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...
| Autores: | , , , , , , |
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| 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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oai:digital.csic.es:10261/399651 |
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The history of a quiet-sun magnetic element revealed by IMaX/Sunrise Requerey, Iker S. Toro, José Carlos del Bellot Rubio, Luis R. Bonet, José A. Martínez Pillet, Valentín Solanki, S. K. Schmidt, W. Convection Magnetic fields Sun: granulation Sun: photosphere Techniques: polarimetric Techniques: spectroscopic 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 The 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 reviewed American Astronomical Society http://hdl.handle.net/10261/399651 |
| 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 |
| 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 |
| topic |
Convection Magnetic fields Sun: granulation Sun: photosphere Techniques: polarimetric Techniques: spectroscopic |
| topic_facet |
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 |
| format |
article |
| status_str |
acceptedVersion |
| url |
http://hdl.handle.net/10261/399651 |
| eu_rights_str_mv |
openAccess |
| publisher |
American Astronomical Society |
| institution |
Consejo Superior de Investigaciones Científicas (CSIC) |
| collection |
DIGITAL.CSIC. Repositorio Institucional del CSIC |
| reponame_str |
DIGITAL.CSIC. Repositorio Institucional del CSIC |
| instname_str |
Consejo Superior de Investigaciones Científicas (CSIC) |
| _version_ |
1878440984044371968 |
| publishDateSort |
2014 |
| author_browse |
Bellot Rubio, Luis R. Bonet, José A. Martínez Pillet, Valentín Requerey, Iker S. Schmidt, W. Solanki, S. K. Toro, José Carlos del |
| publisherStr |
American Astronomical Society |
| score |
6,9303427 |