun: granulation
Sun: photosphere
Techniques: polarimetric
Techniques: spectroscopic
topic Convection
Magnetic fields
Sun: granulation
Sun: photosphere
Techniques: polarimetric
Techniques: spectroscopic
description Isolated flux tubes are considered to be fundamental magnetic building blocks of the solar photosphere. Their formation is usually attributed to the concentration of magnetic field to kG strengths by the convective collapse mechanism. However, the small size of the magnetic elements in quiet-Sun areas has prevented this scenario from being studied in fully resolved structures. Here, we report on the formation and subsequent evolution of one such photospheric magnetic flux tube, observed in the quiet Sun with unprecedented spatial resolution (0.''15-0.''18) and high temporal cadence (33 s). The observations were acquired by the Imaging Magnetograph eXperiment on board the SUNRISE balloon-borne solar observatory. The equipartition field strength magnetic element is the result of the merging of several same polarity magnetic flux patches, including a footpoint of a previously emerged loop. The magnetic structure is then further intensified to kG field strengths by convective collapse. The fine structure found within the flux concentration reveals that the scenario is more complex than can be described by a thin flux tube model with bright points and downflow plumes being established near the edges of the kG magnetic feature. We also observe a daisy-like alignment of surrounding granules and a long-lived inflow toward the magnetic feature. After a subsequent weakening process, the field is again intensified to kG strengths. The area of the magnetic feature is seen to change in anti-phase with the field strength, while the brightness of the bright points and the speed of the downflows varies in phase. We also find a relation between the brightness of the bright point and the presence of upflows within it. © 2014. The American Astronomical Society
publishDate 2014
dc.date.none.fl_str_mv 2014
2025
2025
dc.type.none.fl_str_mv info:eu-repo/semantics/article
http://purl.org/coar/resource_type/c_6501
Postprint
info:eu-repo/semantics/acceptedVersion
format article
status_str acceptedVersion
dc.identifier.none.fl_str_mv http://hdl.handle.net/10261/399651
url http://hdl.handle.net/10261/399651
dc.language.none.fl_str_mv Inglés
language_invalid_str_mv Inglés
dc.relation.none.fl_str_mv #PLACEHOLDER_PARENT_METADATA_VALUE#
info:eu-repo/grantAgreement/AEI//AYA2012-39636-C06
http://dx.doi.org/10.1088/0004-637X/789/1/6
Sí
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
eu_rights_str_mv openAccess
dc.publisher.none.fl_str_mv American Astronomical Society
publisher.none.fl_str_mv American Astronomical Society
dc.source.none.fl_str_mv reponame:DIGITAL.CSIC. Repositorio Institucional del CSIC
instname:Consejo Superior de Investigaciones Científicas (CSIC)
instname_str Consejo Superior de Investigaciones Científicas (CSIC)
reponame_str DIGITAL.CSIC. Repositorio Institucional del CSIC
collection DIGITAL.CSIC. Repositorio Institucional del CSIC
repository.name.fl_str_mv
repository.mail.fl_str_mv
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score 15.81155

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