Temporal relations between magnetic bright points and the solar sunspot cycle

The Sun shows a global magnetic field cycle traditionally best visible in the photosphere as a changing sunspot cycle featuring roughly an 11-year period. In addition we know that our host star also harbours small-scale magnetic fields often seen as strong concentrations of magnetic flux reaching kG...

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Detalles Bibliográficos
Autores: Utz, D., Muller, R., Van Doorsselaere, T.
Tipo de recurso: artículo
Estado:Versión aceptada para publicación
Fecha de publicación:2017
País:España
Institución:Consejo Superior de Investigaciones Científicas (CSIC)
Repositorio:DIGITAL.CSIC. Repositorio Institucional del CSIC
OAI Identifier:oai:digital.csic.es:10261/382975
Acceso en línea:http://hdl.handle.net/10261/382975
Access Level:acceso abierto
Palabra clave:Dynamo
Sun: activity
Sun: magnetic fields
Sunspots
Techniques: high angular resolution
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network_acronym_str ES
network_name_str España
repository_id_str
dc.title.none.fl_str_mv Temporal relations between magnetic bright points and the solar sunspot cycle
title Temporal relations between magnetic bright points and the solar sunspot cycle
spellingShingle Temporal relations between magnetic bright points and the solar sunspot cycle
Utz, D.
Dynamo
Sun: activity
Sun: magnetic fields
Sunspots
Techniques: high angular resolution
title_short Temporal relations between magnetic bright points and the solar sunspot cycle
title_full Temporal relations between magnetic bright points and the solar sunspot cycle
title_fullStr Temporal relations between magnetic bright points and the solar sunspot cycle
title_full_unstemmed Temporal relations between magnetic bright points and the solar sunspot cycle
title_sort Temporal relations between magnetic bright points and the solar sunspot cycle
dc.creator.none.fl_str_mv Utz, D.
Muller, R.
Van Doorsselaere, T.
author Utz, D.
author_facet Utz, D.
Muller, R.
Van Doorsselaere, T.
author_role author
author2 Muller, R.
Van Doorsselaere, T.
author2_role author
author
dc.contributor.none.fl_str_mv NASA
Science and Technology Facilities Council (UK)
European Space Agency
Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]
dc.subject.none.fl_str_mv Dynamo
Sun: activity
Sun: magnetic fields
Sunspots
Techniques: high angular resolution
topic Dynamo
Sun: activity
Sun: magnetic fields
Sunspots
Techniques: high angular resolution
description The Sun shows a global magnetic field cycle traditionally best visible in the photosphere as a changing sunspot cycle featuring roughly an 11-year period. In addition we know that our host star also harbours small-scale magnetic fields often seen as strong concentrations of magnetic flux reaching kG field strengths. These features are situated in inter-granular lanes, where they show up bright as so-called magnetic bright points (MBPs). In this short paper we wish to analyse an homogenous, nearly 10-year-long synoptic Hinode image data set recorded from 2006 November up to 2016 February in the G-band to inspect the relationship between the number of MBPs at the solar disc centre and the relative sunspot number. Our findings suggest that the number of MBPs at the solar disc centre is indeed correlated to the relative sunspot number, but with the particular feature of showing two different temporal shifts between the decreasing phase of cycle 23 including the minimum and the increasing phase of cycle 24 including the maximum. While the former is shifted by about 22 months, the latter is only shifted by less than 12 months. Moreover, we introduce and discuss an analytical model to predict the number of MBPs at the solar disc centre purely depending on the evolution of the relative sunspot number as well as the temporal change of the relative sunspot number and two background parameters describing a possibly acting surface dynamo as well as the strength of the magnetic field diffusion. Finally, we are able to confirm the plausibility of the temporal shifts by a simplistic random walk model. The main conclusion to be drawn from this work is that the injection of magnetic flux, coming from active regions as represented by sunspots, happens on faster time scales than the removal of small-scale magnetic flux elements later on. © The Author 2017.
publishDate 2017
dc.date.none.fl_str_mv 2017
2025
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/10261/382975
url http://hdl.handle.net/10261/382975
dc.language.none.fl_str_mv Inglés
language_invalid_str_mv Inglés
dc.relation.none.fl_str_mv http://dx.doi.org/10.1093/pasj/psx115
Sí
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
eu_rights_str_mv openAccess
dc.publisher.none.fl_str_mv Oxford University Press
publisher.none.fl_str_mv Oxford University Press
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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spelling Temporal relations between magnetic bright points and the solar sunspot cycleUtz, D.Muller, R.Van Doorsselaere, T.DynamoSun: activitySun: magnetic fieldsSunspotsTechniques: high angular resolutionThe Sun shows a global magnetic field cycle traditionally best visible in the photosphere as a changing sunspot cycle featuring roughly an 11-year period. In addition we know that our host star also harbours small-scale magnetic fields often seen as strong concentrations of magnetic flux reaching kG field strengths. These features are situated in inter-granular lanes, where they show up bright as so-called magnetic bright points (MBPs). In this short paper we wish to analyse an homogenous, nearly 10-year-long synoptic Hinode image data set recorded from 2006 November up to 2016 February in the G-band to inspect the relationship between the number of MBPs at the solar disc centre and the relative sunspot number. Our findings suggest that the number of MBPs at the solar disc centre is indeed correlated to the relative sunspot number, but with the particular feature of showing two different temporal shifts between the decreasing phase of cycle 23 including the minimum and the increasing phase of cycle 24 including the maximum. While the former is shifted by about 22 months, the latter is only shifted by less than 12 months. Moreover, we introduce and discuss an analytical model to predict the number of MBPs at the solar disc centre purely depending on the evolution of the relative sunspot number as well as the temporal change of the relative sunspot number and two background parameters describing a possibly acting surface dynamo as well as the strength of the magnetic field diffusion. Finally, we are able to confirm the plausibility of the temporal shifts by a simplistic random walk model. The main conclusion to be drawn from this work is that the injection of magnetic flux, coming from active regions as represented by sunspots, happens on faster time scales than the removal of small-scale magnetic flux elements later on. © The Author 2017.This research received support by the Austrian Science Fund (FWF): P27800. Additional funding was possible through an Odysseus grant of the FWO Vlaanderen, the IAP P7/08 CHARM (Belspo), and GOA-2015-014 (KU Leuven). The authors are very thankful to the Hinode team for operating and maintaining the extremely fruitful Hinode space mission over all these years. The lead author (D.U.) especially wishes to express his gratitude to the whole Hinode team as this mission was his starting point and entry point into the solar physics community more or less exactly 10 years ago. Hinode is a Japanese mission developed and launched by ISAS/JAXA, collaborating with NAOJ as a domestic partner, NASA and STFC (UK) as international partners. Scientific operation of the Hinode mission is conducted by the Hinode science team organized at ISAS/JAXA. This team mainly consists of scientists from institutes in the partner countries. Support for the post-launch operation is provided by JAXA and NAOJ (Japan), STFC (UK), NASA (USA), ESA, and NSC (Norway). Besides, our gratitude goes to the SILSO team from the Royal Belgium Observatory for maintaining and making publicly available the relative sunspot number. SILSO, World Data Center - Sunspot Number and Long-term Solar Observations, Royal Observatory of Belgium, on-line Sunspot Number catalogue: http://www.sidc.be/SILSO/. We wish to express our gratitude to the anonymous referee, who, due to his criticism of the model, enabled us to strengthen our modeling approach considerably.Oxford University PressNASAScience and Technology Facilities Council (UK)European Space AgencyConsejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]2025202520172025info:eu-repo/semantics/articlehttp://purl.org/coar/resource_type/c_6501Postprintinfo:eu-repo/semantics/acceptedVersionhttp://hdl.handle.net/10261/382975reponame:DIGITAL.CSIC. Repositorio Institucional del CSICinstname:Consejo Superior de Investigaciones Científicas (CSIC)Ingléshttp://dx.doi.org/10.1093/pasj/psx115Síinfo:eu-repo/semantics/openAccessoai:digital.csic.es:10261/3829752026-05-22T06:33:51Z
score 15,812429

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