The Solar Internetwork. III. Unipolar versus Bipolar Flux Appearance

This is an Open Access article distributed under the terms of the Creative Commons Attribution License (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted reuse, distribution, and reproduction in any medium, provided the original work is properly cited.

Detalles Bibliográficos
Autores: Gosic, Milan, Bellot Rubio, Luis R., Cheung, M. C. M., Orozco Suárez, David, Katsukawa, Y., Toro, José Carlos del
Tipo de recurso: artículo
Estado:Versión publicada
Fecha de publicación:2022
País:España
Institución:Consejo Superior de Investigaciones Científicas (CSIC)
Repositorio:DIGITAL.CSIC. Repositorio Institucional del CSIC
OAI Identifier:oai:digital.csic.es:10261/282015
Acceso en línea:http://hdl.handle.net/10261/282015
Access Level:acceso abierto
Palabra clave:Solar photosphere
Solar magnetic flux emergence
Solar magnetic fields
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spelling The Solar Internetwork. III. Unipolar versus Bipolar Flux AppearanceGosic, MilanBellot Rubio, Luis R.Cheung, M. C. M.Orozco Suárez, DavidKatsukawa, Y.Toro, José Carlos delSolar photosphereSolar magnetic flux emergenceSolar magnetic fieldsThis is an Open Access article distributed under the terms of the Creative Commons Attribution License (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted reuse, distribution, and reproduction in any medium, provided the original work is properly cited.Small-scale internetwork (IN) magnetic fields are considered to be the main building blocks of quiet Sun magnetism. For this reason, it is crucial to understand how they appear on the solar surface. Here, we employ a high-resolution, high-sensitivity, long-duration Hinode/NFI magnetogram sequence to analyze the appearance modes and spatiotemporal evolution of individual IN magnetic elements inside a supergranular cell at the disk center. From identification of flux patches and magnetofrictional simulations, we show that there are two distinct populations of IN flux concentrations: unipolar and bipolar features. Bipolar features tend to be bigger and stronger than unipolar features. They also live longer and carry more flux per feature. Both types of flux concentrations appear uniformly over the solar surface. However, we argue that bipolar features truly represent the emergence of new flux on the solar surface, while unipolar features seem to be formed by the coalescence of background flux. Magnetic bipoles appear at a faster rate than unipolar features (68 as opposed to 55 Mx cm−2 day−1), and provide about 70% of the total instantaneous IN flux detected in the interior of the supergranule. © 2022. The Author(s). Published by the American Astronomical Society.The data used here were acquired in the framework of Hinode Operation Plan 151, "Flux replacement in the solar network and internetwork." We thank the Hinode Chief Observers for the efforts they made to accommodate our demanding observations. Hinode is a Japanese mission developed and launched by ISAS/JAXA, with NAOJ as a domestic partner and NASA and STFC (UK) as international partners. It is operated by these agencies in cooperation with ESA and NSC (Norway). M.G. acknowledges a JAE-Pre fellowship granted by Agencia Estatal Consejo Superior de Investigaciones Científicas toward the completion of a PhD. This work has been funded by the State Agency for Research of the Spanish Ministerio de Ciencia e Innovación through grant RTI2018-096886-B-C5 (including FEDER funds) and through a Center of Excellence Severo Ochoa award to Instituto de Astrofísica de Andalucía (SEV-2017-0709). NASA supported this work through contract NNM07AA01C (Solar-B (Hinode) Focal Plane Package Phase E). Use of NASA's Astrophysical Data System is gratefully acknowledged.Peer reviewedIOP PublishingMinisterio de Ciencia e Innovación (España)European CommissionNASAConsejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]202220222022info:eu-repo/semantics/articlehttp://purl.org/coar/resource_type/c_6501Publisher's versioninfo:eu-repo/semantics/publishedVersionhttp://hdl.handle.net/10261/282015reponame:DIGITAL.CSIC. Repositorio Institucional del CSICinstname:Consejo Superior de Investigaciones Científicas (CSIC)Inglés#PLACEHOLDER_PARENT_METADATA_VALUE##PLACEHOLDER_PARENT_METADATA_VALUE#info:eu-repo/grantAgreement/MICINN//SEV-2017-0709info:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2017-2020/RTI2018-096886-B-C51http://dx.doi.org/10.3847/1538-4357/ac37beSíinfo:eu-repo/semantics/openAccessoai:digital.csic.es:10261/2820152026-05-22T06:33:51Z
dc.title.none.fl_str_mv The Solar Internetwork. III. Unipolar versus Bipolar Flux Appearance
title The Solar Internetwork. III. Unipolar versus Bipolar Flux Appearance
spellingShingle The Solar Internetwork. III. Unipolar versus Bipolar Flux Appearance
Gosic, Milan
Solar photosphere
Solar magnetic flux emergence
Solar magnetic fields
title_short The Solar Internetwork. III. Unipolar versus Bipolar Flux Appearance
title_full The Solar Internetwork. III. Unipolar versus Bipolar Flux Appearance
title_fullStr The Solar Internetwork. III. Unipolar versus Bipolar Flux Appearance
title_full_unstemmed The Solar Internetwork. III. Unipolar versus Bipolar Flux Appearance
title_sort The Solar Internetwork. III. Unipolar versus Bipolar Flux Appearance
dc.creator.none.fl_str_mv Gosic, Milan
Bellot Rubio, Luis R.
Cheung, M. C. M.
Orozco Suárez, David
Katsukawa, Y.
Toro, José Carlos del
author Gosic, Milan
author_facet Gosic, Milan
Bellot Rubio, Luis R.
Cheung, M. C. M.
Orozco Suárez, David
Katsukawa, Y.
Toro, José Carlos del
author_role author
author2 Bellot Rubio, Luis R.
Cheung, M. C. M.
Orozco Suárez, David
Katsukawa, Y.
Toro, José Carlos del
author2_role author
author
author
author
author
dc.contributor.none.fl_str_mv Ministerio de Ciencia e Innovación (España)
European Commission
NASA
Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]
dc.subject.none.fl_str_mv Solar photosphere
Solar magnetic flux emergence
Solar magnetic fields
topic Solar photosphere
Solar magnetic flux emergence
Solar magnetic fields
description This is an Open Access article distributed under the terms of the Creative Commons Attribution License (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted reuse, distribution, and reproduction in any medium, provided the original work is properly cited.
publishDate 2022
dc.date.none.fl_str_mv 2022
2022
2022
dc.type.none.fl_str_mv info:eu-repo/semantics/article
http://purl.org/coar/resource_type/c_6501
Publisher's version
info:eu-repo/semantics/publishedVersion
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://hdl.handle.net/10261/282015
url http://hdl.handle.net/10261/282015
dc.language.none.fl_str_mv Inglés
language_invalid_str_mv Inglés
dc.relation.none.fl_str_mv #PLACEHOLDER_PARENT_METADATA_VALUE#
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info:eu-repo/grantAgreement/MICINN//SEV-2017-0709
info:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2017-2020/RTI2018-096886-B-C51
http://dx.doi.org/10.3847/1538-4357/ac37be
Sí
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
eu_rights_str_mv openAccess
dc.publisher.none.fl_str_mv IOP Publishing
publisher.none.fl_str_mv IOP Publishing
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
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